# last updated on Thu May 17 07:20:01 JST 2012, dbhost=host=athena, by rodos +--------------------------+-----------+-----------+--------------+--------------+------------+------------------+------------------+-----------+----------+--------------+-----------+-----------+-----------+-----------+----------------+----------------+----------------+----------------+---------------+-------------+-------------+-------------+----------+--------------+------------+-------------------+------------------+-------------+-------------------+--------------------+---------------+--------------------------------------------+--------+----------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------+-------------------------------+---------------+----------+--------------------+----------------+-------------+--------------+---------+-------+----------+--------------------------------------------------------------------------------------------------------------------------+----------+-----------+ | NAME | RA | DEC | LII | BII | ROLL_ANGLE | TIME | STOP_TIME | OBSID | EXPOSURE | TIME_AWARDED | XIS0_EXPO | XIS1_EXPO | XIS2_EXPO | XIS3_EXPO | XIS0_NUM_MODES | XIS1_NUM_MODES | XIS2_NUM_MODES | XIS3_NUM_MODES | HXD_NUM_MODES | HXD_EXPO_CO | HXD_EXPO_FI | HXD_EXPO_NO | HXD_EXPO | HXD_EXPO_WAM | HXD_BURSTS | PROCESSING_STATUS | PROCESSING_DATE | PUBLIC_DATE | DISTRIBUTION_DATE | PROCESSING_VERSION | NUM_PROCESSED | SOFTWARE_VERSION | PRNB | ABSTRACT | SUBJECT_CATEGORY | CATEGORY_CODE | PRIORITY | PI_LNAME | PI_FNAME | COPI_LNAME | COPI_FNAME | COUNTRY | CYCLE | OBS_TYPE | TITLE | AIMPOINT | INJECTION | +--------------------------+-----------+-----------+--------------+--------------+------------+------------------+------------------+-----------+----------+--------------+-----------+-----------+-----------+-----------+----------------+----------------+----------------+----------------+---------------+-------------+-------------+-------------+----------+--------------+------------+-------------------+------------------+-------------+-------------------+--------------------+---------------+--------------------------------------------+--------+----------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------+-------------------------------+---------------+----------+--------------------+----------------+-------------+--------------+---------+-------+----------+--------------------------------------------------------------------------------------------------------------------------+----------+-----------+ | E0102-72 | 16.139 | -72.1205 | 301.50933431 | -44.97149935 | 119.4064 | 53593.3086458333 | 53595.2485069444 | 100001010 | 2406.8 | 70000 | 2406.8 | 2406.8 | 2406.8 | 2406.8 | 1 | 1 | 1 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 54324.1896990741 | 54247 | 54035.5925115741 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000001 | XIS door open with a SMC SNR E0102-72 | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | XIS door open | NULL | N | | E0102-72 | 15.9884 | -72.0403 | 301.56673438 | -45.05476105 | 119.5512 | 53595.2489236111 | 53595.4618518518 | 100001020 | 4159.8 | 10000 | 4159.8 | 4159.8 | 4159.8 | 4159.8 | 1 | 1 | 1 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 54326.8727430556 | 54247 | 54035.6312731482 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000001 | XIS door open with a SMC SNR E0102-72 | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | XIS door open | NULL | N | | N132D | 81.2794 | -69.6524 | 280.31514531 | -32.77566051 | 53.3291 | 53595.4703125 | 53597.5313541667 | 100002010 | 7406.6 | 80000 | 7406.6 | 7406.6 | 7406.6 | 7406.6 | 2 | 2 | 2 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 54330.31 | 54247 | 54038.5875925926 | 2.0.6.13 | 5 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD HV ON WITH N132D | NULL | N | | N132D | 81.1356 | -69.5861 | 280.24807804 | -32.83670135 | 53.4639 | 53597.5317361111 | 53597.6932291667 | 100002020 | 0 | 7000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 54320.5084259259 | 54247 | 54230.4131828704 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD HV ON WITH N132D | NULL | N | | N132D | 81.4173 | -69.7177 | 280.38157857 | -32.71705874 | 53.198 | 53597.6939814815 | 53597.8369328704 | 100002030 | 0 | 7000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 54320.4973032407 | 54247 | 54230.4133449074 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD HV ON WITH N132D | NULL | N | | N132D | 81.0865 | -69.7023 | 280.38777612 | -32.83268249 | 53.5118 | 53597.8375 | 53597.9865625 | 100002040 | 0 | 7000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 54320.6242708333 | 54247 | 54230.4148726852 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD HV ON WITH N132D | NULL | N | | N132D | 81.4727 | -69.6025 | 280.24276086 | -32.71811202 | 53.1485 | 53597.9869444444 | 53598.2398958333 | 100002050 | 0 | 7000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 54320.6674652778 | 54247 | 54230.4157291667 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD HV ON WITH N132D | NULL | N | | N132D | 81.2751 | -69.6506 | 280.31335191 | -32.77744994 | 53.3312 | 53598.2402777778 | 53598.5140046296 | 100002060 | 5963.5 | 7000 | 5963.5 | 5963.5 | 5963.5 | 5963.5 | 1 | 1 | 1 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 54327.1238888889 | 54247 | 54038.4700810185 | 2.0.6.13 | 5 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD HV ON WITH N132D | NULL | N | | DEM_L71/N23 | 76.4474 | -67.958 | 278.75859594 | -34.83581885 | 70.5849 | 53598.5206365741 | 53599.6042592593 | 100003010 | 5789.7 | 40000 | 5789.7 | 5789.7 | 5789.7 | 5789.7 | 2 | 2 | 2 | 2 | 0 | 0 | 0 | 0 | 0 | 93606.1 | 0 | PROCESSED | 54329.4726736111 | 54247 | 54035.7018171296 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000003 | LMC SNRs L71/N23 | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | LMC SNRs | NULL | N | | MCG-6-30-15 | 203.9795 | -34.2919 | 313.29805273 | 27.68293005 | 295.971 | 53599.6735300926 | 53601.1459027778 | 100004010 | 46698.7 | 40000 | 46700.9 | 50916.9 | 46698.7 | 46725.4 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 46484.6 | 46484.6 | 127099.9 | 0 | PROCESSED | 54330.2736458333 | 54247 | 54035.7991782407 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000004 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | MCG-60-30-15 | NULL | N | | Cen A | 201.3695 | -43.0177 | 309.51950829 | 19.41821819 | 303.9158 | 53601.1523032407 | 53602.4098148148 | 100005010 | 64675.9 | 40000 | 64694.2 | 64765.8 | 64675.9 | 64739.9 | 5 | 2 | 5 | 5 | 1 | 0 | 0 | 66258.2 | 66258.2 | 108611.9 | 0 | PROCESSED | 54327.7080208333 | 53705 | 53905.4597106482 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000005 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Cen A | NULL | N | | A 2052 | 229.2779 | 6.8766 | 9.31339919 | 49.96215441 | 281.2328 | 53602.4238078704 | 53602.743287037 | 100006010 | 13902.1 | 20000 | 13902.1 | 13902.1 | 13902.1 | 13902.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13416.3 | 13416.3 | 27583.9 | 0 | PROCESSED | 54320.5582175926 | 53705 | 53905.4607523148 | 2.0.6.13 | 10 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000006 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Outer region of A 2052 | NULL | N | | A 2052 | 229.3237 | 7.1059 | 9.64711471 | 50.05514889 | 281.2373 | 53602.7440393518 | 53603.3406944445 | 100006020 | 25743.1 | 20000 | 25743.1 | 25743.1 | 25743.1 | 25743.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 21064.2 | 21064.2 | 51519.9 | 0 | PROCESSED | 54320.8272106482 | 53705 | 53905.4610300926 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000006 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Outer region of A 2052 | NULL | N | | A 2052 | 229.0933 | 7.1516 | 9.50335527 | 50.26933049 | 281.2093 | 53603.3412615741 | 53603.6114351852 | 100006030 | 12969 | 20000 | 12969 | 12969 | 12969 | 12969 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13141.3 | 13141.3 | 23327.9 | 0 | PROCESSED | 54320.518287037 | 53705 | 53905.4613310185 | 2.0.6.13 | 8 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000006 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Outer region of A 2052 | NULL | N | | A 2052 | 229.0471 | 6.9211 | 9.16646689 | 50.17566284 | 281.2031 | 53603.6121875 | 53603.9938425926 | 100006040 | 16744.3 | 20000 | 16744.3 | 16744.3 | 16744.3 | 16744.3 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 12839.5 | 12839.5 | 32951.9 | 0 | PROCESSED | 54320.5766435185 | 53705 | 53905.4634143518 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000006 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Outer region of A 2052 | NULL | N | | A 2052 | 229.3311 | 7.2632 | 9.85579143 | 50.13807877 | 91.2371 | 53762.482650463 | 53762.9209953704 | 100006050 | 22366 | 20000 | 22366 | 22366 | 22366 | 22366 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20388 | 20388 | 37865.9 | 0 | PROCESSED | 54405.5900578704 | 54247 | 54040.5318634259 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000006 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Outer region of A 2052 | XIS | N | | Crab Nebula | 83.6274 | 22.0192 | 184.55062413 | -5.78629385 | 86.8663 | 53604.1571412037 | 53604.2501273148 | 100007010 | 1722.9 | 5000 | 1722.9 | 1722.9 | 1722.9 | 1722.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1808 | 1808 | 8034 | 0 | PROCESSED | 54320.5038425926 | 54247 | 54105.2758912037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Nebula | NULL | N | | Crab nebula | 83.6201 | 22.1854 | 184.40591259 | -5.70300776 | 86.8631 | 53604.2507175926 | 53604.3889351852 | 100007020 | 3053.1 | 5000 | 3057.1 | 3053.1 | 3053.1 | 3053.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3134.3 | 3134.3 | 11940 | 1 | PROCESSED | 54320.7151273148 | 54247 | 54105.2987268518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Nebula | NULL | N | | Crab nebula | 83.6399 | 21.8519 | 184.69891686 | -5.86604099 | 86.8683 | 53604.3898263889 | 53604.4890972222 | 100007030 | 2786.1 | 5000 | 2786.1 | 2786.1 | 2790.1 | 2786.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2192.7 | 2192.7 | 8554.1 | 0 | PROCESSED | 54320.5508564815 | 54247 | 54105.2865393518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Nebula | NULL | N | | Crab nebula | 83.4512 | 22.0082 | 184.47195778 | -5.93010486 | 86.7989 | 53604.489849537 | 53604.5835416667 | 100007040 | 4268.2 | 5000 | 4268.2 | 4268.2 | 4268.2 | 4268.2 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 4139.2 | 4139.2 | 8056 | 0 | PROCESSED | 54326.8415277778 | 54247 | 54105.3073726852 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Nebula | NULL | N | | Crab nebula | 83.8083 | 22.0272 | 184.63396429 | -5.64031243 | 86.9342 | 53604.5844791667 | 53604.6479861111 | 100007050 | 3262 | 5000 | 3262 | 3262 | 3262 | 3262 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3179 | 3179 | 5448 | 0 | PROCESSED | 54320.5353819444 | 54247 | 54105.3334143518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Nebula | NULL | N | | NGC 4945 | 196.3712 | -49.4666 | 305.27663793 | 13.34118784 | 313.9062 | 53604.7788310185 | 53605.1010763889 | 100008010 | 14338 | 15000 | 14338 | 14338 | 14338 | 14338 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 13806.7 | 13806.7 | 27841.9 | 1 | PROCESSED | 54320.7326157407 | 54247 | 54035.5212152778 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000008 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | NGC 4945 | NULL | N | | NGC 4945 | 196.3733 | -49.4666 | 305.27803835 | 13.34111135 | 313.9078 | 53605.101087963 | 53605.1034490741 | 100008020 | 177.6 | 10000 | 181.5 | 181.5 | 179.6 | 177.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 200.1 | 200.1 | 202 | 0 | PROCESSED | 54320.5963888889 | 54247 | 54034.6891435185 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000008 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | NGC 4945 | NULL | N | | NGC 4945 | 196.3681 | -49.4152 | 305.27752827 | 13.39262005 | 96.1296 | 53750.3365625 | 53752.9655092593 | 100008030 | 95066.3 | 10000 | 95081.7 | 95129.7 | 95066.3 | 95106.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 84981.3 | 84981.3 | 227115.7 | 2 | PROCESSED | 54331.2095949074 | 54247 | 54040.3587615741 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000008 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | NGC 4945 | HXD | N | | PSR1509-58 | 228.4798 | -59.0943 | 320.34145971 | -1.12587132 | 287.6342 | 53605.36 | 53606.8597569444 | 100009010 | 65161.8 | 60000 | 65161.8 | 65322.7 | 65242.7 | 65242.7 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 49735.7 | 49735.7 | 129529.8 | 4 | PROCESSED | 54330.3722222222 | 53705 | 53905.4622337963 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000009 | HXD spectrum and timing check | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | PSR1509-58 | NULL | N | | Crab Nebula | 83.6267 | 22.0751 | 184.50282132 | -5.75691305 | 86.8655 | 53607.0070833333 | 53607.1389814815 | 100010010 | 2937.9 | 5000 | 2937.9 | 2937.9 | 2937.9 | 2937.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 3438.7 | 3438.7 | 11381.9 | 0 | PROCESSED | 54323.3773148148 | 54247 | 54118.9886689815 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N | | Crab nebula | 83.6336 | 21.9568 | 184.60669551 | -5.81484075 | 86.8687 | 53607.1394560185 | 53607.2779282407 | 100010020 | 3653.3 | 5000 | 3653.3 | 3653.3 | 3653.3 | 3653.3 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3806.7 | 3806.7 | 11934 | 0 | PROCESSED | 54320.7270717593 | 54247 | 54118.9337615741 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N | | Crab nebula | 83.6105 | 22.3483 | 184.26290563 | -5.62323625 | 86.8596 | 53607.2790509259 | 53607.5139583333 | 100010030 | 8112.9 | 5000 | 8112.9 | 8112.9 | 8112.9 | 8112.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 7835.9 | 7835.9 | 20264 | 1 | PROCESSED | 54320.9165625 | 54247 | 54118.9698958333 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N | | Crab nebula | 83.6511 | 21.6763 | 184.85366771 | -5.95118505 | 86.8795 | 53607.5153125 | 53607.7153472222 | 100010040 | 9580.6 | 5000 | 9580.6 | 9580.6 | 9580.6 | 9580.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 8178.3 | 8178.3 | 17248 | 0 | PROCESSED | 54326.880474537 | 54247 | 54118.943125 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N | | Crab nebula | 83.2708 | 21.9976 | 184.39063256 | -6.07689385 | 86.7331 | 53607.7165162037 | 53607.9167361111 | 100010050 | 9346.9 | 5000 | 9346.9 | 9346.9 | 9346.9 | 9346.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 6653 | 6653 | 17287.9 | 0 | PROCESSED | 54326.8750347222 | 54247 | 54122.4223611111 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N | | Crab nebula | 83.5677 | 22.0135 | 184.52566905 | -5.83608695 | 86.8444 | 53607.9175810185 | 53608.0695023148 | 100010060 | 4877.9 | 5000 | 4877.9 | 4877.9 | 4877.9 | 4877.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 5021.7 | 5021.7 | 13076 | 0 | PROCESSED | 54320.7265277778 | 54247 | 54122.4195486111 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N | | Crab nebula | 83.6922 | 22.0221 | 184.58047361 | -5.73399538 | 86.8671 | 53608.0699768518 | 53608.2084027778 | 100010070 | 4089.9 | 5000 | 4089.9 | 4089.9 | 4089.9 | 4089.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 4228.3 | 4228.3 | 11925.9 | 0 | PROCESSED | 54323.0051041667 | 54247 | 54119.0149074074 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N | | Crab nebula | 83.6222 | 22.1365 | 184.44846107 | -5.72755512 | 86.8666 | 53608.2089236111 | 53608.316087963 | 100010080 | 3382 | 5000 | 3382 | 3382 | 3382 | 3382 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3700.3 | 3700.3 | 9253.9 | 0 | PROCESSED | 54320.4816435185 | 54247 | 54119.0056134259 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N | | Crab nebula | 83.5807 | 22.8483 | 183.82410841 | -5.37832099 | 86.8677 | 53608.3175810185 | 53608.5139583333 | 100010090 | 6716 | 5000 | 6716 | 6716 | 6716 | 6716 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 6376.8 | 6376.8 | 16950.1 | 0 | PROCESSED | 54323.044537037 | 54247 | 54119.0235648148 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N | | Crab nebula | 83.9887 | 22.0345 | 184.71743044 | -5.49499441 | 86.8666 | 53608.5155902778 | 53608.7153472222 | 100010100 | 9694 | 5000 | 9694 | 9694 | 9694 | 9694 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 7581.2 | 7581.2 | 17247.9 | 0 | PROCESSED | 54326.8826967593 | 54247 | 54122.4242939815 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N | | Crab nebula | 83.5122 | 24.0135 | 182.80375415 | -4.80497322 | 86.8675 | 53608.7179976852 | 53608.930625 | 100010110 | 9480.5 | 5000 | 9480.5 | 9480.5 | 9480.5 | 9480.5 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 7363 | 7363 | 18336 | 0 | PROCESSED | 54320.855462963 | 54247 | 54118.98625 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N | | Crab nebula | 83.6374 | 21.9009 | 184.65605757 | -5.84178049 | 86.8664 | 53608.9333217593 | 53609.069525463 | 100010120 | 4745.6 | 5000 | 4745.6 | 4745.6 | 4745.6 | 4745.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 5178.7 | 5178.7 | 11757.9 | 1 | PROCESSED | 54320.5947337963 | 54247 | 54118.9946180556 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Observation of Galactic Center Region | NULL | N | | 1E1743.1-2843(GC_BGD_3) | 266.592 | -28.6516 | 0.32828705 | 0.00813221 | 264.88 | 53638.7286111111 | 53638.793275463 | 100027050 | 1984.6 | 5000 | 1984.6 | 1984.6 | 1984.6 | 1984.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1793.4 | 1793.4 | 5567.9 | 0 | PROCESSED | 54318.5558912037 | 54247 | 53905.6343055556 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000027 | We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Observation of Galactic Center Region | NULL | N | | HESS J1616-508 | 244.1248 | -50.8971 | 332.40352084 | -0.15000913 | 282.8476 | 53632.5000231482 | 53633.8183333333 | 100028010 | 41352 | 50000 | 41352 | 41376 | 41352 | 41368 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35373.1 | 35373.1 | 113889.9 | 0 | PROCESSED | 54328.1468634259 | 54247 | 54035.4361111111 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000028 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | New HESS sources and the Galactic ridge Background | NULL | N | | HESS J1616-508_BGD1 | 243.666 | -51.1742 | 332.00349288 | -0.15039556 | 283.0062 | 53631.9497222222 | 53632.4990856482 | 100028020 | 19327.7 | 25000 | 19327.7 | 20630 | 19360 | 19632.3 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 16642.6 | 16642.6 | 47447.9 | 0 | PROCESSED | 54320.8714583333 | 54247 | 54035.1692476852 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000028 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | New HESS sources and the Galactic ridge Background | NULL | N | | HESS J1616-508_BGD2 | 244.4656 | -50.6883 | 332.70353325 | -0.14997577 | 283.1793 | 53633.8196412037 | 53634.3120833333 | 100028030 | 21873.5 | 25000 | 21889.5 | 21889.5 | 21881.5 | 21873.5 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18206.3 | 18206.3 | 42535.9 | 0 | PROCESSED | 54322.7236111111 | 54247 | 54035.4698842593 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000028 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | New HESS sources and the Galactic ridge Background | NULL | N | | GRO J1655-40 | 253.5027 | -39.8455 | 344.98315976 | 2.45489032 | 268.0237 | 53635.3140625 | 53636.2968055556 | 100029010 | 35222.8 | 40000 | 0 | 35233.6 | 35222.8 | 35230.8 | 0 | 1 | 2 | 2 | 1 | 0 | 0 | 28731.5 | 28731.5 | 84901.9 | 1 | PROCESSED | 54327.2611689815 | 54247 | 54035.4940625 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000029 | We propose to observe GRO J1655-40, a transient galactic black hole candidate. With M=~7 Msolar and distinct radio lobes, GRO J1655-40 has been classified as a microquasar. It was highly variable during the first few years after its discovery while showing irregular flaring and a wide range of continuum states. Discrete Fe K absorption structure was observed with ASCA. In the summer of 1997 it entered an extended quiescence that lasted for ~8 years. In March 2005 it became active again and XMM & Chandra have observed it since. Only Suzaku can provide the broadband sensitivity required to map the Fe K structure and the continuum as they change. GRO J1655-40 is rapidly declining and must be observed soon before it reenters quiescence. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | GRO J1655-40 | NULL | N | | A 2218 | 249.0001 | 66.203 | 97.724401 | 38.11892096 | 242.3617 | 53644.3643402778 | 53645.3446643518 | 100030010 | 43362.9 | 50000 | 43362.9 | 44717.3 | 43425.3 | 43824.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 41491.8 | 41491.8 | 84678 | 1 | PROCESSED | 54324.0657986111 | 54247 | 54035.7677314815 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000030 | Search of redshifted (z=0.171) OVII emission line from warm-hot intergalactic matter around a cluster which shows a merger feature in the line of sight, with no central cool component. The depth of the structure can be ~20 Mpc, and the redshift allows a clear separation of the lines from the Galactic hot gas. The low background and the superior resolution of XIS in the soft X-ray energy range will allow the best measurement of the WHIM emission so far. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | A2218 and its offset observation | NULL | N | | A2218_offset | 244.4769 | 65.4468 | 97.72059475 | 40.11912915 | 237.1965 | 53645.3474537037 | 53646.32375 | 100030020 | 44859.2 | 50000 | 44859.2 | 46190.7 | 44914.1 | 45374.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42536.6 | 42536.6 | 84343.9 | 0 | PROCESSED | 54412.4325115741 | 54247 | 54036.969224537 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000030 | Search of redshifted (z=0.171) OVII emission line from warm-hot intergalactic matter around a cluster which shows a merger feature in the line of sight, with no central cool component. The depth of the structure can be ~20 Mpc, and the redshift allows a clear separation of the lines from the Galactic hot gas. The low background and the superior resolution of XIS in the soft X-ray energy range will allow the best measurement of the WHIM emission so far. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | A2218 and its offset observation | NULL | N | | NGC3516 | 166.7299 | 72.5779 | 133.2179652 | 42.40001774 | 148.9366 | 53655.5813541667 | 53658.3801388889 | 100031010 | 134469.6 | 150000 | 134509.6 | 134595.6 | 134509.6 | 134469.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 122818 | 122818 | 241684.8 | 0 | PROCESSED | 54331.3324421296 | 54247 | 54036.4704976852 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000031 | NGC 3516 is one of the brightest Seyfert 1s seen in BAT currently visible to Suzaku. Recent BAT and RXTE observations show that this source is ~2-3 mCrb in the 2-10 keV band and ~4-5 mCrb in 15-100 keV. NGC 3516 is currently much brighter than when XMM observed it in 2000 (e.g., it has since returned to "typical" flux). This source's Fe K line and Compton reflection hump are both quite strong (e.g., as seen with SAX; R is ~1.8 in SAX data). | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | NGC 3516 | NULL | N | | ULXs in NGC 1313 | 49.5245 | -66.5352 | 283.41323765 | -44.63106544 | 172.6337 | 53658.556400463 | 53659.6252777778 | 100032010 | 32878 | 40000 | 32878 | 32878 | 32878 | 32878 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 30380 | 30380 | 92343.9 | 1 | PROCESSED | 54327.0733101852 | 54247 | 54036.1929398148 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000032 | We propose Suzaku observation of a nearby (4.5 Mpc) galaxy NGC 1313 hosting two prototypical ULXs. These ASCA specta of many ULXs were described with a "high temperature diskbb" model, spectra obtained with XMM (and Chandra) prefer a "power-law plus low-temperature disk" modeling. The superior 5-10 keV sensitivity of Suzaku allows us to examine whether the spectra of luminous ULXs indeed exhibit a turn-over around 5 keV or extend up to 10 keV. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | ULXs in NGC 1313 | NULL | N | | M82-Wind | 148.8893 | 69.7655 | 141.33880284 | 40.49464345 | 137.7608 | 53647.5072800926 | 53648.1418287037 | 100033010 | 32327.4 | 100000 | 32327.4 | 32327.4 | 32327.4 | 32327.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30222.4 | 30222.4 | 54802.1 | 0 | PROCESSED | 54327.0792592593 | 54247 | 54037.0057175926 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000033 | We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Largely Extended Emission (~12kpc) around M82 | NULL | N | | M82-Wind | 148.894 | 69.7643 | 141.33883884 | 40.49666381 | 146.246 | 53662.0401273148 | 53662.9390393518 | 100033020 | 40358.6 | 100000 | 40358.6 | 40382.6 | 40358.6 | 40366.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38353.3 | 38353.3 | 77658 | 0 | PROCESSED | 54324.7042708333 | 54247 | 54036.4196296296 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000033 | We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Largely Extended Emission (~12kpc) around M82 | NULL | N | | M82-Wind | 148.8885 | 69.7652 | 141.33933547 | 40.4945935 | 137.7608 | 53670.4681134259 | 53671.1002199074 | 100033030 | 28363.8 | 100000 | 28379.8 | 28379.8 | 28371.8 | 28363.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25812.1 | 25812.1 | 54604 | 1 | PROCESSED | 54320.7539930556 | 54247 | 54036.8639467593 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000033 | We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Largely Extended Emission (~12kpc) around M82 | NULL | N | | A 3376 | 90.5561 | -39.9584 | 246.50686261 | -25.98989573 | 107.6124 | 53649.6153703704 | 53653.4495833333 | 100034010 | 118779.2 | 150000 | 118779.2 | 121737.3 | 118849.8 | 119335.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 100540.1 | 100540.1 | 331253.7 | 3 | PROCESSED | 54331.7007060185 | 54247 | 54109.6396990741 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000034 | Abell 3376 (z=0.046) is a merging cluster with a T=4 keV (*3) hosting a pair of strong radio halos (see figure). It is one of the few clusters from which BeppoSAX positively detected excess hard X-rays (Nevalainen et al. ApJ 608, 166, 2004). Because of the relatively low temperature, the HXD-PIN energy band is expected to be relatively free from thermal emission, making this object ideal to the search for non-thermal signals. We expect the non-thermal flux to be 4-5% of the PIN background at 20 keV, and a 150 ksec on-source exposure would be needed to securely detect this. To know the current background over the full COR range, an off-source exposure for one day or a ~40 ksec exposure onto a very soft source, would be required immediately before or after the on-source data acquisition. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Diffuse Hard X-rays from Clusters | NULL | N | | Her X-1 | 254.465 | 35.3306 | 58.13562438 | 37.51514805 | 249.5714 | 53648.6450462963 | 53649.4341898148 | 100035010 | 36123.5 | 40000 | 36923.5 | 36123.5 | 36923.5 | 36923.5 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 33322.9 | 33322.9 | 68178 | 0 | PROCESSED | 54412.4794560185 | 54247 | 54036.0084375 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000035 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD Performance Verification using Her X-1 | NULL | N | | CYG X-1 | 299.5907 | 35.1892 | 71.32454904 | 3.06010347 | 276.9898 | 53648.2025347222 | 53648.6335532407 | 100036010 | 18213 | 20000 | 18213 | 18213 | 18213 | 18213 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18145.7 | 18145.7 | 37229.9 | 0 | PROCESSED | 54412.5121412037 | 54247 | 54037.7278819444 | 2.1.6.15 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000036 | We propose to probe the geometry of optically-thick accretion disks which should exist around a BH even in the hard state and to verify the HXD performance to thermal cut-off in hard X-rays expected from AGN. The 1st may be done by measuring the cool disk emission with the XIS-BI, resolving the fluorescent Fe-K line with the XIS-FI and detecting the reflection continuum with the HXD. Since these features are thought to come from the optically-thick disk a simultaneous measurement will for the 1st time allow for self-consistent constraining of the disk geometry in the hard state. Cyg X-1 is the best & most secure object for this stufy and is now in the low/hard state. A 20 ks Suzaku obs. is sufficient to get a fine spectrum up to 300 keV & to determine the cutoff with a high significance. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Cyg X-1 in the low state | NULL | N | | Sgr_A_west | 266.3063 | -29.1685 | 359.75676556 | -0.04750971 | 264.9604 | 53642.1914467593 | 53643.187025463 | 100037010 | 43741.2 | 50000 | 43741.2 | 43749.2 | 43749.2 | 43749.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39394.1 | 39394.1 | 86013.9 | 0 | PROCESSED | 54325.098900463 | 54247 | 54035.6663310185 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N | | 1A1742-294(GCBGD1) | 266.5239 | -29.5135 | 359.5610912 | -0.38914955 | 264.8673 | 53643.1880092593 | 53643.2536921296 | 100037020 | 3273 | 5000 | 3281 | 3273 | 3288.7 | 3281 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3091.1 | 3091.1 | 5671.9 | 0 | PROCESSED | 54389.6632638889 | 54247 | 54035.5547453704 | 2.1.6.14 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N | | KS1741-293(GCBGD2) | 266.2067 | -29.3539 | 359.55327497 | -0.0701996 | 265.0162 | 53643.254537037 | 53643.3203703704 | 100037030 | 2970 | 5000 | 2994 | 2986 | 2978 | 2970 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2824.4 | 2824.4 | 5679.9 | 0 | PROCESSED | 54389.6703819444 | 54247 | 54035.7774189815 | 2.1.6.14 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N | | Sgr_A_East | 266.5133 | -28.9266 | 0.05752244 | -0.07594372 | 264.7159 | 53643.3215393518 | 53644.2648611111 | 100037040 | 42917.6 | 50000 | 42957.6 | 42961.6 | 42917.6 | 42939.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39453.3 | 39453.3 | 81494 | 1 | PROCESSED | 54389.7149305556 | 54247 | 54035.7619675926 | 2.1.6.14 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N | | 1E1743.1-2843 GCBGD3 | 266.5944 | -28.6526 | 0.32852719 | 0.00581314 | 264.8798 | 53644.2657523148 | 53644.3162268518 | 100037050 | 2400 | 5000 | 2400 | 2400 | 2400 | 2400 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2232.9 | 2232.9 | 4353.9 | 0 | PROCESSED | 54320.5997453704 | 54247 | 54056.1970833333 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N | | Sgr_B2 | 266.8775 | -28.4435 | 0.63628385 | -0.09835114 | 265.3727 | 53653.5194560185 | 53655.2954050926 | 100037060 | 76596.6 | 100000 | 76628.6 | 76644.6 | 76596.6 | 76628.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 70819.2 | 70819.2 | 153431.9 | 0 | PROCESSED | 54329.7041666667 | 54247 | 54036.2262731482 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N | | Sgr_B2_BGD | 267.0943 | -28.1356 | 0.99854005 | -0.10262599 | 269.0208 | 53655.2988888889 | 53655.4620833333 | 100037070 | 9161.2 | 10000 | 9161.2 | 9164.3 | 9164.3 | 9163.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9536.4 | 9536.4 | 14092 | 0 | PROCESSED | 54320.6769560185 | 54247 | 54036.0749884259 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N | | NORTH POLAR SPUR | 260.5905 | 4.7489 | 26.83412197 | 21.95376599 | 264.1143 | 53646.4785763889 | 53647.4515277778 | 100038010 | 43068.9 | 50000 | 43148.9 | 44212.9 | 43068.9 | 43292.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 40771.5 | 40771.5 | 84001.9 | 0 | PROCESSED | 54412.4658680556 | 54247 | 54035.8928009259 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000038 | We propose to observe the North Polar Spur for 100 ksec. The main objectives are below (1) Search for emission lines of N and C that originates from low kT emission (2) Precisely determine the abundance of the NPS The measurement of N and C lines will be the first for XIS. This is also the first for extended sources. The first trial to measure the emission from the C-band (below 0.3keV) by using BI. This will be a guide line how to use the C-band data. Since the C-band intensity is already known, this will be the first calibration of the BI at low energy. The scientific objectives are already given in the mail distributed in the swg. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | North Polar Spur | NULL | N | | GRS1915+105 | 288.8014 | 10.9368 | 45.35928754 | -0.22611181 | 260.5762 | 53659.6951967593 | 53661.9724305556 | 100039010 | 84777.7 | 80000 | 85063.1 | 86430.5 | 85071.1 | 84777.7 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 68862.3 | 68862.3 | 196733.8 | 2 | PROCESSED | 54332.4893402778 | 54247 | 54043.8117476852 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000039 | This observation will be performed as a part of the big multiwavelength campain including Suzaku, VLA, Integral, RXTE, and Spitzer. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Campaign of coordinated observation of GRS 1915+105 | NULL | N | | MKN 3 | 93.8839 | 71.0477 | 143.2836301 | 22.71631463 | 71.8326 | 53665.0848263889 | 53667.2682175926 | 100040010 | 95026.5 | 100000 | 95026.5 | 95077.2 | 95045.2 | 95034.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 91344.1 | 91344.1 | 188629.9 | 0 | PROCESSED | 54329.9908796296 | 54247 | 53906.4896759259 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000040 | Mkn 3 is the second brightest Compton-thick Sy 2 currently visible with Suzaku. The broadband spectrum of Mkn 3, as probed by previous SAX and Chandra observations, is dominated by a reflection component (Compton hump strength R is near 1), but there is also evidence for a strongly absorbed hard X-ray power law that may be direct emission from the obscured nucleus, filtering through Compton-thick material (such as the molecular torus). | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | MKN 3 | HXD | N | | RXJ1856.5-3754 | 284.1498 | -37.9103 | 358.59888263 | -17.21635309 | 269.4259 | 53667.2829976852 | 53669.4793287037 | 100041010 | 76254.8 | 80000 | 0 | 76254.8 | 0 | 0 | 0 | 2 | 0 | 0 | 1 | 0 | 0 | 62621.7 | 62621.7 | 189720 | 3 | PROCESSED | 54330.4892476852 | 54247 | 54037.2294791667 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000041 | We propose Suzaku observation of a nearby isolated neuron star RXJ1856.5-3754 for the low energy QE calibration of the XIS. Our main purpose is, however, using this source as a soft X-ray QE calibrator on the sky. We hope this source will be observed again in future to check possible contamination on the filter surface etc. Note that the calibration is not only for the BI-CCD(XIS1), but also for FI-CCDs or relative QE among them. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | LOW ENERGY QE CALIBRATION OF XIS | XIS | N | | RXJ1856.5-3754 | 284.1433 | -37.91 | 358.59722216 | -17.21146697 | 84.0127 | 53817.9388078704 | 53819.4433217593 | 100041020 | 79169 | 80000 | 79177 | 79169 | 79177 | 79177 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53209.9 | 53209.9 | 129975.9 | 1 | PROCESSED | 54327.6521064815 | 54247 | 54042.2967824074 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000041 | We propose Suzaku observation of a nearby isolated neuron star RXJ1856.5-3754 for the low energy QE calibration of the XIS. Our main purpose is, however, using this source as a soft X-ray QE calibrator on the sky. We hope this source will be observed again in future to check possible contamination on the filter surface etc. Note that the calibration is not only for the BI-CCD(XIS1), but also for FI-CCDs or relative QE among them. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | LOW ENERGY QE CALIBRATION OF XIS | XIS | N | | CAS A | 350.8729 | 58.8094 | 111.74406014 | -2.13880346 | 214.7372 | 53768.5363657407 | 53768.833599537 | 100043010 | 0 | 10000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 10326.8 | 10326.8 | 25673.9 | 1 | PROCESSED | 54405.6122569444 | 54247 | 54040.7488888889 | 2.1.6.15 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N | | CAS A | 350.8761 | 58.8091 | 111.74552355 | -2.13963884 | 214.5537 | 53783.6003472222 | 53783.9218055556 | 100043020 | 14155 | 10000 | 14155 | 14155 | 14155 | 14155 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17371.3 | 17371.3 | 27768 | 0 | PROCESSED | 54322.8381018518 | 54247 | 54041.4627893518 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N | | E0102-72 | 15.9926 | -72.0236 | 301.56327722 | -45.07133229 | 226.8326 | 53720.0716203704 | 53723.4377199074 | 100044010 | 59731 | 20000 | 59735 | 125919.5 | 59731 | 59737 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 115330.2 | 115330.2 | 290803.7 | 1 | PROCESSED | 54331.8694907407 | 54247 | 54119.7612615741 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | NULL | N | | E0102-72 | 16.0206 | -72.0231 | 301.55102123 | -45.07123322 | 281.396 | 53752.9742708333 | 53755.3752199074 | 100044020 | 41260.5 | 20000 | 41268 | 41852.4 | 41260.5 | 41361 | 3 | 4 | 3 | 4 | 1 | 0 | 0 | 99793.5 | 99793.5 | 207429.8 | 3 | PROCESSED | 54331.0584375 | 54247 | 54040.6979513889 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N | | E0102-72 | 16.027 | -72.0223 | 301.54815221 | -45.07189388 | 294.0751 | 53768.8467592593 | 53769.4065393518 | 100044030 | 20827.7 | 20000 | 20835.7 | 20843.7 | 20843.7 | 20827.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20268.8 | 20268.8 | 48360 | 1 | PROCESSED | 54405.6412268518 | 54247 | 53905.6764351852 | 2.1.6.15 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N | | ETA CARINAE | 161.248 | -59.6859 | 287.58997588 | -0.63475906 | 156.124 | 53769.4163194444 | 53769.9481944444 | 100045010 | 21367.8 | 20000 | 21367.8 | 21367.8 | 21367.8 | 21367.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 18145.8 | 18145.8 | 45945.9 | 1 | PROCESSED | 54326.9105902778 | 54247 | 54040.9846643518 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N | | LOCKMANHOLE | 163.4063 | 57.6108 | 148.98193179 | 53.14624927 | 119.611 | 53688.2372337963 | 53689.8300694444 | 100046010 | 76980.6 | 100000 | 76980.6 | 77044.6 | 77012.6 | 77020.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 94510.7 | 94510.7 | 137607.9 | 3 | PROCESSED | 54329.2318634259 | 54247 | 54037.5889814815 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001098 | We propose a 100 ks observation of LockmanHole with Suzaku. The main purpose is to obtain a template dataset of HXD background. | CALIBRATION | 1 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 0 | SWG | BACKGROUND ESTABLISHMENT OF HXD | XIS | N | | GALACTIC CENTER | 266.5135 | -28.9269 | 0.05735731 | -0.07624929 | 270.2495 | 53986.0995833333 | 53987.3793402778 | 100048010 | 63007.9 | 50000 | 63007.9 | 63007.9 | 63007.9 | 63007.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60322.8 | 60322.8 | 110567.9 | 2 | PROCESSED | 54325.0017824074 | 54526 | 54056.4849189815 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | SWG | XIS FLIGHT CALIBRATION PLAN | XIS | N | | CYGNUS LOOP | 314.0345 | 31.9311 | 75.67403832 | -8.61676541 | 64.2261 | 53884.1556018518 | 53884.3793865741 | 100049010 | 8380.5 | 10000 | 8380.5 | 8380.5 | 8380.5 | 8380.5 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 6021.1 | 6021.1 | 19304 | 0 | PROCESSED | 54405.7350925926 | 54258 | 54059.411099537 | 2.1.6.15 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | SWG | XIS FLIGHT CALIBRATION PLAN | SPE | N | | CYGNUS LOOP | 314.0785 | 32.0438 | 75.78588033 | -8.57358243 | 64.2263 | 53884.3796759259 | 53884.6086342593 | 100049020 | 7892.8 | 10000 | 7892.8 | 7892.8 | 7892.8 | 7892.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 7452 | 7452 | 19769.9 | 0 | PROCESSED | 54405.7474074074 | 54258 | 54088.8429513889 | 2.1.6.15 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | SWG | XIS FLIGHT CALIBRATION PLAN | SPE | N | | CYGNUS LOOP | 313.9494 | 32.0818 | 75.74490282 | -8.46508453 | 64.2292 | 53884.6089236111 | 53884.8377777778 | 100049030 | 11697.1 | 10000 | 11705.1 | 11697.1 | 11705.1 | 11705.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 12268.8 | 12268.8 | 19772 | 0 | PROCESSED | 54405.7510763889 | 54258 | 54052.4915046296 | 2.1.6.15 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | SWG | XIS FLIGHT CALIBRATION PLAN | SPE | N | | CYGNUS LOOP | 313.9037 | 31.9696 | 75.63250703 | -8.50670526 | 64.2245 | 53884.8380671296 | 53885.0891666667 | 100049040 | 11765.6 | 10000 | 11781.6 | 11781.6 | 11773.6 | 11765.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9788 | 9788 | 21687.9 | 0 | PROCESSED | 54405.7566435185 | 54258 | 54052.5201157407 | 2.1.6.15 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | SWG | XIS FLIGHT CALIBRATION PLAN | SPE | N | | HER X-1 | 254.4224 | 35.4083 | 58.22535664 | 37.56185232 | 67.8783 | 53823.7669907407 | 53824.640462963 | 101001010 | 33062.1 | 40000 | 33062.1 | 38804.5 | 33062.1 | 33070.1 | 4 | 3 | 4 | 4 | 1 | 0 | 0 | 26222.8 | 26222.8 | 75437.9 | 0 | PROCESSED | 54327.3297800926 | 53826 | 53906.9875925926 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015002 | The main purpose of this observation is to calibrate the enery scale of HXD-GSO, which show a long-term decreasing trend. Another objective is to cross-calibrate the effective area between PIN and GSO. | CALIBRATION | 1 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATION OF HER X-1 FOR HXD CALIBRATION | HXD | N | | LOCKMAN HOLE | 162.9366 | 57.2557 | 149.70344314 | 53.20093146 | 281.8721 | 53872.7389583333 | 53874.7939583333 | 101002010 | 80398.2 | 80000 | 80398.2 | 80406.2 | 80406.2 | 80406.2 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 88854 | 88854 | 177513.8 | 4 | PROCESSED | 54329.1568865741 | 53826 | 53927.7689814815 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015003 | We propose an additional observation of the Lockman Hole for a purpose of the verification of the background (CXB+NXB) modeling of HXD. | CALIBRATION | 1 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATION OF LOCKMANHOLE | XIS | N | | CRAB | 83.6569 | 21.9577 | 184.61755594 | -5.79610428 | 250.9424 | 53830.5463425926 | 53831.5925115741 | 101003010 | 37832.3 | 40000 | 37832.3 | 37853.3 | 37832.3 | 37832.3 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 30989 | 30989 | 90379.9 | 1 | PROCESSED | 54328.6719444444 | 53826 | 53907.1306944445 | 2.0.6.13 | 5 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015004 | Crab cal at the XIS and HXD nominal positions. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB | HXD | N | | CRAB | 83.6371 | 22.0108 | 184.56259415 | -5.78319491 | 253.3318 | 53824.652650463 | 53825.1668865741 | 101004010 | 16363.2 | 20000 | 16363.2 | 16372.8 | 16365 | 16365 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9761.6 | 9761.6 | 44426 | 0 | PROCESSED | 54324.0120023148 | 53826 | 53906.0621875 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015004 | Crab cal at the XIS and HXD nominal positions. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB | XIS | N | | CRAB | 83.6368 | 22.0131 | 184.56049184 | -5.78219867 | 250.943 | 53829.1296643518 | 53829.5974305556 | 101004020 | 19138.9 | 20000 | 19138.9 | 19145.8 | 19138.9 | 19138.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13283.1 | 13283.1 | 40411.9 | 1 | PROCESSED | 54323.9096412037 | 53826 | 53906.6409375 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015004 | Crab cal at the XIS and HXD nominal positions. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB | XIS | N | | E0102.2-7219 | 16.0331 | -72.0338 | 301.54662861 | -45.06029066 | 8.2024 | 53841.404212963 | 53841.9793865741 | 101005010 | 21324 | 40000 | 21340 | 21324 | 21332 | 21340 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 16683.1 | 16683.1 | 49663.9 | 0 | PROCESSED | 54323.0970949074 | 53826 | 53905.6938425926 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | | E0102.2-7219 | 16.0278 | -72.0394 | 301.54948943 | -45.0548182 | 34.4136 | 53876.719525463 | 53877.1793287037 | 101005020 | 18161.9 | 20000 | 18161.9 | 18193.9 | 18161.9 | 18193.9 | 2 | 1 | 2 | 1 | 1 | 0 | 0 | 17763.3 | 17763.3 | 39719.9 | 0 | PROCESSED | 54323.0878703704 | 53826 | 53926.1422222222 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | | E0102.2-7219 | 16.0175 | -72.0405 | 301.55408267 | -45.05394165 | 60.6353 | 53912.8662731482 | 53913.4245833333 | 101005030 | 21675.8 | 20000 | 21715.8 | 21683.8 | 21715.8 | 21675.8 | 2 | 4 | 2 | 4 | 1 | 0 | 0 | 35062.6 | 35062.6 | 48203.9 | 0 | PROCESSED | 54326.9764467593 | 53826 | 53928.4586458333 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | | E0102.2-7219 | 15.9978 | -72.0424 | 301.56284618 | -45.05246644 | 92.9794 | 53933.2656597222 | 53933.9030439815 | 101005040 | 22063.4 | 20000 | 22063.4 | 22103.4 | 22063.4 | 22095.4 | 4 | 2 | 4 | 2 | 1 | 0 | 0 | 20982.3 | 20982.3 | 55047.9 | 1 | PROCESSED | 54327.0259606482 | 53826 | 53942.4630092593 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | | E0102.2-7219 | 15.9824 | -72.0369 | 301.56901677 | -45.05828014 | 133.8232 | 53972.2052662037 | 53973.3933333333 | 101005050 | 68363.2 | 20000 | 68987.2 | 68363.2 | 68987.2 | 68971.2 | 5 | 5 | 5 | 6 | 1 | 0 | 0 | 68002.4 | 68002.4 | 102633.9 | 1 | PROCESSED | 54329.2787962963 | 53826 | 54020.9929050926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | | E0102.2-7219 | 15.9812 | -72.0315 | 301.5690149 | -45.06369281 | 159.2453 | 53997.2263425926 | 53997.562662037 | 101005060 | 10790.7 | 40000 | 10806.7 | 10806.7 | 10790.7 | 10798.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 10322.3 | 10322.3 | 29050 | 0 | PROCESSED | 54323.1288425926 | 53826 | 54021.1325115741 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | | E0102.2-7219 | 15.9801 | -72.0277 | 301.56912514 | -45.06750714 | 192.8855 | 54029.650625 | 54030.2265625 | 101005070 | 37130.5 | 40000 | 37170.5 | 37130.5 | 37170.5 | 37162.5 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 36471.6 | 36471.6 | 49760 | 0 | PROCESSED | 54323.2554513889 | 53826 | 54055.5631828704 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 16.0029 | -72.0223 | 301.55865958 | -45.07240987 | 252.2709 | 54082.7869907407 | 54083.1279976852 | 101005090 | 28226 | 20000 | 28226 | 28226 | 0 | 28226 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23054.6 | 23054.6 | 29455.9 | 0 | PROCESSED | 54320.7912037037 | 53826 | 54094.5930324074 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 16.0137 | -72.0201 | 301.5537348 | -45.07437383 | 265.9905 | 54115.1395023148 | 54115.6655555556 | 101005100 | 22614 | 20000 | 22614 | 22614 | 0 | 22614 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19149.6 | 19149.6 | 45424 | 1 | PROCESSED | 54323.0598148148 | 53826 | 54132.8509490741 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | | E0102.2-7219 | 16.0273 | -72.0256 | 301.54834682 | -45.06859544 | 302.8131 | 54141.9262384259 | 54142.812662037 | 101005110 | 36093.8 | 20000 | 36101.8 | 36093.8 | 0 | 36101.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 52703.8 | 52703.8 | 76575.9 | 1 | PROCESSED | 54322.7344675926 | 53826 | 54153.2227430556 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 16.0373 | -72.0314 | 301.54456169 | -45.06259438 | 341.0006 | 54177.8828587963 | 54178.2994675926 | 101005120 | 18242 | 20000 | 18242 | 18250 | 0 | 18258 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14755.1 | 14755.1 | 35983.9 | 0 | PROCESSED | 54320.5929513889 | 53826 | 54185.4459027778 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | | PKS2155-304 | 329.7138 | -30.2259 | 17.72949775 | -52.24318888 | 57.9013 | 53856.2600925926 | 53857.2501041667 | 101006010 | 38551.5 | 30000 | 38551.5 | 38551.5 | 38551.5 | 38551.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 23947.6 | 23947.6 | 85514.1 | 2 | PROCESSED | 54327.1750694444 | 53826 | 53913.2773842593 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | | RXJ1856.5-3754 | 284.1489 | -37.9077 | 358.6011477 | -17.21474589 | 254.2953 | 54028.5128472222 | 54029.6405208333 | 101009010 | 40784.1 | 40000 | 40784.1 | 40784.1 | 40784.1 | 40784.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35169.9 | 35169.9 | 97403.9 | 1 | PROCESSED | 54324.6576851852 | 53826 | 54055.4732523148 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | | CRAB | 83.6301 | 22.0172 | 184.55366892 | -5.78525038 | 85.7026 | 53983.2227430556 | 53983.8196643518 | 101010010 | 20717.5 | 20000 | 20877.5 | 20717.5 | 20893.5 | 20885.5 | 3 | 2 | 3 | 3 | 1 | 0 | 0 | 19607.1 | 19607.1 | 51569.9 | 1 | PROCESSED | 54323.921412037 | 53826 | 54024.6695833333 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015014 | HXD cal. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 1 | AO1 | CRAB CAL FOR HXD ON 2006 AUTUMN | XIS | N | | THE CRAB OFFSETS | 83.6209 | 22.1323 | 184.45137768 | -5.73082135 | 85.7132 | 53983.8199537037 | 53983.8891087963 | 101011010 | 3348 | 2000 | 3348 | 3348 | 3348 | 3348 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3676 | 3676 | 5967.9 | 0 | PROCESSED | 54320.5337268518 | 53826 | 54104.4418287037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.6229 | 22.105 | 184.47554642 | -5.74387633 | 85.7146 | 53983.889212963 | 53983.9516087963 | 101011020 | 3350 | 2000 | 3350 | 3350 | 3350 | 3350 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3004 | 3004 | 5383.9 | 0 | PROCESSED | 54320.5378587963 | 53826 | 54104.4374189815 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.6254 | 22.076 | 184.50140903 | -5.75744861 | 85.7164 | 53983.951712963 | 53984.0904976852 | 101011030 | 6703 | 2000 | 6703 | 6703 | 6703 | 6703 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 5445.8 | 5445.8 | 11983.9 | 0 | PROCESSED | 54320.5911226852 | 53826 | 54104.972650463 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | HXD | N | | THE CRAB OFFSETS | 83.6274 | 22.0499 | 184.52456216 | -5.76985767 | 85.719 | 53984.0906018518 | 53984.1529976852 | 101011040 | 3353 | 2000 | 3353 | 3353 | 3353 | 3353 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2414 | 2414 | 5383.9 | 0 | PROCESSED | 54320.5453703704 | 53826 | 54104.4143518518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.6323 | 21.9916 | 184.57650041 | -5.79723168 | 85.7244 | 53984.1531944445 | 53984.2224421296 | 101011050 | 3355 | 2000 | 3355 | 3355 | 3355 | 3355 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2187 | 2187 | 5975.9 | 0 | PROCESSED | 54320.5475347222 | 53826 | 54104.4478587963 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.6331 | 21.9589 | 184.60466298 | -5.81410844 | 87.5062 | 53996.8758680556 | 53996.9515509259 | 101011060 | 3368 | 2000 | 3368 | 3368 | 3368 | 3368 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2716 | 2716 | 6527.9 | 0 | PROCESSED | 54320.4950115741 | 53826 | 54104.4231481482 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.6338 | 21.931 | 184.62870178 | -5.82849289 | 87.5103 | 53996.9516550926 | 53997.0140509259 | 101011070 | 2636 | 2000 | 2636 | 2636 | 2636 | 2636 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2157 | 2157 | 5383.9 | 0 | PROCESSED | 54320.4840046296 | 53826 | 54104.4160069444 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.6343 | 21.9041 | 184.65179297 | -5.84249768 | 87.5094 | 53997.0141550926 | 53997.0834953704 | 101011080 | 2251 | 2000 | 2251 | 2251 | 2251 | 2251 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2275 | 2275 | 5983.9 | 1 | PROCESSED | 54320.6079861111 | 53826 | 54104.4469675926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.7555 | 22.0251 | 184.60946275 | -5.68280554 | 87.8963 | 53997.0840625 | 53997.1529282407 | 101011090 | 1895 | 2000 | 1895 | 1895 | 1895 | 1895 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2081.5 | 2081.5 | 5945.9 | 0 | PROCESSED | 54320.6105092593 | 53826 | 54104.4517708333 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.7241 | 22.023 | 184.59560566 | -5.70852703 | 87.5484 | 53997.1534490741 | 53997.2154513889 | 101011100 | 1545 | 2000 | 1545 | 1545 | 1545 | 1545 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1806 | 1806 | 5356 | 0 | PROCESSED | 54320.4757060185 | 53826 | 54104.4337731482 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.6927 | 22.0229 | 184.58004352 | -5.7331758 | 85.756 | 53984.5680092593 | 53984.6252199074 | 101011110 | 2635.4 | 2000 | 2635.4 | 2635.4 | 2635.4 | 2635.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2457.3 | 2457.3 | 4942 | 0 | PROCESSED | 54320.6459375 | 53826 | 54104.4321527778 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.6616 | 22.0194 | 184.56751127 | -5.75940556 | 85.7473 | 53984.6253703704 | 53984.6876967593 | 101011120 | 2976.1 | 2000 | 2976.1 | 2976.1 | 2976.1 | 2976.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2802 | 2802 | 5380 | 0 | PROCESSED | 54320.6675115741 | 53826 | 54104.4254513889 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.5991 | 22.0137 | 184.54117278 | -5.81139714 | 85.7249 | 53984.6879398148 | 53984.7572222222 | 101011130 | 3366.1 | 2000 | 3366.1 | 3366.1 | 3366.1 | 3366.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3190 | 3190 | 5983.9 | 0 | PROCESSED | 54320.6656712963 | 53826 | 54104.4575 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.5675 | 22.0116 | 184.5271819 | -5.8372614 | 85.7131 | 53984.7573263889 | 53984.8197222222 | 101011140 | 3369 | 2000 | 3369 | 3369 | 3369 | 3369 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3632 | 3632 | 5383.9 | 0 | PROCESSED | 54320.6588425926 | 53826 | 54104.4270601852 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.536 | 22.0119 | 184.51119717 | -5.8617583 | 85.703 | 53984.8198263889 | 53984.8891666667 | 101011150 | 3370 | 2000 | 3370 | 3370 | 3370 | 3370 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3347.2 | 3347.2 | 5983.9 | 0 | PROCESSED | 54320.5381712963 | 53826 | 54104.9730439815 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | THE CRAB OFFSETS | 83.5056 | 22.0085 | 184.49889553 | -5.88737418 | 85.6939 | 53984.8892708333 | 53984.935 | 101011160 | 2765.1 | 2000 | 2765.1 | 2765.1 | 2765.1 | 2765.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2152 | 2152 | 3943.9 | 0 | PROCESSED | 54320.6432986111 | 53826 | 54104.4508449074 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | | PERSEUS CLUSTER | 49.9436 | 41.5175 | 150.56798595 | -13.25929387 | 66.0393 | 53976.788275463 | 53980.0793865741 | 101012010 | 150905.1 | 150000 | 150905.1 | 150921.1 | 150937.1 | 150921.1 | 6 | 6 | 6 | 6 | 1 | 0 | 0 | 142533.4 | 142533.4 | 284336 | 3 | PROCESSED | 54331.9796412037 | 53826 | 54024.8648726852 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015016 | We propose the observation of Perseus cluster for 150ks. To recover the energy resolution of the XIS, we will try the periodic charge injection method. However, the charge injection will change calibrations such as gain, QE and so on dramatically. To study the change of the clibrations, Perseus cluster is one of the best targets, because it is extended over the whole XIS FOV and the iron K line from the cluster is extremely strong. For the first 50ks, the observation will be done with the normal mode without the charge injection. For the second and third 50ks, we will do the charge injections with every 54 and 108 rows, repectively. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | PERSEUS OBSERVATION FOR CALIBRATIONS ON THE PERIODIC CHARGE INJECTION METHOD | XIS | Y | | PERSEUS CLUSTER | 49.9542 | 41.5047 | 150.58204074 | -13.26559499 | 258.6515 | 54136.6651388889 | 54137.6043287037 | 101012020 | 43871.4 | 40000 | 43895.4 | 43879.4 | 0 | 43871.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41573.2 | 41573.2 | 81137.9 | 1 | PROCESSED | 54326.7386111111 | 53826 | 54151.6542361111 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015017 | we propose observations for the XIS flight calibrations during the left term of AO-1. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS CALIBRATIONS FOR AO1 | XIS | Y | | CYGNUS LOOP | 314.0118 | 31.9912 | 75.70842949 | -8.56360013 | 217.4642 | 54090.3953935185 | 54090.6848842593 | 101013010 | 9102 | 10000 | 9102 | 9102 | 0 | 9102 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9212.6 | 9212.6 | 25006 | 1 | PROCESSED | 54320.6062962963 | 53826 | 54108.4571990741 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015017 | we propose observations for the XIS flight calibrations during the left term of AO-1. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS CALIBRATIONS FOR AO1 | XIS | Y | | CYGNUS LOOP | 314.0133 | 31.992 | 75.70987313 | -8.56406979 | 213.2117 | 54090.6869791667 | 54091.1175231482 | 101013020 | 21004 | 20000 | 21004 | 21004 | 0 | 21004 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18871.9 | 18871.9 | 37168 | 1 | PROCESSED | 54320.8528819444 | 53826 | 54132.7085763889 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015017 | we propose observations for the XIS flight calibrations during the left term of AO-1. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS CALIBRATIONS FOR AO1 | XIS | Y | | CYGNUS LOOP | 314.0129 | 31.9925 | 75.71004378 | -8.56348961 | 212.8468 | 54091.1180439815 | 54091.6036342593 | 101013030 | 19729.5 | 20000 | 19729.5 | 19729.5 | 0 | 19729.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20100.5 | 20100.5 | 41927.9 | 1 | PROCESSED | 54326.8660069444 | 53826 | 54132.7375694444 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 015017 | we propose observations for the XIS flight calibrations during the left term of AO-1. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS CALIBRATIONS FOR AO1 | XIS | Y | | E0102.2-7219 | 16.0421 | -72.0341 | 301.54273778 | -45.05979748 | 2.5391 | 54200.4410648148 | 54200.8127199074 | 102001010 | 18115 | 20000 | 18115 | 18115 | 0 | 18115 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24523 | 24523 | 32103.9 | 0 | PROCESSED | 54320.8671759259 | 54191 | 54210.6037268518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 16.0153 | -72.0406 | 301.55505042 | -45.05388895 | 60.6693 | 54264.42375 | 54265.1467476852 | 102002010 | 27871.7 | 20000 | 27871.7 | 27871.7 | 0 | 27871.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28315.5 | 28315.5 | 62463.9 | 1 | PROCESSED | 54320.758912037 | 54191 | 54271.4505092593 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 15.9919 | -72.0394 | 301.56512259 | -45.05558467 | 110.1956 | 54324.2230208333 | 54325.1565277778 | 102003010 | 39482 | 20000 | 39490 | 39482 | 0 | 39490 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 37350.5 | 37350.5 | 80647.9 | 1 | PROCESSED | 54404.4523611111 | 54191 | 54347.4795717593 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 15.9812 | -72.0282 | 301.56869429 | -45.06698503 | 193.1812 | 54398.5171875 | 54399.375162037 | 102004010 | 26175.7 | 20000 | 26175.7 | 26175.7 | 0 | 26175.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25480.7 | 25480.7 | 74093.8 | 0 | PROCESSED | 54407.5148148148 | 54191 | 54407.5260416667 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 16.0039 | -72.0219 | 301.55818443 | -45.07278758 | 249.4582 | 54435.8094907407 | 54436.4099421296 | 102005010 | 24766.7 | 20000 | 24766.7 | 24790.7 | 0 | 24790.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23722.3 | 23722.3 | 51871.9 | 1 | PROCESSED | 54441.0045833333 | 54191 | 54441.0108449074 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 16.0383 | -72.0304 | 301.54402708 | -45.06357038 | 338.1 | 54540.2385069444 | 54540.8648611111 | 102006010 | 28238.9 | 20000 | 28238.9 | 28238.9 | 0 | 28238.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38612.6 | 38612.6 | 54114 | 0 | PROCESSED | 54550.2177314815 | 54191 | 54550.2250347222 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | CYGNUS LOOP | 313.9884 | 32.004 | 75.70560343 | -8.54015129 | 44.0016 | 54263.5520833333 | 54263.8668402778 | 102007010 | 13345.5 | 10000 | 13353.5 | 13345.5 | 0 | 13353.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12560.7 | 12560.7 | 27191.9 | 1 | PROCESSED | 54320.8209722222 | 54191 | 54269.4117013889 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | CYGNUS LOOP | 314.0072 | 31.9862 | 75.70201861 | -8.56378367 | 248.0186 | 54437.219224537 | 54437.5627314815 | 102008010 | 13265.5 | 10000 | 13265.5 | 13265.5 | 0 | 13265.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13271.6 | 13271.6 | 29676 | 0 | PROCESSED | 54445.1796412037 | 54191 | 54445.1862731482 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | CYGNUS LOOP | 313.9882 | 32.0035 | 75.70510458 | -8.54033943 | 43.7589 | 54263.8673148148 | 54264.412025463 | 102009010 | 22896.5 | 20000 | 22896.5 | 22900.5 | 0 | 22916.5 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 18570.8 | 18570.8 | 47060 | 0 | PROCESSED | 54326.9052893518 | 54191 | 54269.4275462963 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | CYGNUS_LOOP_55FE | 314.0065 | 31.9862 | 75.70163572 | -8.56332634 | 247.7519 | 54437.5631597222 | 54438.1890740741 | 102010010 | 29585 | 20000 | 29585 | 29585 | 0 | 29585 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 27780.4 | 27780.4 | 54075.9 | 0 | PROCESSED | 54445.2233449074 | 54191 | 54451.4647916667 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | PERSEUS CLUSTER | 49.9461 | 41.5179 | 150.56936377 | -13.25792808 | 83.376 | 54327.5283449074 | 54328.477337963 | 102011010 | 42281.7 | 40000 | 42281.7 | 42281.7 | 0 | 42281.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36206.3 | 36206.3 | 81983.9 | 1 | PROCESSED | 54404.4795486111 | 54191 | 54347.6070833333 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | PERSEUS_CLUSTER_Normal | 49.9565 | 41.505 | 150.58334697 | -13.26439478 | 255.1861 | 54503.0900694444 | 54504.4377199074 | 102012010 | 61742.6 | 40000 | 61742.6 | 61742.6 | 0 | 61742.6 | 4 | 4 | 0 | 4 | 1 | 0 | 0 | 62315.7 | 62315.7 | 116399.9 | 0 | PROCESSED | 54546.3906828704 | 54191 | 54515.8301736111 | 2.2.7.18 | 2 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | GALACTIC CENTER | 266.5129 | -28.9278 | 0.05631549 | -0.07626904 | 265.2972 | 54346.7924768518 | 54348.2224537037 | 102013010 | 51396 | 50000 | 51396 | 51420 | 0 | 51404 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44477.8 | 44477.8 | 123535.8 | 0 | PROCESSED | 54404.4841319444 | 54191 | 54356.3951388889 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | RXJ1856.5-3754 | 284.1483 | -37.9083 | 358.60038232 | -17.21452318 | 271.9345 | 54388.7289930556 | 54389.587025463 | 102014010 | 41318 | 40000 | 41318 | 41318 | 0 | 41318 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40654.5 | 40654.5 | 74129.9 | 1 | PROCESSED | 54403.0509837963 | 54191 | 54403.060462963 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | RXJ1856.5-3754 | 284.1438 | -37.9098 | 358.59756743 | -17.21176167 | 89.7041 | 54547.2693402778 | 54548.4723842593 | 102015010 | 50652.3 | 40000 | 50652.3 | 50668.3 | 0 | 50652.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38365.4 | 38365.4 | 103923.8 | 2 | PROCESSED | 54566.3017592593 | 54191 | 54566.3157523148 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | | PSR 1509-58 AT NOM. | 228.4878 | -59.1337 | 320.32453924 | -1.16169081 | 289.2119 | 54333.5632060185 | 54334.1044444444 | 102016010 | 41213.8 | 40000 | 41221.8 | 41221.8 | 0 | 41213.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32908.4 | 32908.4 | 46759.9 | 1 | PROCESSED | 54404.4475347222 | 54191 | 54350.4146875 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025156 | PSR 1509-58 | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 2 | AO2 | PSR 1509-58 | XIS | Y | | PSR 1509-58 AT FIXEA | 228.4815 | -59.094 | 320.34236207 | -1.12606748 | 287.6329 | 54334.1057060185 | 54334.7690277778 | 102017010 | 43803.8 | 40000 | 43843.8 | 43827.8 | 0 | 43803.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37119.9 | 37119.9 | 57303.9 | 3 | PROCESSED | 54404.4777777778 | 54191 | 54350.6658449074 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025156 | PSR 1509-58 | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 2 | AO2 | PSR 1509-58 | XIS | Y | | LOCKMANHOLE | 162.9257 | 57.2581 | 149.70707974 | 53.19495056 | 319.512 | 54223.9667592593 | 54226.0835532407 | 102018010 | 96071.6 | 80000 | 96079.6 | 96079.6 | 0 | 96071.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92778 | 92778 | 182824.8 | 3 | PROCESSED | 54329.3278356482 | 54191 | 54230.4555902778 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025157 | The purpose of this observation is to verify the energy response of HXD-PIN/GSO. | CALIBRATION | 1 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | CALIBRATION OBSERVATION OF HXD WITH CRAB | XIS | Y | | CRAB | 83.6357 | 21.9546 | 184.60961134 | -5.81437304 | 269.3898 | 54179.4457407407 | 54180.6008912037 | 102019010 | 47633.1 | 40000 | 47633.1 | 47633.1 | 0 | 47633.1 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 43407.5 | 43407.5 | 99773.9 | 1 | PROCESSED | 54319.6803356482 | 54191 | 54314.6631597222 | 2.0.6.13 | 5 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025158 | The purpose of this observation is to verify the energy response of HXD-PIN/GSO. | CALIBRATION | 1 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | CALIBRATION OBSERVATION OF HXD WITH CRAB | HXD | Y | | PKS2155-304 | 329.716 | -30.2268 | 17.72837689 | -52.24517694 | 58.2058 | 54212.5208796296 | 54212.8488310185 | 102020010 | 12036.6 | 15000 | 12036.6 | 12036.6 | 0 | 12036.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10572 | 10572 | 28327.9 | 1 | PROCESSED | 54320.6566319444 | 54191 | 54217.2257523148 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025160 | This is a coordinated observation of PKS2155-304 with Chandra and XMM-Newton for spectral calibration. The observation also aims at evaluating the amount of contaminant on the XIS OBF. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 2 | AO2 | PKS2155-304 COORDINATED WITH CHANDRA AND XMM-NEWTON | XIS | Y | | E0102.2-7219 | 15.976 | -72.0294 | 301.57107704 | -45.06589786 | 179.7828 | 54371.2595833333 | 54371.6390509259 | 102021010 | 25314.6 | 12000 | 25314.6 | 25314.6 | 0 | 25314.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20225 | 20225 | 32781.9 | 0 | PROCESSED | 54402.263125 | 54191 | 54402.2749421296 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | N | | E0102.2-7219 | 16.0349 | -72.0243 | 301.54490568 | -45.06972875 | 306.7237 | 54510.7065740741 | 54512.1322222222 | 102022010 | 48424.5 | 40000 | 48424.5 | 48437.3 | 0 | 48432.5 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 46842.1 | 46842.1 | 123151.8 | 0 | PROCESSED | 54553.194837963 | 54191 | 54553.2132523148 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 025161 | 4 Calibration in Ao-2 phase. E0102-72 with PSUM mode and HXD lower gain operation. Her X-1 with XIS Timing mode. PSR B0545-69 for cross calibration of the absolute effective area. Perseus[cluster for gain calibration of 1/4 window mode. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 2 | AO2 | SUZAKU ADDITIONAL CALIBRATION | XIS | Y | | PSR B0540-69 | 85.0333 | -69.3191 | 279.70305196 | -31.5216772 | 241.3303 | 54512.1372337963 | 54513.444537037 | 102023010 | 52168.9 | 40000 | 52168.9 | 52168.9 | 0 | 52168.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46459 | 46459 | 112937.8 | 1 | PROCESSED | 54522.213599537 | 54191 | 54522.2283217593 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 025161 | 4 Calibration in Ao-2 phase. E0102-72 with PSUM mode and HXD lower gain operation. Her X-1 with XIS Timing mode. PSR B0545-69 for cross calibration of the absolute effective area. Perseus[cluster for gain calibration of 1/4 window mode. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 2 | AO2 | SUZAKU ADDITIONAL CALIBRATION | XIS | Y | | HER X-1 | 254.4589 | 35.3557 | 58.16585628 | 37.52408174 | 104.6168 | 54517.6276736111 | 54518.4863888889 | 102024010 | 38931 | 40000 | 38939 | 38931 | 0 | 38939 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34312.1 | 34312.1 | 74190 | 2 | PROCESSED | 54525.4793171296 | 54191 | 54525.4895138889 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 025161 | 4 Calibration in Ao-2 phase. E0102-72 with PSUM mode and HXD lower gain operation. Her X-1 with XIS Timing mode. PSR B0545-69 for cross calibration of the absolute effective area. Perseus[cluster for gain calibration of 1/4 window mode. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 2 | AO2 | SUZAKU ADDITIONAL CALIBRATION | XIS | Y | | E0102.2-7219 | 16.0298 | -72.0236 | 301.54705976 | -45.07053683 | 295.9817 | 54501.0571990741 | 54501.5245833333 | 102026010 | 0 | 15000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 19059.4 | 19059.4 | 40380 | 0 | PROCESSED | 54515.4175115741 | 54191 | 54515.8508912037 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 025162 | Recovery operation of XIS CPU HALT | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 2 | AO2 | XIS RECOVERY AND VERIFICATION | XIS | Y | | E0102.2-7219 | 16.0427 | -72.0346 | 301.54252595 | -45.05928576 | 1.5429 | 54564.6063888889 | 54565.2190277778 | 103001010 | 22361.5 | 20000 | 22377.5 | 22361.5 | 0 | 22377.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22318.5 | 22318.5 | 52926 | 1 | PROCESSED | 54580.9326388889 | 54557 | 54580.9409722222 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 16.0204 | -72.038 | 301.5525741 | -45.05637352 | 46.6005 | 54622.1603356482 | 54622.8557175926 | 103001020 | 21313 | 20000 | 21329 | 21313 | 0 | 21329 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19486.9 | 19486.9 | 60069.9 | 0 | PROCESSED | 54636.3151851852 | 54557 | 54636.3245833333 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 15.987 | -72.0401 | 301.56732456 | -45.05499026 | 122.9265 | 54690.9315740741 | 54691.5905555556 | 103001030 | 21301.8 | 20000 | 21309.8 | 21309.8 | 0 | 21301.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17083.1 | 17083.1 | 56929.9 | 0 | PROCESSED | 54710.2652662037 | 54557 | 54710.2804166667 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 15.9798 | -72.0267 | 301.56915878 | -45.06851113 | 190.5435 | 54761.1055092593 | 54761.6265277778 | 103001040 | 25405.2 | 20000 | 25405.2 | 25405.2 | 0 | 25405.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22263.6 | 22263.6 | 45005.9 | 1 | PROCESSED | 54778.0033101852 | 54557 | 54780.7231134259 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 16.0024 | -72.0211 | 301.55876018 | -45.07361767 | 248.5277 | 54813.5648263889 | 54814.3092476852 | 103001050 | 29618 | 20000 | 29633.6 | 29634 | 0 | 29618 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27676.9 | 27676.9 | 64293.9 | 0 | PROCESSED | 54839.9805439815 | 54557 | 54839.9906481482 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | E0102.2-7219 | 16.0385 | -72.0294 | 301.54384101 | -45.06456362 | 331.5978 | 54899.1304861111 | 54899.6454282407 | 103001060 | 23843.9 | 20000 | 23859.9 | 23843.9 | 0 | 23867.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21711.2 | 21711.2 | 44463.9 | 0 | PROCESSED | 54962.3705902778 | 54557 | 54916.3664814815 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | CYGNUS LOOP | 313.9898 | 32.0072 | 75.70886169 | -8.53902556 | 62.1393 | 54628.6164814815 | 54629.4703125 | 103002010 | 33166.9 | 10000 | 33166.9 | 33166.9 | 0 | 33166.9 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 29636.1 | 29636.1 | 73763.9 | 0 | PROCESSED | 54642.2957523148 | 54557 | 54655.4782523148 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | CYGNUS LOOP | 313.9023 | 31.8775 | 75.55993186 | -8.5644348 | 221.2652 | 54811.2228587963 | 54811.8571064815 | 103002020 | 21920.2 | 10000 | 21920.2 | 21920.2 | 0 | 21920.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19489.9 | 19489.9 | 54770 | 0 | PROCESSED | 54826.3421412037 | 54557 | 54826.3522569444 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | CYGNUS LOOP (WIN FE) | 313.9898 | 32.0072 | 75.70886169 | -8.53902556 | 62.1393 | 54628.6164814815 | 54629.4703125 | 103003010 | 33166.9 | 20000 | 33166.9 | 33166.9 | 0 | 33166.9 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 29636.1 | 29636.1 | 73763.9 | 0 | PROCESSED | 54642.3231597222 | 54557 | 54655.483287037 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | CYGNUS LOOP (WIN FE) | 313.902 | 31.8775 | 75.55976783 | -8.56423835 | 221.2647 | 54811.8571180556 | 54812.4321064815 | 103003020 | 26673.2 | 20000 | 26673.2 | 26673.2 | 0 | 26673.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22795.9 | 22795.9 | 49663.9 | 1 | PROCESSED | 54826.1622685185 | 54557 | 54828.3679166667 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | PERSEUS | 49.9468 | 41.518 | 150.56975635 | -13.25755566 | 86.8161 | 54691.602974537 | 54692.6204166667 | 103004010 | 40568.5 | 40000 | 40584.5 | 40568.5 | 0 | 40584.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31597.9 | 31597.9 | 87897.9 | 1 | PROCESSED | 54710.2585300926 | 54557 | 54710.2764467593 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | PERSEUS | 49.9546 | 41.5055 | 150.58184418 | -13.26476244 | 256.0759 | 54873.7298611111 | 54874.8141087963 | 103004020 | 50006.6 | 40000 | 50014.6 | 50014.6 | 0 | 50006.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44840.4 | 44840.4 | 93669.9 | 0 | PROCESSED | 54962.4890625 | 54557 | 54893.3133680556 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | PERSEUS (1/4WIN) | 49.9475 | 41.518 | 150.57020557 | -13.25726666 | 86.8158 | 54692.6204282407 | 54693.1071643518 | 103005010 | 21478 | 20000 | 21478 | 21501 | 0 | 21486 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 16992.2 | 16992.2 | 42049.9 | 0 | PROCESSED | 54710.3053125 | 54557 | 54780.5282291667 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | PERSEUS (1/4WIN) | 49.9551 | 41.5057 | 150.58205177 | -13.2643891 | 255.655 | 54874.8146759259 | 54875.4398032407 | 103005020 | 28816.2 | 20000 | 28816.2 | 28840.2 | 0 | 28824.2 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 26779.3 | 26779.3 | 53986 | 0 | PROCESSED | 54962.2071875 | 54557 | 54893.0113888889 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | RXJ1856.5-3754 | 284.1503 | -37.908 | 358.6012758 | -17.21588394 | 280.5087 | 54759.7973148148 | 54761.0974421296 | 103006010 | 43040.2 | 40000 | 43048.2 | 43048.2 | 0 | 43040.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37677.4 | 37677.4 | 112322 | 0 | PROCESSED | 54778.0592824074 | 54557 | 54780.5234837963 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y | | CRAB | 83.6308 | 22.0168 | 184.5543577 | -5.78491639 | 87.005 | 54705.3561458333 | 54706.218912037 | 103007010 | 39822 | 40000 | 39822 | 39822 | 0 | 39822 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32782.3 | 32782.3 | 74527.8 | 1 | PROCESSED | 54720.3652662037 | 54557 | 54780.5351851852 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 035002 | We are the HXD team. We propose Crab XIS nominal and HXD nominal observation, each with 40ks exposure for response calibration, a Lockman hole observation with 80 ks exposure for NXB+CXB long term stability study, and a 20ks Cyg X-1 observation for cross-check of Crab calibration. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 3 | AO3 | HXD CALIBRATIONS ON AO-3 | XIS | Y | | CRAB | 83.6295 | 22.0815 | 184.49878495 | -5.75129488 | 87.125 | 54710.3844560185 | 54711.412662037 | 103008010 | 45090 | 40000 | 45090 | 45090 | 0 | 45090 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33916.7 | 33916.7 | 88827.8 | 0 | PROCESSED | 54777.4816666667 | 54557 | 54780.4386458333 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 035002 | We are the HXD team. We propose Crab XIS nominal and HXD nominal observation, each with 40ks exposure for response calibration, a Lockman hole observation with 80 ks exposure for NXB+CXB long term stability study, and a 20ks Cyg X-1 observation for cross-check of Crab calibration. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 3 | AO3 | HXD CALIBRATIONS ON AO-3 | HXD | Y | | LOCKMANHOLE | 162.9369 | 57.2546 | 149.70462232 | 53.2017902 | 281.5296 | 54604.4635300926 | 54606.0529398148 | 103009010 | 83419.7 | 80000 | 83419.7 | 83419.7 | 0 | 83419.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87485.2 | 87485.2 | 137300 | 3 | PROCESSED | 54616.4074768518 | 54557 | 54616.4206597222 | 2.2.7.18 | 2 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 035002 | We are the HXD team. We propose Crab XIS nominal and HXD nominal observation, each with 40ks exposure for response calibration, a Lockman hole observation with 80 ks exposure for NXB+CXB long term stability study, and a 20ks Cyg X-1 observation for cross-check of Crab calibration. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 3 | AO3 | HXD CALIBRATIONS ON AO-3 | XIS | Y | | PKS2155-304 | 329.7153 | -30.2277 | 17.72680762 | -52.24467434 | 58.2307 | 54598.5708912037 | 54599.1120138889 | 103011010 | 23119 | 20000 | 23119 | 23119 | 0 | 23119 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17813.1 | 17813.1 | 46745.9 | 0 | PROCESSED | 54608.9835069444 | 54557 | 54608.9900115741 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 035003 | XMM/Chandra/Suzaku cross calibration by an coordinated observation of PKS215-304. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 3 | AO3 | COORDINATED OBSERVATION FOR CROSS-CALIBRATION WITH PKS2155-304 | XIS | Y | | CRAB | 83.6356 | 21.9544 | 184.60973125 | -5.81455843 | 269.3968 | 54923.0747337963 | 54924.0418287037 | 104001010 | 42105.2 | 40000 | 42808.5 | 42105.2 | 0 | 42808.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33587.7 | 33587.7 | 83539.8 | 0 | PROCESSED | 54945.440162037 | 54922 | 54949.4458680556 | 2.3.12.25 | 3 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045003 | N/A | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 4 | AO4 | CRAB CAL 2009 | HXD | Y | | CRAB | 83.6363 | 22.0087 | 184.56397797 | -5.78494551 | 270.0021 | 55250.0427199074 | 55251.1904976852 | 104001070 | 45830.9 | 40000 | 45830.9 | 45830.9 | 0 | 45830.9 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 16318 | 16318 | 99157.9 | 1 | PROCESSED | 55267.2501157407 | 54922 | 55267.2846643518 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045003 | N/A | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 4 | AO4 | CRAB CAL 2009 | XIS | Y | | LOCKMAN HOLE | 162.9377 | 57.2549 | 149.70376614 | 53.20190951 | 281.53 | 54994.3039351852 | 54996.0634375 | 104002010 | 92848.4 | 80000 | 92848.4 | 92848.4 | 0 | 92848.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79880 | 79880 | 152000 | 0 | PROCESSED | 55005.1218634259 | 54922 | 55005.1389814815 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045004 | HXD / XIS NXB/ CXB cal | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 4 | AO4 | LOCKMAN HOLE 2009 | XIS | Y | | LOCKMAN HOLE | 162.9419 | 57.2782 | 149.67240249 | 53.18794557 | 110.367 | 55161.4316319444 | 55161.7502199074 | 104002020 | 2359.1 | 12000 | 2383.1 | 2359.1 | 0 | 2375.1 | 5 | 2 | 0 | 3 | 1 | 0 | 0 | 10017.4 | 10017.4 | 27515.9 | 0 | PROCESSED | 55182.5883101852 | 54922 | 55182.6514467593 | 2.4.12.27 | 3 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045004 | HXD / XIS NXB/ CXB cal | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 4 | AO4 | LOCKMAN HOLE 2009 | XIS | Y | | PKS2155-304 | 329.7145 | -30.2263 | 17.72895666 | -52.2438339 | 83.4423 | 54978.6583217593 | 54980.486400463 | 104004010 | 62440.1 | 60000 | 62440.1 | 62440.1 | 0 | 62440.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53071.7 | 53071.7 | 157931.8 | 2 | PROCESSED | 54994.3203819444 | 54922 | 54994.3621296296 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045006 | This is a cross calibration observation with PKD2155-304 among Suzaku, XMM-Newton and Chandra. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 4 | AO4 | CROSS CALIBRATION OF SUZAKU/XMM/CHANDRA WITH PKS2155-304 | XIS | Y | | E0102-72 | 16.0343 | -72.0367 | 301.54639234 | -45.05737191 | 19.8885 | 54944.6369560185 | 54945.6225 | 104005010 | 45028.7 | 20000 | 45654.5 | 45028.7 | 0 | 45654.5 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 49726.9 | 49726.9 | 85135.8 | 1 | PROCESSED | 54966.3423958333 | 54922 | 54966.3543518518 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | E0102-72 | 16.0181 | -72.0439 | 301.55415549 | -45.05053701 | 69.1611 | 55008.1544097222 | 55008.571087963 | 104006010 | 22061.5 | 20000 | 22061.5 | 22061.5 | 0 | 22061.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16326.3 | 16326.3 | 35991.9 | 1 | PROCESSED | 55022.2321180556 | 54922 | 55022.2400694445 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | E0102-72 | 15.9824 | -72.0274 | 301.56809353 | -45.06775773 | 194.7588 | 55130.7598148148 | 55131.4169444444 | 104007010 | 20375.6 | 20000 | 20383.6 | 20383.6 | 0 | 20375.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18037.9 | 18037.9 | 56761.8 | 1 | PROCESSED | 55141.2386574074 | 54922 | 55141.2502777778 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | E0102-72 | 15.9813 | -72.0285 | 301.56867985 | -45.06668362 | 180.8386 | 55115.6048032407 | 55116.6237615741 | 104008010 | 31449.9 | 20000 | 31449.9 | 49641.1 | 0 | 49935.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43716.7 | 43716.7 | 88013.9 | 1 | PROCESSED | 55134.2097106482 | 54922 | 55134.4398842593 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | E0102-72 | 16.0091 | -72.0251 | 301.55623091 | -45.06948422 | 251.7193 | 55190.9159837963 | 55191.5411921296 | 104009010 | 21985.2 | 20000 | 21993.2 | 21985.2 | 0 | 21993.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21639.6 | 21639.6 | 54016 | 0 | PROCESSED | 55225.1324884259 | 54922 | 55225.1469328704 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | E0102-72 | 16.0186 | -72.0293 | 301.55250278 | -45.06509107 | 296.1745 | 55231.7435069444 | 55232.4343055556 | 104010010 | 20500.6 | 20000 | 20508.6 | 20500.6 | 0 | 20508.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24497.1 | 24497.1 | 59675.9 | 2 | PROCESSED | 55249.7128587963 | 54922 | 55249.7236111111 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | E0102-72 1/4 WIN | 15.9806 | -72.0277 | 301.56890722 | -45.06749655 | 189.3214 | 55124.8016203704 | 55125.3654282407 | 104011010 | 19091.3 | 20000 | 19091.3 | 20038.1 | 0 | 20038.1 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 16209 | 16209 | 48711.9 | 1 | PROCESSED | 55134.1666203704 | 54922 | 55134.1777777778 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | E0102-72 1/4 WIN | 16.0261 | -72.0284 | 301.54914583 | -45.06582801 | 296.9556 | 55232.435150463 | 55233.0002777778 | 104012010 | 23553.7 | 20000 | 23553.7 | 23553.7 | 0 | 23560 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25339.4 | 25339.4 | 48815.9 | 0 | PROCESSED | 55266.2249421296 | 54922 | 55266.2358449074 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | E0102-72 PSUM | 15.9904 | -72.0242 | 301.56429483 | -45.07078046 | 218.0047 | 55166.9023032407 | 55167.9336111111 | 104014010 | 62658.9 | 20000 | 63019.2 | 62658.9 | 0 | 63011.2 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 54915.1 | 54915.1 | 89091.8 | 1 | PROCESSED | 55181.2059259259 | 54922 | 55181.4406365741 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | N | | CYGNUS LOOP NE2 | 313.9438 | 31.9667 | 75.6521583 | -8.53477618 | 43.0005 | 54998.5732407407 | 54998.7883449074 | 104015010 | 10889.7 | 10000 | 10889.7 | 10889.7 | 0 | 10889.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9923 | 9923 | 18577.9 | 0 | PROCESSED | 55008.0992592593 | 54922 | 55008.1053356482 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | CYGNUS LOOP NE2 | 313.9634 | 31.9567 | 75.65508045 | -8.55396375 | 223.0007 | 55175.7922106482 | 55176.0640509259 | 104016010 | 12573.5 | 10000 | 12573.5 | 12573.5 | 0 | 12573.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10077.6 | 10077.6 | 23479.9 | 0 | PROCESSED | 55189.1092939815 | 54922 | 55189.115625 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | CYGNUS LOOP P8 | 313.9958 | 31.4752 | 75.29735897 | -8.88195371 | 62.5173 | 54998.7930787037 | 54999.0668865741 | 104017010 | 9708.7 | 10000 | 9708.7 | 9708.7 | 0 | 9708.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6711.9 | 6711.9 | 23652 | 1 | PROCESSED | 55108.9983101852 | 54922 | 55008.151087963 | 2.4.12.27 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | PERSEUS | 49.9444 | 41.5171 | 150.56872595 | -13.25929731 | 66.998 | 55069.1669907407 | 55070.1453009259 | 104018010 | 41279.8 | 40000 | 41279.8 | 41279.8 | 0 | 41295.8 | 4 | 3 | 0 | 3 | 1 | 0 | 0 | 37348.8 | 37348.8 | 84499.8 | 1 | PROCESSED | 55088.1088541667 | 54922 | 55088.1261458333 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | PERSEUS | 49.9512 | 41.4934 | 150.58651783 | -13.27626038 | 277.3248 | 55228.3356944444 | 55229.2502199074 | 104019010 | 38615.1 | 40000 | 38615.1 | 38615.1 | 0 | 38615.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35781.4 | 35781.4 | 78997.9 | 0 | PROCESSED | 55249.7809259259 | 54922 | 55249.7985069444 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | PERSEUS 1/4 WIN | 49.9444 | 41.516 | 150.56934906 | -13.260215 | 66.9976 | 55070.1453125 | 55071.500162037 | 104020010 | 55044.9 | 20000 | 55067.7 | 55052.9 | 0 | 55044.9 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 51280.2 | 51280.2 | 117049.8 | 2 | PROCESSED | 55106.3415277778 | 54922 | 55109.4175115741 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | PERSEUS 1/4 WIN | 49.9506 | 41.4949 | 150.58528271 | -13.27525693 | 276.9447 | 55229.250787037 | 55229.7078587963 | 104021010 | 21641.5 | 20000 | 21649.1 | 21646.9 | 0 | 21641.5 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 21574.3 | 21574.3 | 39482 | 0 | PROCESSED | 55249.7033912037 | 54922 | 55249.7129513889 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | RXJ1856.5 | 284.1483 | -37.909 | 358.59969969 | -17.21477781 | 277.829 | 55127.9550115741 | 55128.8363425926 | 104022010 | 43484.5 | 40000 | 43484.5 | 43492.5 | 0 | 43492.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39424.6 | 39424.6 | 76101.8 | 0 | PROCESSED | 55141.2708912037 | 54922 | 55141.2812384259 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | RXJ1856.5 | 284.0709 | -37.7784 | 358.70367738 | -17.11026819 | 79.4744 | 55269.4572569444 | 55270.6856944444 | 104022020 | 40415.2 | 40000 | 40426.9 | 40415.2 | 0 | 40415.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34577.2 | 34577.2 | 106107.9 | 0 | PROCESSED | 55285.0717939815 | 54922 | 55285.0858564815 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | RXJ1856.5 | 284.1421 | -37.9072 | 358.59959193 | -17.20956639 | 77.5864 | 55281.1527083333 | 55282.3710069444 | 104022030 | 42450.9 | 40000 | 42450.9 | 42450.9 | 0 | 42450.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11139.6 | 11139.6 | 105252 | 2 | PROCESSED | 55301.2699537037 | 54922 | 55301.2941203704 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y | | G21.5-0.9 | 278.3939 | -10.5728 | 21.49883061 | -0.89086145 | 264.65 | 55114.5957986111 | 55115.5953009259 | 104023010 | 40156.1 | 40000 | 40156.1 | 40156.1 | 0 | 40156.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30452.1 | 30452.1 | 86354 | 0 | PROCESSED | 55131.2417361111 | 54922 | 55131.2519675926 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 045008 | We propose G21.5-0.9 observation for the cross-calibtaions of XIS. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 4 | AO4 | CROSS CALIBRATION OF G21.5-0.9 | XIS | Y | | PKS2155-304 | 329.7122 | -30.2251 | 17.73054892 | -52.24172704 | 58.9372 | 55313.9868171296 | 55315.8536458333 | 105001010 | 63457.2 | 60000 | 63465.2 | 63471 | 0 | 63457.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54701.5 | 54701.5 | 161277.8 | 2 | PROCESSED | 55327.3554976852 | 55287 | 55327.3816087963 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055001 | This observation of PKS2155-304 is coordinated with XMM-Newton and Chandra. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 5 | AO5 | COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTON | XIS | Y | | CRAB | 83.6381 | 22.0079 | 184.56555504 | -5.78396412 | 269.4791 | 55291.5258680556 | 55292.5001273148 | 105002010 | 481.5 | 40000 | 481.5 | 481.6 | 0 | 481.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33897.4 | 33897.4 | 84133.8 | 1 | PROCESSED | 55350.3157291667 | 55287 | 55350.3368981482 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055002 | We propose an annual calibration of Crab, as a standard candle from 1 kev upto 500 keV. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 5 | AO5 | AO-5 CRAB CALIBRATION | XIS | Y | | LOCKMAN_HOLE | 162.9382 | 57.2507 | 149.70866001 | 53.20492954 | 279.8869 | 55358.311875 | 55360.0828935185 | 105003010 | 77997.6 | 80000 | 78013.6 | 77997.6 | 0 | 78258.3 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 73083.2 | 73083.2 | 152981.8 | 1 | PROCESSED | 55370.3136921296 | 55287 | 55370.3379861111 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055003 | 2010 Annual observation of Lockman hole, with XIS in the Psum mode. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 5 | AO5 | LOCKMAN HOLE | XIS | N | | E0102-72 | 16.0161 | -72.0335 | 301.55400478 | -45.06095473 | 357.7405 | 55291.0014699074 | 55291.5147453704 | 105004010 | 21592.8 | 20000 | 21592.8 | 21592.8 | 0 | 21592.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17139 | 17139 | 44311.9 | 0 | PROCESSED | 55306.2070486111 | 55287 | 55306.2144328704 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | E0102-72 | 16.0035 | -72.0383 | 301.55996349 | -45.05643533 | 65.2308 | 55366.1296412037 | 55366.7869791667 | 105004020 | 19230.2 | 20000 | 19238.2 | 19238.2 | 0 | 19230.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16589.5 | 16589.5 | 56783.9 | 2 | PROCESSED | 55413.2677199074 | 55287 | 55413.4019097222 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | E0102-72 | 16.00833 | -72.03131 | 301.55717515 | -45.06330557 | -99 | NULL | NULL | 105004030 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 55287 | NULL | NULL | NULL | NULL | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | N | | E0102-72 | 16.0129 | -72.0282 | 301.55487873 | -45.06631044 | 194.5389 | 55495.8125694444 | 55496.3217939815 | 105004040 | 20018.9 | 20000 | 20619.9 | 20018.9 | 0 | 20643.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19219.3 | 19219.3 | 43988 | 0 | PROCESSED | 55505.2191666667 | 55287 | 55505.2302893518 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | E0102-72 | 16.0026 | -72.0263 | 301.55918173 | -45.06842583 | 227.0923 | 55539.0256481482 | 55539.487662037 | 105004050 | 20046.8 | 20000 | 20070.8 | 20070.8 | 0 | 20046.8 | 1 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 39913.9 | 0 | PROCESSED | 55551.4886921296 | 55287 | 55552.4359953704 | 2.5.16.29 | 2 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | E0102-72 | 16.0173 | -72.0347 | 301.55359992 | -45.05973194 | 299.5457 | 55600.0152430556 | 55600.4516319444 | 105004060 | 17242.6 | 20000 | 17258.6 | 17242.6 | 0 | 17258.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13743.2 | 13743.2 | 37695.9 | 0 | PROCESSED | 55614.7171643518 | 55287 | 55617.4086805556 | 2.5.16.29 | 2 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | E0102-72_1_4_WIN | 16.0018 | -72.0347 | 301.56035188 | -45.06006295 | 65.8655 | 55366.7877314815 | 55367.3098842593 | 105005010 | 20345.6 | 20000 | 20353.6 | 20345.6 | 0 | 20361.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17482.3 | 17482.3 | 45080 | 2 | PROCESSED | 55400.2717476852 | 55287 | 55400.4271412037 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | E0102-72_1_4_WIN | 16.0156 | -72.0284 | 301.55372169 | -45.06605315 | 226.5285 | 55539.4883680556 | 55540.2502546296 | 105005020 | 22538.8 | 20000 | 22546.8 | 22538.8 | 0 | 22554.8 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 5796.9 | 5796.9 | 65821.9 | 2 | PROCESSED | 55550.9296875 | 55287 | 55550.9436689815 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | E0102-72_PSUM | 15.883 | -72.0319 | 301.61184542 | -45.06533979 | 66.3881 | 55367.3105439815 | 55368.5202314815 | 105006010 | 356.5 | 40000 | 356.5 | 356.5 | 0 | 356.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 303 | 303 | 36191.9 | 0 | PROCESSED | 55400.3158564815 | 55287 | 55400.4299537037 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | N | | E0102-72_PSUM | 16.0136 | -72.0296 | 301.55471109 | -45.06489883 | 226.8844 | 55537.8034375 | 55539.0252199074 | 105006020 | 40871.5 | 40000 | 40936.3 | 40871.5 | 0 | 41120.5 | 4 | 3 | 0 | 1 | 1 | 0 | 0 | 157.4 | 157.4 | 105549.9 | 0 | PROCESSED | 55777.5091898148 | 55287 | 55778.433275463 | 2.7.16.30 | 4 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | N | | E0102-72_PSUM | 16.0081 | -72.0302 | 301.5571666 | -45.06441782 | 138.5223 | 55437.769525463 | 55438.8884606482 | 105006030 | 37067.5 | 40000 | 37083.1 | 37067.5 | 0 | 37636.5 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 33043.8 | 33043.8 | 96641.9 | 1 | PROCESSED | 55449.0119328704 | 55287 | 55449.0261574074 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | N | | CYGNUS LOOP P8 | 313.9885 | 31.4813 | 75.29810685 | -8.87326903 | 62.5188 | 55358.0139583333 | 55358.3015393518 | 105007010 | 12093.9 | 10000 | 12881.6 | 12093.9 | 0 | 12889.6 | 2 | 3 | 0 | 2 | 1 | 0 | 0 | 9985.5 | 9985.5 | 24839.9 | 0 | PROCESSED | 55370.6569675926 | 55287 | 55376.4220717593 | 2.5.16.28 | 2 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | CYGNUS LOOP P8 CI 6 | 314.021 | 31.4644 | 75.3027873 | -8.90540252 | 222.2994 | 55552.9622569444 | 55553.0467824074 | 105007020 | 2740 | 10000 | 2755.6 | 2740 | 0 | 2755.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2487.4 | 2487.4 | 7295.9 | 0 | PROCESSED | 55593.253125 | 55287 | 55593.2584722222 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | CYGNUS LOOP P8 CI 2 | 314.0088 | 31.4691 | 75.29974588 | -8.89438689 | 222.2165 | 55553.0469791667 | 55553.1446990741 | 105007030 | 4963.1 | 10000 | 4987 | 4979 | 0 | 4963.1 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 3566.5 | 3566.5 | 8431.9 | 0 | PROCESSED | 55593.2589930556 | 55287 | 55593.2653587963 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | RXJ1856.5-3754 | 284.1491 | -37.9166 | 358.59252855 | -17.21813017 | 271.239 | 55496.329537037 | 55497.4509722222 | 105008010 | 40091.7 | 40000 | 40091.7 | 40099.7 | 0 | 40107.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32908.1 | 32908.1 | 96875.8 | 0 | PROCESSED | 55509.0452546296 | 55287 | 55509.0637731482 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | PERSEUS | 49.9406 | 41.5199 | 150.56470121 | -13.25852998 | 66.581 | 55417.3825925926 | 55418.010625 | 105009010 | 33624.2 | 40000 | 33624.2 | 33624.2 | 0 | 33624.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37659.6 | 37659.6 | 54254 | 0 | PROCESSED | 55428.0437037037 | 55287 | 55428.0593171296 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | PERSEUS | 49.9557 | 41.5028 | 150.58408011 | -13.26656036 | 259.7325 | 55595.0249421296 | 55595.9578472222 | 105009020 | 40461.1 | 40000 | 40469.1 | 40461.1 | 0 | 40477.1 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 29594.3 | 29594.3 | 80593.9 | 1 | PROCESSED | 55610.2551967593 | 55287 | 55610.273587963 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | PERSEUS_1_4_WIN | 49.9403 | 41.521 | 150.56388564 | -13.25773608 | 66.5805 | 55418.0106365741 | 55418.6467476852 | 105010010 | 27372.7 | 20000 | 27372.7 | 27380.4 | 0 | 27386.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33712.7 | 33712.7 | 54955.9 | 1 | PROCESSED | 55428.0581481482 | 55287 | 55428.0721759259 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | PERSEUS_1_4_WIN | 49.9552 | 41.5037 | 150.58324921 | -13.26601613 | 259.969 | 55594.4623958333 | 55595.0245138889 | 105010020 | 21092.6 | 20000 | 21096.3 | 21096.3 | 0 | 21092.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16573 | 16573 | 48559.9 | 0 | PROCESSED | 55610.2520486111 | 55287 | 55610.2645717593 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | N132D | 81.279 | -69.6505 | 280.31295018 | -32.77613267 | 32.9954 | 55404.1821296296 | 55405.1411226852 | 105011010 | 35849.5 | 30000 | 35849.5 | 35849.5 | 0 | 35849.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32540.9 | 32540.9 | 82839.8 | 1 | PROCESSED | 55414.0839236111 | 55287 | 55414.1006828704 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055005 | We propose a observation of N132D for the calibration of the XIS in the AO5 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | CRAB_80OFF_0DEG | 83.6952 | 20.686 | 185.71797799 | -6.44521522 | 87.4149 | 55452.6214467593 | 55453.046712963 | 105012010 | 19241.5 | 20000 | 19241.5 | 19241.5 | 0 | 19241.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17364.4 | 17364.4 | 36736 | 0 | PROCESSED | 55463.1437962963 | 55287 | 55463.4094212963 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_80OFF_22.5DEG | 83.1525 | 20.7619 | 185.38009186 | -6.83349718 | 86.9209 | 55453.0474189815 | 55453.4918518518 | 105013010 | 18989.1 | 20000 | 18989.1 | 18989.1 | 0 | 18989.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13723 | 13723 | 38376 | 0 | PROCESSED | 55463.1640509259 | 55287 | 55463.4117013889 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_80OFF_45DEG | 82.6663 | 21.0307 | 184.90557346 | -7.07161845 | 87.0482 | 55453.4925578704 | 55453.9550115741 | 105014010 | 20599.2 | 20000 | 20607.2 | 20607.2 | 0 | 20599.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19812.1 | 19812.1 | 39937.9 | 2 | PROCESSED | 55463.1749189815 | 55287 | 55463.4144675926 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_50OFF_45DEG | 83.0202 | 21.413 | 184.76043538 | -6.58765564 | 87.6753 | 55431.8338194445 | 55432.0682291667 | 105015010 | 10549.2 | 10000 | 11277.2 | 10549.2 | 0 | 11277.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10191.7 | 10191.7 | 20245.9 | 1 | PROCESSED | 55446.2122800926 | 55287 | 55446.446875 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_50OFF_135DEG | 82.9576 | 22.5813 | 183.73915584 | -6.0064164 | 86.6565 | 55432.0694907407 | 55432.3105555556 | 105016010 | 6489.4 | 10000 | 6489.4 | 6497.4 | 0 | 6497.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 3638.1 | 3638.1 | 20822 | 0 | PROCESSED | 55446.2337268518 | 55287 | 55446.4488425926 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_50OFF_225DEG | 84.2344 | 22.6444 | 184.32067652 | -4.97776831 | 87.1427 | 55432.3115856482 | 55432.5827777778 | 105017010 | 12345.6 | 10000 | 12353.6 | 12345.6 | 0 | 12361.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12151 | 12151 | 23423.9 | 0 | PROCESSED | 55447.2142824074 | 55287 | 55447.4086921296 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_50OFF_315DEG | 84.2968 | 21.4693 | 185.35120349 | -5.55324373 | 87.1743 | 55432.5838078704 | 55432.8980555556 | 105018010 | 14432.3 | 10000 | 14432.3 | 14456.3 | 0 | 14440.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12415.6 | 12415.6 | 27143.9 | 1 | PROCESSED | 55447.2415509259 | 55287 | 55447.4099884259 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_65OFF_0DEG | 83.6859 | 20.9369 | 185.49975653 | -6.31874712 | 87.2696 | 55446.25 | 55446.4605439815 | 105019010 | 9657.5 | 10000 | 9657.5 | 9657.5 | 0 | 9657.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7899.5 | 7899.5 | 18183.9 | 0 | PROCESSED | 55460.9539583333 | 55287 | 55461.3910763889 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_65OFF_45DEG | 82.8482 | 21.2156 | 184.84096902 | -6.82899548 | 86.9607 | 55446.4614351852 | 55446.6875694444 | 105020010 | 9450.4 | 10000 | 9458.4 | 9450.4 | 0 | 9458.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7906.9 | 7906.9 | 19533.9 | 0 | PROCESSED | 55460.9663888889 | 55287 | 55461.3925231482 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_65OFF_90DEG | 82.4629 | 21.9742 | 184.00329077 | -6.72000946 | 87.3211 | 55446.6885532407 | 55446.9076967593 | 105021010 | 10912 | 10000 | 10921.9 | 10920 | 0 | 10912 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10033.9 | 10033.9 | 18930 | 0 | PROCESSED | 55460.9870486111 | 55287 | 55461.3931944444 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_65OFF_135DEG | 82.7613 | 22.7517 | 183.49649927 | -6.06655162 | 87.038 | 55446.9086805556 | 55447.1314236111 | 105022010 | 9248.2 | 10000 | 9248.2 | 9248.2 | 0 | 9248.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7939.3 | 7939.3 | 19237.9 | 0 | PROCESSED | 55466.1589814815 | 55287 | 55466.4006365741 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_65OFF_180DEG | 83.5739 | 23.1022 | 183.60559643 | -5.24730073 | 87.2466 | 55447.1322685185 | 55447.3557291667 | 105023010 | 11470.6 | 10000 | 11470.6 | 11478.6 | 0 | 11478.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10091.3 | 10091.3 | 19295.9 | 0 | PROCESSED | 55461.0497453704 | 55287 | 55461.3950810185 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_65OFF_225DEG | 84.3921 | 22.8458 | 184.22714627 | -4.7474889 | 85.6608 | 55447.3571296296 | 55447.5793402778 | 105024010 | 9404.2 | 10000 | 9412.2 | 9404.2 | 0 | 9420.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7822.5 | 7822.5 | 19191.9 | 0 | PROCESSED | 55461.0795949074 | 55287 | 55461.3963541667 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_65OFF_270DEG | 84.7966 | 22.0949 | 185.06495422 | -4.82832438 | 86.3168 | 55447.5802777778 | 55447.7918287037 | 105025010 | 8891 | 10000 | 8891 | 8891 | 0 | 8891 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8535 | 8535 | 18273.9 | 0 | PROCESSED | 55461.1209143518 | 55287 | 55461.3998032407 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | CRAB_65OFF_315DEG | 84.4913 | 21.2878 | 185.60226135 | -5.4958009 | 87.6059 | 55447.7930902778 | 55448.0217824074 | 105026010 | 11382 | 10000 | 11390 | 11390 | 0 | 11382 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9884.1 | 9884.1 | 19750 | 0 | PROCESSED | 55461.1300578704 | 55287 | 55461.4004050926 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y | | PERSEUS_CI_6 | 49.9577 | 41.5001 | 150.58689381 | -13.26798644 | 252.2456 | 55614.2081365741 | 55615.187662037 | 105027010 | 45272.2 | 40000 | 45905.5 | 45272.2 | 0 | 45905.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41885.9 | 41885.9 | 84609.8 | 0 | PROCESSED | 55624.2063194444 | 55287 | 55624.2249421296 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | PERSEUS_1_4_WIN_CI_6 | 49.9565 | 41.5014 | 150.58538691 | -13.26739774 | 252.427 | 55613.7422106482 | 55614.2078009259 | 105028010 | 20636.3 | 20000 | 20636.3 | 20636.3 | 0 | 20636.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17845 | 17845 | 40215.9 | 0 | PROCESSED | 55624.1538657407 | 55287 | 55624.1639814815 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y | | CRAB | 83.6359 | 22.0094 | 184.56318415 | -5.78488405 | 269.6199 | 55641.8131828704 | 55643.1459490741 | 105029010 | 614.6 | 40000 | 614.6 | 614.6 | 0 | 614.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36940.8 | 36940.8 | 115139.9 | 0 | PROCESSED | 55652.144375 | 55287 | 55652.1669097222 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 055002 | We propose an annual calibration of Crab, as a standard candle from 1 kev upto 500 keV. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 5 | AO5 | AO-5 CRAB CALIBRATION | XIS | Y | | LOCKMAN HOLE | 162.9265 | 57.2528 | 149.71315343 | 53.19882847 | 305.9894 | 55685.7406712963 | 55686.7675925926 | 106001010 | 42278 | 40000 | 42278 | 43590.5 | 0 | 44442.7 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 57821.4 | 57821.4 | 88709.8 | 0 | PROCESSED | 55768.7908217593 | 55652 | 55768.8116898148 | 2.6.16.30 | 3 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | N | | E0102-72 CI 6 | 15.9973 | -72.0342 | 301.56226334 | -45.06065755 | 3.8307 | 55662.8284490741 | 55663.3522569444 | 106002010 | 20386.2 | 30000 | 20386.2 | 20386.2 | 0 | 20386.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17842 | 17842 | 45247.9 | 0 | PROCESSED | 55687.536400463 | 55652 | 55690.5690625 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | E0102-72 | 16.0024 | -72.0368 | 301.56029587 | -45.05795518 | 69.5441 | 55741.0977314815 | 55741.5828009259 | 106002020 | 28782 | 30000 | 28790 | 28798 | 0 | 28782 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24611.5 | 24611.5 | 41903.9 | 1 | PROCESSED | 55775.2410069444 | 55652 | 55775.250150463 | 2.6.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | E0102-72 | 16.001 | -72.0295 | 301.56019202 | -45.06526758 | 183.1599 | 55848.6463310185 | 55849.0905092593 | 106002030 | 32817.5 | 30000 | 32825.5 | 32817.5 | 0 | 32825.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29913.7 | 29913.7 | 38361.9 | 0 | PROCESSED | 55872.9987615741 | 55652 | 55873.0106597222 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | E0102-72 | 16.0145 | -72.0334 | 301.55469199 | -45.06108873 | 340.2388 | 56003.3836574074 | 56004.1619444445 | 106002040 | 32378 | 30000 | 32394 | 32378 | 0 | 32394 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30718 | 30718 | 67244 | 0 | PROCESSED | 56019.2667592593 | 55652 | 56019.2768518518 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | E0102-72 CI 2 | 15.9944 | -72.0366 | 301.5637608 | -45.05832492 | 4.3228 | 55663.352962963 | 55663.8890740741 | 106002050 | 20814.3 | 20000 | 20825.2 | 20822.2 | 0 | 20814.3 | 2 | 3 | 0 | 2 | 1 | 0 | 0 | 19623.9 | 19623.9 | 46318 | 0 | PROCESSED | 55687.5378356482 | 55652 | 55690.5705439815 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | E0102-72_1_4_WIN | 16.0104 | -72.0348 | 301.55661541 | -45.05977973 | 4.7976 | 55663.8897337963 | 55664.4098726852 | 106003010 | 16829.5 | 30000 | 16829.5 | 18277.5 | 0 | 18277.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16956.4 | 16956.4 | 44931.9 | 0 | PROCESSED | 55687.5426041667 | 55652 | 55690.5713310185 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | E0102-72_1_4_WIN | 16.0013 | -72.0289 | 301.56000261 | -45.06585975 | 183.5797 | 55849.0910763889 | 55849.5446643518 | 106003020 | 31657.1 | 30000 | 31657.1 | 31753.1 | 0 | 31769.1 | 4 | 3 | 0 | 3 | 1 | 0 | 0 | 24464.3 | 24464.3 | 39183.9 | 0 | PROCESSED | 55873.0320949074 | 55652 | 55873.0426736111 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | CYGNUS_LOOP_P8 | 313.9841 | 31.4885 | 75.30130763 | -8.86579122 | 62.5162 | 55721.2910763889 | 55721.5835532407 | 106004010 | 11551.1 | 10000 | 11559.1 | 11567.1 | 0 | 11551.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10646.2 | 10646.2 | 25255.9 | 0 | PROCESSED | 55748.5317476852 | 55652 | 55757.6943287037 | 2.6.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | CYGNUS_LOOP_P8 | 314.0101 | 31.4557 | 75.29000417 | -8.90377623 | 240.0029 | 55915.0575231482 | 55915.3196527778 | 106004020 | 11990 | 10000 | 11990 | 11990 | 0 | 11990 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12321.2 | 12321.2 | 22643.9 | 0 | PROCESSED | 55932.0868402778 | 55652 | 55932.095162037 | 2.7.16.31 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | PERSEUS | 49.9433 | 41.526 | 150.56297877 | -13.25232631 | 83.8173 | 55769.5188888889 | 55770.5467939815 | 106005010 | 40838.2 | 40000 | 40854.2 | 40838.2 | 0 | 40963.1 | 2 | 3 | 0 | 2 | 1 | 0 | 0 | 36688.5 | 36688.5 | 88801.9 | 1 | PROCESSED | 55792.3044212963 | 55652 | 55792.3246990741 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | N | | PERSEUS | 49.9531 | 41.5016 | 150.58309121 | -13.26863527 | 261.9986 | 55964.8470138889 | 55965.9169328704 | 106005020 | 46813.8 | 40000 | 46813.8 | 46813.8 | 0 | 46821.8 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 45202.5 | 45202.5 | 92427.8 | 0 | PROCESSED | 56019.2486805556 | 55652 | 56019.2664583333 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | PERSEUS_CI_2 | 49.9439 | 41.5251 | 150.56387356 | -13.25282951 | 84.2575 | 55768.5049768518 | 55769.518275463 | 106006010 | 40145.3 | 40000 | 40153.3 | 40161.3 | 0 | 40145.3 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 35470.3 | 35470.3 | 87505.9 | 0 | PROCESSED | 55792.212650463 | 55652 | 55792.2315740741 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | PERSEUS_1_4_WIN | 49.9438 | 41.5162 | 150.5688507 | -13.26029585 | 67.7327 | 55796.234849537 | 55796.7167824074 | 106007010 | 20971.3 | 20000 | 20971.3 | 21003.2 | 0 | 20985.5 | 2 | 3 | 0 | 2 | 1 | 0 | 0 | 18760.7 | 18760.7 | 41633.9 | 2 | PROCESSED | 55809.1854398148 | 55652 | 55809.1967013889 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | PERSEUS_1_4_WIN | 49.954 | 41.5015 | 150.58372556 | -13.26834695 | 262.0009 | 55965.9169444444 | 55966.4167824074 | 106007020 | 20856.9 | 20000 | 20880.9 | 20872.9 | 0 | 20856.9 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 21425.5 | 21425.5 | 43173.9 | 1 | PROCESSED | 55991.4404976852 | 55652 | 55991.4500810185 | 2.7.16.31 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | PERSEUS_1_4_WIN_CI_2 | 49.9427 | 41.5184 | 150.56689856 | -13.25891455 | 67.7307 | 55795.7574305556 | 55796.234837963 | 106008010 | 23202.3 | 20000 | 23210.3 | 23202.3 | 0 | 23218.3 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 22067.8 | 22067.8 | 41244 | 0 | PROCESSED | 55806.3383333333 | 55652 | 55806.3485069445 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | PERSEUS_1_4_WIN_CI_2 | 49.95042 | 41.51169 | 150.57565427 | -13.261325 | -99 | NULL | NULL | 106008020 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 55652 | NULL | NULL | NULL | NULL | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | N | | PERSEUS_1_4_WIN_CI_2 | 49.95042 | 41.51169 | 150.57565427 | -13.261325 | -99 | NULL | NULL | 106008030 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 55652 | NULL | NULL | NULL | NULL | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | N | | RXJ1856.5-3754 | 284.1491 | -37.9147 | 358.59438145 | -17.21743909 | 269.0594 | 55856.467037037 | 55857.327962963 | 106009010 | 39312.3 | 40000 | 39312.3 | 39320.3 | 0 | 39312.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35512.7 | 35512.7 | 74370.1 | 1 | PROCESSED | 55873.9707175926 | 55652 | 55873.9976041667 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | N132D | 81.27 | -69.6453 | 280.30751952 | -32.78013136 | 312.914 | 55676.4828935185 | 55677.0820138889 | 106010010 | 26045.3 | 25000 | 26045.3 | 26045.3 | 0 | 26045.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23421 | 23421 | 51753.9 | 0 | PROCESSED | 55697.1299768518 | 55652 | 55697.1447685185 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | N132D | 81.2448 | -69.6458 | 280.30994764 | -32.78867022 | 111.8253 | 55841.4446759259 | 55841.8703935185 | 106010020 | 23903 | 25000 | 23903 | 23903 | 0 | 23903 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22252.9 | 22252.9 | 36763.9 | 0 | PROCESSED | 55858.3557175926 | 55652 | 55858.3789814815 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y | | PKS2155-304 | 329.71 | -30.2187 | 17.74059687 | -52.23913549 | 58.7962 | 55677.0907291667 | 55678.5925925926 | 106011010 | 60569.3 | 60000 | 60577.3 | 60583 | 0 | 60569.3 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 49583.6 | 49583.6 | 129709.8 | 1 | PROCESSED | 55697.2141898148 | 55652 | 55697.2337152778 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065002 | This observation is a coordinated observation with Chandra and XMM carried out regularly once per year. The purpose is to calibrate relative effective areas among the three observatories. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 6 | AO6-CAL | COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTON | XIS | Y | | CRAB | 83.6298 | 22.0234 | 184.54825576 | -5.78216614 | 87.1025 | 55805.2472916667 | 55806.2585532407 | 106012010 | 509.9 | 40000 | 509.9 | 509.9 | 0 | 509.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36558.9 | 36558.9 | 87353.9 | 1 | PROCESSED | 55847.5962268518 | 55652 | 55851.4353356482 | 2.7.16.30 | 2 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065003 | We propose to observe the Crab in order to calibrate the HXD response functions. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 6 | AO6-CAL | CALIBRATION OF HXD RESPONSE FUNCTIONS | XIS | Y | | CRAB | 83.6357 | 22.0122 | 184.56070723 | -5.78354183 | 269.6254 | 55985.4765740741 | 55986.5585532407 | 106013010 | 521.7 | 40000 | 521.7 | 521.7 | 0 | 521.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36421.7 | 36421.7 | 93465.8 | 1 | PROCESSED | 55995.2314351852 | 55652 | 55995.2489699074 | 2.7.16.31 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065004 | We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 6 | AO6-CAL | CALIBRATION OF THE HXD RESPONSE FUNCTIONS | XIS | Y | | CRAB | 83.6352 | 22.0094 | 184.56283497 | -5.78543222 | 269.6994 | 56000.0051967593 | 56001.1391435185 | 106014010 | 607 | 40000 | 607 | 607 | 0 | 607 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44787.9 | 44787.9 | 97955.8 | 1 | PROCESSED | 56019.3102430556 | 55652 | 56019.3369907407 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065004 | We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 6 | AO6-CAL | CALIBRATION OF THE HXD RESPONSE FUNCTIONS | XIS | Y | | CRAB | 83.6348 | 22.004 | 184.56721998 | -5.78863608 | 269.6984 | 56012.5465393518 | 56013.5182407407 | 106015010 | 533.6 | 40000 | 533.6 | 533.6 | 0 | 533.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 24545 | 24545 | 83940.9 | 1 | PROCESSED | 56023.2521875 | 55652 | 56023.2694212963 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 065004 | We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 6 | AO6-CAL | CALIBRATION OF THE HXD RESPONSE FUNCTIONS | XIS | Y | | LOCKMAN HOLE | 162.9375 | 57.26667 | 149.68932697 | 53.19392671 | -99 | NULL | NULL | 107001010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y | | E0102-72 | 16.0127 | -72.0346 | 301.55559389 | -45.0599301 | 14.0258 | 56039.926099537 | 56040.7294212963 | 107002010 | 30438.2 | 30000 | 30470.2 | 30438.2 | 0 | 30462.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28052.8 | 28052.8 | 69401.9 | 0 | PROCESSED | 56054.2591203704 | 56018 | 56054.2693634259 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y | | E0102-72 | 16.00833 | -72.03131 | 301.55717515 | -45.06330557 | -99 | NULL | NULL | 107002020 | -99 | 30000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | E0102-72 | 16.00833 | -72.03131 | 301.55717515 | -45.06330557 | -99 | NULL | NULL | 107002030 | -99 | 30000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | E0102-72 | 16.00833 | -72.03131 | 301.55717515 | -45.06330557 | -99 | NULL | NULL | 107002040 | -99 | 30000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | E0102-72_1_4_WIN | 16.00833 | -72.03131 | 301.55717515 | -45.06330557 | -99 | NULL | NULL | 107003010 | -99 | 30000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y | | E0102-72_1_4_WIN | 16.00833 | -72.03131 | 301.55717515 | -45.06330557 | -99 | NULL | NULL | 107003020 | -99 | 30000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | CYGNUS_LOOP_P8 | 313.99579 | 31.47519 | 75.29734567 | -8.8819535 | -99 | NULL | NULL | 107004010 | -99 | 10000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | CYGNUS_LOOP_P8 | 313.99579 | 31.47519 | 75.29734567 | -8.8819535 | -99 | NULL | NULL | 107004020 | -99 | 10000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | PERSEUS | 49.95042 | 41.51169 | 150.57565427 | -13.261325 | -99 | NULL | NULL | 107005010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | PERSEUS | 49.95042 | 41.51169 | 150.57565427 | -13.261325 | -99 | NULL | NULL | 107005020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | PERSEUS_1_4_WIN | 49.95042 | 41.51169 | 150.57565427 | -13.261325 | -99 | NULL | NULL | 107006010 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | PERSEUS_1_4_WIN | 49.95042 | 41.51169 | 150.57565427 | -13.261325 | -99 | NULL | NULL | 107006020 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | RXJ1856.5-3754 | 284.1441 | -37.9006 | 358.60662879 | -17.20863504 | 88.5024 | 56019.1209143518 | 56020.3237384259 | 107007010 | 42087.7 | 40000 | 42095.7 | 42087.7 | 0 | 42095.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37740.3 | 37740.3 | 103914 | 1 | PROCESSED | 56034.2854398148 | 56018 | 56034.3014699074 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y | | RXJ1856.5-3754 | 284.14629 | -37.9085 | 358.59958333 | -17.21311871 | -99 | NULL | NULL | 107007020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | N132D | 81.25917 | -69.64417 | 280.30698796 | -32.78403883 | -99 | NULL | NULL | 107008010 | -99 | 25000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | N132D | 81.25917 | -69.64417 | 280.30698796 | -32.78403883 | -99 | NULL | NULL | 107008020 | -99 | 25000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | PSK2155-304 | 329.71696 | -30.22558 | 17.73050588 | -52.24586776 | -99 | NULL | NULL | 107009010 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N | | PKS2155-304 | 329.71696 | -30.22558 | 17.73050588 | -52.24586776 | -99 | NULL | NULL | 107010010 | -99 | 60000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075002 | This observation is a coordinated observation with Chandra and XMM carried out regularly once per year. The purpose is to calibrate relative effective areas among the three observatories. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 7 | AO7 | COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTON | XIS | Y | | CRAB | 83.63321 | 22.0145 | 184.55751251 | -5.78426048 | -99 | NULL | NULL | 107011010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075003 | We propose to observe the Crab in order to calibrate the HXD response functions. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 7 | AO7 | CALIBRATION OF HXD RESPONSE FUNCTIONS | XIS | N | | CRAB | 83.63321 | 22.0145 | 184.55751251 | -5.78426048 | -99 | NULL | NULL | 107012010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 075004 | We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 7 | AO7 | CALIBRATION OF THE HXD RESPONSE FUNCTIONS | XIS | N | | AE AQUARII | 310.0457 | -0.9355 | 45.22275468 | -24.45710482 | 264.8759 | 53673.9022685185 | 53676.043275463 | 400001010 | 70528.9 | 100000 | 70528.9 | 70616.9 | 70568.9 | 70544.9 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 59453.8 | 59453.8 | 184956.9 | 2 | PROCESSED | 54328.3910763889 | 54247 | 54036.9851388889 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001004 | We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku. | GALACTIC POINT SOURCES | 4 | A | TERADA | YUKIKATSU | NULL | NULL | JAP | 0 | SWG | SEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKU | NULL | N | | AE AQUARII | 310.0612 | -0.931 | 45.23545862 | -24.46836188 | 250.6241 | 54033.2319907407 | 54034.3829282407 | 400001020 | 47974.3 | 50000 | 47974.3 | 48595.6 | 48131.6 | 48310.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45538.4 | 45538.4 | 99423.9 | 1 | PROCESSED | 54327.126712963 | 54526 | 54109.7083449074 | 2.0.6.13 | 8 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001004 | We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku. | GALACTIC POINT SOURCES | 4 | A | TERADA | YUKIKATSU | NULL | NULL | JAP | 0 | SWG | SEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKU | HXD | N | | GX 349+2 | 256.427 | -36.366 | 349.14511841 | 2.78820606 | 85.6584 | 53808.5453240741 | 53809.2216782407 | 400003010 | 25230.8 | 50000 | 25230.8 | 25233.2 | 25230.8 | 25230.8 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 20050.7 | 20050.7 | 58434 | 2 | PROCESSED | 54327.3834375 | 54247 | 54041.9132060185 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001026 | We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure. | GALACTIC POINT SOURCES | 4 | A | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 0 | SWG | SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES) | HXD | N | | GX 349+2 | 256.4194 | -36.3657 | 349.14166441 | 2.79326977 | 78.9359 | 53813.9267708333 | 53814.6043402778 | 400003020 | 28117.7 | 50000 | 28117.7 | 28131.7 | 28120.4 | 28120.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25657.3 | 25657.3 | 58538 | 0 | PROCESSED | 54327.4043634259 | 54247 | 54042.1657407407 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001026 | We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure. | GALACTIC POINT SOURCES | 4 | A | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 0 | SWG | SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES) | HXD | N | | SS CYG | 325.6789 | 43.5736 | 90.55119171 | -7.12024619 | 276.5788 | 53676.0503703704 | 53676.9856944444 | 400006010 | 39451.2 | 40000 | 39451.2 | 39451.2 | 39451.2 | 39451.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32047.2 | 32047.2 | 80810 | 1 | PROCESSED | 54325.1179282407 | 54247 | 54036.9898148148 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001043 | Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst. | GALACTIC POINT SOURCES | 4 | A | ISHIDA | MANABU | NULL | NULL | JAP | 0 | SWG | SS CYG OBSERVATION IN QUIESCENCE | NULL | N | | SS CYG | 325.6842 | 43.5739 | 90.55430501 | -7.12254626 | 256.8767 | 53692.6066203704 | 53693.8646759259 | 400007010 | 56043 | 60000 | 56059 | 56179 | 56043 | 56059 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54357.2 | 54357.2 | 108665.8 | 2 | PROCESSED | 54328.1064351852 | 54247 | 54037.9128472222 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001044 | Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst. | GALACTIC POINT SOURCES | 4 | A | ISHIDA | MANABU | NULL | NULL | JAP | 0 | SWG-TOO | SS CYG OBSERVATION IN OUTBURST | XIS | N | | X1630-472 | 248.4828 | -47.3401 | 336.93914719 | 0.29801709 | 78.3341 | 53774.6318981482 | 53775.1390972222 | 400010010 | 22190.2 | 200000 | 22190.2 | 22190.2 | 22190.2 | 22190.2 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 22247 | 22247 | 43816 | 0 | PROCESSED | 54327.217337963 | 54247 | 54040.9540856482 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N | | X1630-472 | 248.4706 | -47.343 | 336.93140696 | 0.30212129 | 69.0657 | 53781.9791087963 | 53782.5474305556 | 400010020 | 21429 | 200000 | 21429 | 21485 | 21429 | 21429 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17022.3 | 17022.3 | 49101.9 | 0 | PROCESSED | 54322.9506828704 | 54247 | 54041.4892013889 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N | | X1630-472 | 248.4772 | -47.3405 | 336.93627828 | 0.30053306 | 75.5959 | 53794.9708333333 | 53795.6968055556 | 400010030 | 21521.6 | 200000 | 21521.6 | 21521.6 | 21521.6 | 21521.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19032.8 | 19032.8 | 62718 | 0 | PROCESSED | 54323.0049884259 | 54247 | 54041.5956018518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N | | X1630-472 | 248.5414 | -47.3441 | 336.96314137 | 0.26612574 | 120.5775 | 53802.0758796296 | 53802.7300231482 | 400010040 | 21248.1 | 200000 | 21248.1 | 21249.9 | 21249.9 | 21249.9 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 20477.8 | 20477.8 | 56512 | 0 | PROCESSED | 54320.7897222222 | 54247 | 54041.7698726852 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N | | X1630-472 | 248.5239 | -47.3401 | 336.95804041 | 0.27755382 | 107.6616 | 53809.226412037 | 53809.743912037 | 400010050 | 23167.1 | 200000 | 23175.1 | 23176.9 | 23176.8 | 23167.1 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 18860.5 | 18860.5 | 44706 | 0 | PROCESSED | 54324.0568981482 | 54247 | 54041.9302662037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N | | X1630-472 | 248.5405 | -47.3458 | 336.96147829 | 0.2654214 | 120.3 | 53817.4260300926 | 53817.9313425926 | 400010060 | 21654.1 | 200000 | 21662.1 | 21654.1 | 21654.1 | 21654.1 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 22761.9 | 22761.9 | 43655.9 | 1 | PROCESSED | 54324.1960532407 | 54247 | 54042.1043287037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N | | 4U1626-67 | 248.0601 | -67.4675 | 321.78071552 | -13.09322804 | 103.0359 | 53803.0543518518 | 53805.818275463 | 400015010 | 102639.2 | 100000 | 102654 | 102639.2 | 102647.2 | 102654 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93393.2 | 93393.2 | 238781.9 | 3 | PROCESSED | 54330.2336574074 | 54247 | 54042.4663657407 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001081 | The X-ray spectrum of the 7 second LMXRB pulsar 4U1626-67 is dominated by low energy line emission with little evedence of iron K line in the pulse phase resolved spectra. It showd also cyclotron line at 37 keV that departs from the correlation of energy cutoff cyclotron energy observed in many other X-ray pulsars. This Suzaku observation allow to characterize the overall continuum, the low energy, the iron K alpha and cyclotron lines as function of the pulse phase, | GALACTIC POINT SOURCES | 4 | A | ANGELINI | LORELLA | NULL | NULL | JAP | 0 | SWG | 4U1626-67: PHASE RESOLVED SPECTRA AND CYCLOTRON LINE | XIS | N | | CH CYG | 291.1621 | 50.2424 | 81.86550652 | 15.56609243 | 185.7481 | 53739.5736458333 | 53740.2919560185 | 400016020 | 33305.8 | 25000 | 33307.5 | 33337.8 | 33315.5 | 33305.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28461.5 | 28461.5 | 62056 | 1 | PROCESSED | 54323.9210185185 | 54247 | 54039.6712268518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001082 | CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS. | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | JAP | 0 | SWG | SUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNI | XIS | N | | CH CYG | 291.1168 | 50.2494 | 81.85997028 | 15.59541424 | 38.1861 | 53883.3112962963 | 53884.1502199074 | 400016030 | 35144 | 35000 | 35152 | 35160 | 35160 | 35144 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 37459 | 37459 | 72447.9 | 1 | PROCESSED | 54323.2026157407 | 54258 | 54109.7043981482 | 2.0.6.13 | 8 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001082 | CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS. | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | JAP | 0 | SWG | SUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNI | XIS | N | | JUPITER | 226.5694 | -16.1887 | 343.96536778 | 35.7224308 | 118.4901 | 53790.7643402778 | 53791.7940277778 | 401001010 | 37759.4 | 36000 | 37767.4 | 37759.4 | 37767.4 | 37767.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32836.1 | 32836.1 | 88936.1 | 1 | PROCESSED | 54323.0172569444 | 54401 | 53905.533900463 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | ELSNER | RONALD | NULL | NULL | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N | | JUPITER | 226.5948 | -16.1928 | 343.98613419 | 35.70433361 | 118.4906 | 53791.7941319445 | 53792.7940277778 | 401001020 | 37704 | 36000 | 37704 | 37704 | 37704 | 37704 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 32778.1 | 32778.1 | 86360 | 1 | PROCESSED | 54326.9105208333 | 54401 | 53905.5035416667 | 2.0.6.13 | 5 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | ELSNER | RONALD | NULL | NULL | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N | | JUPITER | 226.6157 | -16.1957 | 344.00356707 | 35.68981432 | 118.4907 | 53792.7940856482 | 53793.8599421296 | 401001030 | 40791.2 | 36000 | 40799.2 | 40791.2 | 40799.2 | 40799.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35536.3 | 35536.3 | 92073.9 | 0 | PROCESSED | 54322.9911574074 | 54401 | 53905.5868055556 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | ELSNER | RONALD | NULL | NULL | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N | | JUPITER | 226.6349 | -16.1983 | 344.01962259 | 35.67652355 | 118.4908 | 53793.86 | 53794.9585532407 | 401001040 | 42255.8 | 36000 | 42263.8 | 42263.8 | 42263.8 | 42255.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35706.7 | 35706.7 | 94905.9 | 2 | PROCESSED | 54324.1065625 | 54401 | 53906.5712615741 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | ELSNER | RONALD | NULL | NULL | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N | | XB1323-619 | 201.6454 | -62.1418 | 307.02498182 | 0.45033402 | 99.5731 | 54109.4794907407 | 54110.9168402778 | 401002010 | 55936.8 | 50000 | 55936.8 | 55936.8 | 0 | 55936.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81817.3 | 81817.3 | 124176.9 | 1 | PROCESSED | 54324.7906365741 | 54735 | 54133.0271759259 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010002 | XB 1323-619 is a non-transient dipping LMXB and one of the few LMXB with spectrum extending to high energies. Our XMM-Newton observation revealed many lines including Fe XXV and XXVI absorption. Uniquely, the rate of bursting has increased systematically over 18 years by 15 times to every 20 min in 2006/07 making it the best source for study of absorption in bursts. Suzaku allows measurement of ADC temperature via the high energy cut-off and can give the first detection of cooling by soft photons from the neutron star from the change of cut-off energy during bursts. Curve-of-growth analysis gives the absorber temperature and tests our suggestion that absorption lines are formed in the ADC. Detailed comparison with burst theory is possible because of the regular bursting. | GALACTIC POINT SOURCES | 4 | C | DOTANI | TADAYASU | NULL | NULL | JAP | 1 | AO1 | BORADBAND INVESTIGATIONS OF THE DIPPING, BURSTGING LOW MASS X-RAY BINARY XB1323-619 | XIS | Y | | SS 433 | 287.9531 | 4.9906 | 39.69950989 | -2.2379409 | 78.6445 | 53829.6109606482 | 53830.5327662037 | 401003010 | 38676.7 | 40000 | 38676.7 | 38676.7 | 38676.7 | 38676.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28241.1 | 28241.1 | 79634 | 1 | PROCESSED | 54323.8806365741 | 54394 | 53906.1478125 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010031 | SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber. | GALACTIC POINT SOURCES | 4 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 1 | AO1 | SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE | XIS | N | | SS 433 | 287.9527 | 4.99 | 39.69879316 | -2.23786427 | 78.6446 | 53833.4611458333 | 53834.4579166667 | 401004010 | 40197.6 | 40000 | 40221.6 | 40197.6 | 40229.6 | 40213.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30474.9 | 30474.9 | 86110 | 2 | PROCESSED | 54327.1886458333 | 54400 | 53906.5501736111 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010031 | SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber. | GALACTIC POINT SOURCES | 4 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 1 | AO1 | SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE | XIS | N | | G11.2-0.3 | 272.8676 | 19.433 | 46.34586116 | 17.29738119 | 77.6432 | 53834.4626041667 | 53835.6634143518 | 401010010 | 43984.6 | 50000 | 43992.6 | 43984.6 | 43992.6 | 43992.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37387.9 | 37387.9 | 83679.9 | 1 | PROCESSED | 54327.0387152778 | 54397 | 53905.4671875 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010049 | The PSR 1811-1925 in a historical supernova remnant G11.2-0.3 has its characteristic age as 10 times longer than the age of the remnant. The pulsar has its period 64 ms and the hard spectrum. We suggest that the pulsar shows the signs of having the small magnetic field. The SUZAKU observation must give the answer for this hypothesis. First, HXD allows us to observe the spectrum in the high energy range, and if the cut-off would be observed, the magnetic fields of pulsar will be estimate. Seconds, XIS has the great energy resolution to determine the abundance of the shell. This would let us estimate the mass of the progenitor. Third, HXD provides the new spin down rate observation. Then, we can make sure the constancy of the spin down rate. The pulsar age mystery must be solved by SUZAKU. | GALACTIC POINT SOURCES | 4 | C | HAYATO | ASAMI | NULL | NULL | JAP | 1 | AO1 | CLEARING UP THE MECHANISM OF THE PSR J1811-1925 IN SNR G11.2-0.3 | XIS | N | | CYGNUS X-3 | 308.2593 | 40.981 | 79.93230299 | 0.62160244 | 252.424 | 54052.0902893518 | 54054.3676388889 | 401011010 | 99744.5 | 100000 | 99746.2 | 99746.2 | 0 | 99744.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95389.3 | 95389.3 | 196745 | 1 | PROCESSED | 54331.2167824074 | 54456 | 54088.9545023148 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010058 | We propose an observation of the unusual X-ray binary Cygnus X-3. Cyg X-3 is a final stage of the massive binary stars consisting of a WR(N) star and a compact star. However the nature of the compact star is not well understood. We have fore scientific objective. (A)Determine the Doppler modulation of iron K lines and discuss the binary nature. (2) Determine the iron abundance in the WR wind. (3) Search for the high energy cut off about 100keV of the power law component. (4) Search for the X-ray emission from radio knots. For these four sciences, we propose 100ksec observation of Cyg X-3. | GALACTIC POINT SOURCES | 4 | C | KITAMOTO | SHUNJI | NULL | NULL | JAP | 1 | AO1 | WIDE BAND OBSERVATION OF CYGNUS X-3 WITH SUZAKU | SPE | Y | | LMC X-2 | 80.025 | -71.9941 | 283.14092563 | -32.7117801 | 313.3022 | 53849.381712963 | 53850.7731365741 | 401012010 | 56152 | 60000 | 56165.7 | 56165.7 | 56152 | 56160 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 73408 | 73408 | 120193.8 | 1 | PROCESSED | 54329.0935185185 | 54394 | 53907.6288078704 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010090 | We propose the Suzaku observation of LMC X-2, to detect the slim disk structure in its flaring branch. The luminosity of LMC X-2 is always as luminous as the Eddington limit, and the absorption is so low that the energy spectrum can be observed over the 0.2-30 keV energy range. Then, LMC X-2 is the best target to study whether the disk structure becomes the slim disk or not. | GALACTIC POINT SOURCES | 4 | B | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 1 | AO1 | DETECTION OF SLIM-DISK STRUCTURE FROM LOW-MASS X-RAY BINARY LMC X-2 | HXD | N | | SGR1806-20 | 272.1595 | -20.349 | 10.0481975 | -0.20823053 | 88.7483 | 54189.6305555556 | 54190.0627199074 | 401021010 | 19288.9 | 20000 | 19288.9 | 19595 | 0 | 19356.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16507.1 | 16507.1 | 37327.9 | 1 | PROCESSED | 54323.026099537 | 54561 | 54209.5169212963 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010124 | We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs. | GALACTIC POINT SOURCES | 4 | A | NAKAGAWA | YUJIN | NULL | NULL | JAP | 1 | AO1-TOO | PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR" | HXD | N | | SGR1900+14 | 286.803 | 9.3875 | 43.07594962 | 0.80149907 | 86.5533 | 53826.3631597222 | 53826.9113310185 | 401022010 | 17056.2 | 20000 | 17704.6 | 21707.4 | 21655.5 | 17056.2 | 1 | 2 | 1 | 1 | 1 | 0 | 0 | 14360.4 | 14360.4 | 47336 | 1 | PROCESSED | 54323.156400463 | 54394 | 53906.0977893518 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010124 | We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs. | GALACTIC POINT SOURCES | 4 | A | NAKAGAWA | YUJIN | NULL | NULL | JAP | 1 | AO1-TOO | PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR" | HXD | N | | HESS J1837-069 | 279.4395 | -6.8651 | 25.2664546 | -0.10276403 | 102.6144 | 54164.5341898148 | 54165.4286342593 | 401026010 | 42191.1 | 40000 | 42191.1 | 42199.1 | 0 | 42207.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37702.1 | 37702.1 | 77259.9 | 1 | PROCESSED | 54322.861087963 | 54750 | 54171.2613425926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010131 | The HESS (High Energy Stereoscopic System) collaboration has recently reported the TeV survey of the inner-part of the Galaxy, which revealed the existence of a new population of gamma-ray objects. Most of which are unknown, but at least two of them, HESS J1813-178 and HESS J1837-069 are point-like, and the ASCA Galactic survey and the INTEGRAL survey detected the counterparts in 0.5-10 keV and 20-100 keV, respectively. Making full use of Suzaku's wide-band spectral capability, we will study spectral characteristics of HESS J1813-178 and HESS J1837-069 in 0.5 keV to ~200 keV, and investigate for their origins. We will also carry out pulse-search to evaluate the pulsar-wind hypothesis. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 1 | AO1 | INVESTIGATION OF TWO HESS SOURCES DETECTED WITH INTEGRAL | HXD | Y | | 1E1207.4-5209 | 182.5062 | -52.436 | 296.5458403 | 9.92149786 | 302.4939 | 53946.5682060185 | 53948.2603587963 | 401030010 | 96351.9 | 120000 | 96351.9 | 102278.4 | 96367.9 | 96351.9 | 3 | 2 | 3 | 3 | 1 | 0 | 0 | 94049.8 | 94049.8 | 135379.9 | 1 | PROCESSED | 54328.1902430556 | 54750 | 54132.8187268518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010152 | 1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object. | GALACTIC POINT SOURCES | 4 | B | YOSHIDA | ATSUMASA | NULL | NULL | JAP | 1 | AO1 | A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209 | XIS | N | | 1E1207.4-5209 | 182.4916 | -52.442 | 296.53791481 | 9.91413144 | 148.6893 | 54146.2087384259 | 54147.6390509259 | 401030020 | 49826.6 | 50000 | 50073.4 | 49826.6 | 0 | 50089.4 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 44446.8 | 44446.8 | 123576 | 2 | PROCESSED | 54329.2028009259 | 54750 | 54153.9886458333 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010152 | 1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object. | GALACTIC POINT SOURCES | 4 | B | YOSHIDA | ATSUMASA | NULL | NULL | JAP | 1 | AO1 | A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209 | XIS | Y | | AB DOR | 82.2835 | -65.427 | 275.26967334 | -33.00819219 | 154.6774 | 54060.0265277778 | 54061.4586111111 | 401031010 | 53451.7 | 80000 | 53451.7 | 53459.7 | 0 | 53461.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48033.4 | 48033.4 | 123708 | 1 | PROCESSED | 54324.929212963 | 54502 | 54133.0222916667 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011021 | We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku. | GALACTIC POINT SOURCES | 4 | B | AUDARD | MARC | NULL | NULL | USA | 1 | AO1 | NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES | HXD | N | | AB DOR | 82.2881 | -65.4658 | 275.31538375 | -33.00189818 | 204.2849 | 54108.0647569444 | 54109.4724421296 | 401031020 | 49096.5 | 45000 | 49096.5 | 49096.5 | 0 | 49096.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44961.1 | 44961.1 | 121619.9 | 2 | PROCESSED | 54324.0499074074 | 54502 | 54133.0127083333 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011021 | We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku. | GALACTIC POINT SOURCES | 4 | B | AUDARD | MARC | NULL | NULL | USA | 1 | AO1 | NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES | HXD | N | | HR 9024 | 357.4125 | 36.4308 | 109.27773456 | -24.79729068 | 49.8624 | 53939.0616782407 | 53940.6016087963 | 401032010 | 58775.7 | 60000 | 58799.7 | 58775.7 | 58783.7 | 58791.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 56011.6 | 56011.6 | 133039.8 | 1 | PROCESSED | 54324.8656597222 | 54401 | 53950.2624074074 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011022 | Suzaku-XIS is the best available instrument to study the Fe fluorescence emission from late-type evolved stars. Fe fluorescence is produced by illumination of the photosphere by ionizing coronal X-rays and its intensity depends on the height of the X-ray source. We propose to observe Fe fluorescence in the single G-type giant HR 9024 and in the active RS CVn system II Peg to obtain a direct geometrical constraint on the scale height of their coronal structures. These two stars have the brightest Fe fluorescence features of all the late-type stars observed by the Chandra-HETGS and their different stellar parameters (stellar radius, gravity, multiplicity,..) and evolutionary stage will allow us to probe the typical coronal scale for significantly different conditions. | GALACTIC POINT SOURCES | 4 | B | TESTA | PAOLA | NULL | NULL | USA | 1 | AO1 | GEOMETRY DIAGNOSTICS FROM FE FLUORESCENT EMISSION IN LATE-TYPE EVOLVED STARS | XIS | N | | SIGMA^2 CRB | 243.6552 | 33.7881 | 54.56402364 | 46.14689859 | 281.1207 | 53969.4764467593 | 53972.1925231482 | 401034010 | 109160.4 | 110000 | 109190.4 | 109160.4 | 109168.4 | 109176.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 98837.6 | 98837.6 | 234653.9 | 3 | PROCESSED | 54330.9158217593 | 54526 | 54021.2578587963 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011025 | Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission from RS CVn binaries. We propose to obtain 110 ksec (3 day elapsed time) observations of the RS CVn systems Sigma^2 CrB (F6V + G0V) and Sigma Gem (K0III +?). Our goals are i) to better characterize their hard (> 10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, and iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability in the 10-25 keV region provided by HXD. | GALACTIC POINT SOURCES | 4 | B | BROWN | ALEXANDER | NULL | NULL | USA | 1 | AO1 | SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL EMISSION ON THE RS CVN BINARIES SIGMA^2 CRB AND SIGMA GEM | HXD | N | | BETA LYR | 282.5094 | 33.3738 | 63.19462876 | 14.79594569 | 59.4704 | 53862.545474537 | 53862.9952083333 | 401036010 | 20251.5 | 20000 | 20267.5 | 20251.5 | 20267.5 | 20267.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9894.7 | 9894.7 | 38851.9 | 1 | PROCESSED | 54323.0649884259 | 54401 | 53913.8191550926 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011031 | The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 1 | AO1 | AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE | XIS | N | | BETA LYR | 282.5098 | 33.3716 | 63.19266924 | 14.79477853 | 53.4974 | 53867.1260185185 | 53867.6252199074 | 401036020 | 21496.2 | 20000 | 21496.2 | 21496.2 | 21496.2 | 21496.2 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19164.2 | 19164.2 | 43119.9 | 2 | PROCESSED | 54323.1969212963 | 54401 | 53914.2784143518 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011031 | The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 1 | AO1 | AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE | XIS | N | | BETA LYR | 282.5093 | 33.3719 | 63.19278609 | 14.79528012 | 53.4973 | 53871.4311226852 | 53871.8571875 | 401036030 | 18195.4 | 20000 | 18195.4 | 18195.4 | 18195.4 | 18195.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19842.1 | 19842.1 | 36807.9 | 0 | PROCESSED | 54320.7847337963 | 54401 | 53920.4164351852 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011031 | The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 1 | AO1 | AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE | XIS | N | | 1RX J154814.5-452845 | 237.0511 | -45.4226 | 332.46961393 | 7.07040697 | 85.7358 | 54132.6368518518 | 54135.3543865741 | 401037010 | 99454.1 | 100000 | 99454.1 | 99462.1 | 0 | 99470.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86855.2 | 86855.2 | 234783.8 | 3 | PROCESSED | 54329.9169212963 | 54702 | 54139.4767939815 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011102 | Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber. | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | USA | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION | HXD | Y | | 1RXS J213344.1+51072 | 323.4354 | 51.1973 | 94.50909334 | -0.42447705 | 94.0452 | 53854.2853009259 | 53856.2501736111 | 401038010 | 81924.1 | 80000 | 81924.1 | 81924.1 | 81924.1 | 81924.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 62888.1 | 62888.1 | 169726.1 | 3 | PROCESSED | 54327.5816550926 | 54391 | 53908.1887962963 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011102 | Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber. | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | USA | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION | HXD | N | | V893 SCO | 243.8144 | -28.6275 | 348.06577336 | 15.88028883 | 274.6746 | 53973.4024189815 | 53974.056412037 | 401041010 | 18497.8 | 20000 | 18497.8 | 18497.8 | 18497.8 | 18497.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16140.3 | 16140.3 | 56482 | 0 | PROCESSED | 54322.6723726852 | 54526 | 54053.4763888889 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011103 | The RXTE All-Sky Slew Survey (XSS) catalog, containing 294 objects detected in the 3-20 keV sky, is of great potential use for a variety of purposes. Included in this catalog are two sources identified with lesser known dwarf novae, V893 Sco and SS Aur. Although these are known to be soft X-ray sources from the ROSAT All-sky Survey, there has never been a pointed observation with an imaging X-ray telescope of either object. Here I propose short Suzaku observations of V893 Sco and SS Aur to check the reliability of XSS fluxes, hence that of the luminosity functions derived from the XSS catalog. In addition, such observations serve as a pilot study to determine if these individual dwarf novae may merit further in-depth X-ray studies. | GALACTIC POINT SOURCES | 4 | B | MUKAI | KOJI | NULL | NULL | USA | 1 | AO1 | CONFIRMING THE IDENTIFICATION OF RXTE ALL-SKY SLEW SURVEY SOURCES WITH DWARF NOVAE | XIS | N | | T CRB | 239.8773 | 25.9106 | 42.36027985 | 48.16117824 | 268.9321 | 53984.9474652778 | 53986.0911921296 | 401043010 | 46303.3 | 50000 | 46311.3 | 46311.3 | 46319.3 | 46303.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45431.4 | 45431.4 | 98815.9 | 1 | PROCESSED | 54324.1068981482 | 54526 | 54053.4340856482 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011106 | Hard X-ray emission up to ~100 keV has recently been detected with INTEGRAL and Swift from 3 exceptional symbiotic stars. These 3 objects are members of a subclass of symbiotics characterized by rapid optical flickering, and in some cases jets, recurrent nova eruptions, and high-mass white dwarfs possibly headed toward supernova Type Ia explosion. The origin of the hard X-ray emission from these accreting white dwarfs is a mystery. Broad-band X-ray observations, which only Suzaku can provide, are needed to bridge the gap between existing soft and hard X-ray spectra. We propose to perform such Suzaku observations of RT Cru, T CrB, and RS Oph to distinguish among thermal emission from a magnetic accretion column, non-thermal emission from a jet, or some unforeseen emission mechanism. | GALACTIC POINT SOURCES | 4 | A | SOKOLOSKI | JENNIFER | NULL | NULL | USA | 1 | AO1 | THE NATURE OF HARD X-RAY SYMBIOTIC BINARIES | XIS | N | | 4U 1705-44 | 257.2295 | -44.1004 | 343.32321952 | -2.34240238 | 264.0794 | 53976.2429166667 | 53976.7731712963 | 401046010 | 18315.5 | 20000 | 18315.5 | 18315.5 | 18315.5 | 18315.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 15371.5 | 15371.5 | 45809.9 | 0 | PROCESSED | 54322.587349537 | 54526 | 54021.306087963 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | YOUNG | ANDREW | NULL | NULL | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N | | 4U 1705-44 | 257.2281 | -44.1019 | 343.32141433 | -2.34248879 | 264.0666 | 53996.5173611111 | 53996.8619675926 | 401046020 | 17134 | 20000 | 17342 | 17134 | 17334 | 17334 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 15447.7 | 15447.7 | 29767.9 | 0 | PROCESSED | 54323.9647569444 | 54526 | 54020.9055555556 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | YOUNG | ANDREW | NULL | NULL | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N | | 4U 1705-44 | 257.2313 | -44.1028 | 343.32206131 | -2.34487049 | 297.0793 | 54014.4242708333 | 54015.0891087963 | 401046030 | 20065 | 20000 | 20065 | 20065 | 20065 | 20065 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17919.6 | 17919.6 | 57423.9 | 2 | PROCESSED | 54322.900462963 | 54526 | 54021.6765162037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | YOUNG | ANDREW | NULL | NULL | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N | | 4U 1820-30 | 275.9207 | -30.3623 | 2.78792233 | -7.91550172 | 265.9754 | 53992.9234606482 | 53993.6605902778 | 401047010 | 25700.8 | 37000 | 25700.8 | 25810.9 | 25723.9 | 25714.8 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 31878.2 | 31878.2 | 63633.9 | 1 | PROCESSED | 54329.4727662037 | 54526 | 54021.2227083333 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011113 | The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. | GALACTIC POINT SOURCES | 4 | B | MILLER | JON | NULL | NULL | USA | 1 | AO1 | A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES | XIS | N | | SERPENS X-1 | 279.9934 | 5.0285 | 36.11311789 | 4.83561165 | 256.1423 | 54032.2853819444 | 54033.2259143518 | 401048010 | 37157.8 | 37000 | 37157.8 | 37269.8 | 37205.8 | 37165.8 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 31069.5 | 31069.5 | 81239.9 | 2 | PROCESSED | 54330.1792939815 | 54526 | 54056.4719328704 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011113 | The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. | GALACTIC POINT SOURCES | 4 | B | MILLER | JON | NULL | NULL | USA | 1 | AO1 | A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES | XIS | N | | CYGNUS X-2 | 326.1653 | 38.3323 | 87.3318132 | -11.3049847 | 76.3142 | 53871.8636805556 | 53872.7293171296 | 401049010 | 39390.3 | 37000 | 39390.3 | 39406.3 | 39390.3 | 39390.3 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 36880.4 | 36880.4 | 74786 | 1 | PROCESSED | 54330.792962963 | 54401 | 53927.6429166667 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011113 | The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. | GALACTIC POINT SOURCES | 4 | B | MILLER | JON | NULL | NULL | USA | 1 | AO1 | A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES | XIS | N | | 4U 1636-536 | 250.2262 | -53.7541 | 332.91086545 | -4.81751491 | 91.2457 | 54140.3877546296 | 54140.99125 | 401050010 | 24232 | 19000 | 24232 | 24232 | 0 | 24232 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 21689.5 | 21689.5 | 52136 | 0 | PROCESSED | 54322.7352083333 | 54525 | 54151.5052893518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | HOMAN | JEROEN | NULL | NULL | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | | 4U 1636-536 | 250.2273 | -53.7542 | 332.91122007 | -4.81806999 | 91.2447 | 54153.2955787037 | 54154.3544560185 | 401050020 | 40096 | 38000 | 40096 | 40104 | 0 | 40096 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 35550 | 35550 | 91477.9 | 0 | PROCESSED | 54328.4423032407 | 54525 | 54158.392037037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | HOMAN | JEROEN | NULL | NULL | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | | 4U 1636-536 | 250.2272 | -53.754 | 332.91133194 | -4.81789372 | 91.2454 | 54160.0424421296 | 54160.8931597222 | 401050030 | 38719.3 | 38000 | 38727.4 | 38719.3 | 0 | 38719.4 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 48145.9 | 48145.9 | 73498 | 1 | PROCESSED | 54327.3161921296 | 54695 | 54167.6400462963 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | HOMAN | JEROEN | NULL | NULL | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | | 4U 1636-536 | 250.2277 | -53.7538 | 332.91167841 | -4.81798429 | 93.2445 | 54186.4802777778 | 54187.3043287037 | 401050040 | 32130.4 | 38000 | 32130.4 | 32138.4 | 0 | 32130.4 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 27784.2 | 27784.2 | 71177.9 | 1 | PROCESSED | 54324.2956597222 | 54695 | 54209.541412037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | HOMAN | JEROEN | NULL | NULL | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | | 4U 1636-536 | 250.2259 | -53.7533 | 332.911352 | -4.8168543 | 100.7755 | 54188.4720717593 | 54188.7856944445 | 401050050 | 12241.8 | 38000 | 12249.8 | 12241.8 | 0 | 12249.8 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 11804 | 11804 | 27088 | 0 | PROCESSED | 54320.8789236111 | 54695 | 54200.4687731482 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | HOMAN | JEROEN | NULL | NULL | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | | 4U 1822-37 | 276.4461 | -37.1042 | 356.85149319 | -11.29112534 | 258.4537 | 54010.4563888889 | 54011.5189699074 | 401051010 | 37743.4 | 40000 | 37768.2 | 37768.2 | 37743.4 | 37743.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33178.5 | 33178.5 | 91805.9 | 0 | PROCESSED | 54324.6250347222 | 54695 | 54024.6539814815 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011121 | We propose a 40 ks observation of the accretion disk corona source 4U 1822-37. Despite repeated observations over the years and even excellent high-resolution data from the Chandra Observatory, the nature and origin of the corona and even the source of the Fe K fluorescence emission remains controversial. The spectral resolution of the XIS and the broad-band coverage provided by the combined XIS and HXD instruments make Suzaku uniquely suited to a definitive measurement. Determining the physical conditions in this source is particularly interesting. Because of its geometry 4U 1822-37 is a link between x-ray binaries and AGN, and an therefore serve as a laboratory for studying accretion processes throughout the universe. | GALACTIC POINT SOURCES | 4 | B | COTTAM | JEAN | NULL | NULL | USA | 1 | AO1 | ACCRETION PHYSICS IN THE ADC SOURCE 4U 1822-37 | XIS | Y | | IGRJ16465-4507 | 251.6303 | -45.1738 | 340.00343338 | 0.10772124 | 284.9562 | 53987.3839814815 | 53987.9203009259 | 401052010 | 22527.9 | 20000 | 22535.9 | 22527.9 | 22535.9 | 22535.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24645.4 | 24645.4 | 46332 | 0 | PROCESSED | 54320.9010648148 | 54526 | 54021.113287037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N | | SWIFTJ2000.6+3210 | 300.0869 | 32.2033 | 68.99570836 | 1.1443147 | 87.4233 | 53837.6619212963 | 53837.9139351852 | 401053010 | 12438.4 | 20000 | 12444 | 12451.2 | 12451.2 | 12438.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9876.7 | 9876.7 | 21767.9 | 0 | PROCESSED | 54320.5594444445 | 54775 | 53927.3549189815 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N | | SWIFTJ2000.6+3210 | 300.1137 | 32.1218 | 68.93835501 | 1.08211502 | 255.6072 | 54039.0205671296 | 54039.3029976852 | 401053020 | 12748.4 | 10000 | 12756.4 | 12748.4 | 12756.4 | 12756.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 11727 | 11727 | 24393.9 | 0 | PROCESSED | 54320.6820717593 | 54775 | 54056.1959953704 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | Y | | IGRJ16493-4348 | 252.3173 | -43.8652 | 341.31911758 | 0.57823277 | 287.444 | 54013.8822916667 | 54014.4204166667 | 401054010 | 21199.8 | 20000 | 21215.8 | 21215.8 | 21199.8 | 21207.8 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 20219.7 | 20219.7 | 46463.9 | 1 | PROCESSED | 54322.6086574074 | 54695 | 54025.4796412037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | Y | | SWIFTJ1010.1-5747 | 152.7309 | -57.8539 | 282.8705066 | -1.37559689 | 290.7012 | 53891.2175 | 53891.5544560185 | 401055010 | 19171.7 | 20000 | 19171.7 | 19171.7 | 19171.7 | 19171.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17877.8 | 17877.8 | 29087.9 | 0 | PROCESSED | 54320.6983333333 | 54401 | 53926.1075347222 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N | | IGRJ16195-4945 | 244.8541 | -49.816 | 333.49117084 | 0.29973526 | 284.0301 | 53998.8508333333 | 53999.7231481482 | 401056010 | 39148.6 | 40000 | 39148.6 | 39148.6 | 39148.6 | 39148.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42265.2 | 42265.2 | 75357.9 | 1 | PROCESSED | 54322.8721875 | 54526 | 54020.9227199074 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N | | 4U1907+09 | 287.4013 | 9.8378 | 43.74739314 | 0.48531727 | 60.2599 | 53857.2580324074 | 53858.7322222222 | 401057010 | 58440.3 | 60000 | 58440.3 | 58456.3 | 58448.3 | 58456.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38821.5 | 38821.5 | 127353.9 | 1 | PROCESSED | 54326.7703587963 | 54401 | 53913.4367476852 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011133 | We propose 60ksec of Suzaku observations of the high mass X-ray binary 4U1907+09, to study the little known spectrum of the source below 2keV and to measure its behavior during its frequent dips, where matter ceases to accrete onto the magnetic poles of the neutron star. Making use of Suzaku's unique broad band capabilities, we will also perform pulse phase spectroscopy of the cyclotron line and study the parameters of the fundamental and first harmonic cyclotron lines, as 4U1907+09 is one of the few accreting neutron stars where two cyclotron lines lie within the energy range of the XIS and HXD-PIN detectors. The scientific aims of this proposal address questions within NASA's Goals and Research Focus Area ``Structure and Evolution of the Universe''. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 1 | AO1 | THE BROAD BAND SPECTRUM OF 4U1907+09 | XIS | N | | 4U1700-37 | 255.9894 | -37.8441 | 347.75582102 | 2.17172645 | 269.6945 | 53991.447662037 | 53992.918912037 | 401058010 | 81442.5 | 80000 | 81456.9 | 81470.4 | 81442.5 | 81454.4 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 82109.3 | 82109.3 | 127109 | 1 | PROCESSED | 54329.710150463 | 54526 | 54053.5428240741 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011135 | The compact object in the massive X-ray binary 4U1700-37/HD153919 has been inferred to be a neutron star based on its spectral shape, but no pulsations have been observed. One possible explanation for the absence of observed pulsations is that the pulsed signal is beamed in directions other than our line of sight. This can be tested using Suzaku by searching for pulsations in the iron K line. This line is formed efficiently under almost all conditions of ionization and temperature, and so represents an X-ray bolometer which should respond to pulsed X-rays no matter where they are pointed. We plan to make such a search, and to probe the other properties of the wind and compact object in this system by observing with Suzaku for 80 ks away from eclipse. | GALACTIC POINT SOURCES | 4 | A | KALLMAN | TIMOTHY | NULL | NULL | USA | 1 | AO1 | IRON LINE VARIABILITY IN 4U1700-37 | XIS | N | | CYGNUS X-1 | 299.6124 | 35.133 | 71.28577556 | 3.01567368 | 256.2202 | 54038.1501273148 | 54038.8225 | 401059010 | 27706.8 | 30000 | 27706.8 | 27737.8 | 27706.8 | 27706.8 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 27689.2 | 27689.2 | 58083.9 | 0 | PROCESSED | 54325.0852662037 | 54526 | 54063.4924884259 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011141 | We request three, 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | B | NOWAK | MICHAEL | NULL | NULL | USA | 1 | AO1 | ENHANCING THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA | HXD | N | | GX 339-4 | 255.7025 | -48.7916 | 338.93635594 | -4.32587966 | 86.7489 | 54143.2316087963 | 54146.2003009259 | 401068010 | 77205.3 | 100000 | 83893.5 | 77205.3 | 0 | 82113.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94026 | 94026 | 256484 | 4 | PROCESSED | 54332.1519907407 | 54535 | 54167.7751851852 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011146 | Skewed iron emission lines from the inner accretion disk and broad-band disk reflection spectra are incisive diagnostics of relativistic effects and the inner accretion flow geometry in black hole binaries. With its high effective area, efficient instrument modes, and sensitivity in hard X-rays, Suzaku is ideally suited to fully exploit these diagnostics. We request a total of 154 ksec in up to four observations to observe a black hole transient in outburst, using a scheme tailored to accommodate different source fluxes and Suzaku's observing windows. We will support these observations with a global multi-wavelength network of observatories. Understanding accretion onto black holes is central to NASA's ``SEU'' research theme. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | NULL | NULL | USA | 1 | AO1-TOO | SUZAKU OBSERVATIONS OF A BLACK HOLE TRANSIENT IN OUTBURST | XIS | N | | SGR 1806-20 | 272.166 | -20.4729 | 9.94279657 | -0.27364584 | 269.9473 | 53987.9261921296 | 53989.1668287037 | 401092010 | 48915.5 | 50000 | 48915.5 | 48923.5 | 48931.5 | 48931.5 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 55408.5 | 55408.5 | 107175.9 | 1 | PROCESSED | 54322.8112615741 | 54526 | 54021.1112615741 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 012017 | The soft gamma-ray repeater SGR 1806-20 has recently emitted the most powerful giant flare ever observed from these sources. This probably involved a large scale restructuring of the magnetosphere, leading to observable variations in the properties of its persistent emission, from IR to hard X-rays. We propose to observe SGR 1806-20 with Suzaku considering the unique opportunity offered by this satellite to study the spectrum of this source simultaneously both in the soft and hard X-ray bands. We also suggest to coordinate this observation with a simultaneous XMM-Newton one, in order to obtain a significantly better determination of the broad band spectral parameters. | GALACTIC POINT SOURCES | 4 | B | MEREGHETTI | SANDRO | NULL | NULL | EUR | 1 | AO1 | COORDINATED SUZAKU AND XMM-NEWTON OBSERVATIONS OF SGR 1806-20 AFTER THE GIANT FLARE | HXD | N | | ALGOL | 47.0831 | 40.8965 | 149.0355551 | -14.93487401 | 244.4771 | 54167.6197222222 | 54169.6132986111 | 401093010 | 102164.2 | 105000 | 102164.2 | 102164.2 | 0 | 102164.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102472.9 | 102472.9 | 172192.8 | 1 | PROCESSED | 54329.1126041667 | 54736 | 54186.3983564815 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 012024 | Stellar and solar coronae reveal high-energy phenomena including the presence of accelerated electrons, explosive dissipation of magnetic energy, and heating to extreme temperatures. Many of these processes are likely to be physically related. We propose to use Suzaku's suite of instruments to observe the interplay between thermal and non-thermal high-energy processes in the active, eclipsing binary Algol. Our prime objective is the observation of hard X-rays above 10 keV, but also the appearance of an Fe fluorescence line that could be induced either by irradiation from flaring plasma or by electron beams. These models can be distinguished by correlating the emission with nonthermal hard X-rays as possibly detected by the HXD. | GALACTIC POINT SOURCES | 4 | C | GUEDEL | MANUEL | NULL | NULL | EUR | 1 | AO1 | A SYNOPTIC VIEW OF HIGH-ENERGY PHENOMENA IN THE CORONA OF ALGOL | HXD | Y | | IGR J16318-4848 | 247.9691 | -48.8061 | 335.63186461 | -0.44896472 | 266.5948 | 53961.4825 | 53964.3488310185 | 401094010 | 97253.8 | 100000 | 97269.8 | 97253.8 | 97269.8 | 97269.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 87112.8 | 87112.8 | 247605.9 | 5 | PROCESSED | 54330.6531365741 | 54526 | 54020.9181597222 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 012034 | We propose a detailed study of Compton thick X-ray absorption in neutral or weakly ionized material by using 100ksec of Suzaku observations of the strongly absorbed (N_H~2E24cm2) Galactic X-ray binary IGR J16318-4848. Measuring a high signal to noise ratio broad band spectrum will allow us to determine the curvature in the >10keV continuum caused by Compton downscattering in the absorber, to deduce its ionization state from observations of the Fe Kalpha line, and to study the variability of the source and the absorber. These observations will also shed more light onto the nature of the compact object in IGR J16318-4848. | GALACTIC POINT SOURCES | 4 | B | WILMS | JOERN | NULL | NULL | EUR | 1 | AO1 | OBSERVING IGR J16318-4848: PROBING COMPTON-THICK ABSORPTION | XIS | N | | XB 1916-053 | 289.7027 | -5.2415 | 31.35614078 | -8.46800846 | 250.2538 | 54047.242974537 | 54048.1119791667 | 401095010 | 38464.7 | 40000 | 39096.7 | 39088.7 | 38464.7 | 39096.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37485.7 | 37485.7 | 75082 | 2 | PROCESSED | 54324.2446296296 | 54735 | 54088.866087963 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 012038 | We propose Suzaku observations of the dipping low mass X-ray binaries XB1916-053, XB1323-619, EXO0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been recently demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the photoionised absorbers and reliably determine the values of the ionization parameter for each source, and the simultaneous spectra of HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components and to extend the photoionized absorber fits to higher energies. This will test the validity of the ionized absorber model also >10 keV. | GALACTIC POINT SOURCES | 4 | A | DIAZ TRIGO | MARIA | NULL | NULL | EUR | 1 | AO1 | BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS | XIS | Y | | HESS J1731-347 | 263.0179 | -34.7706 | 353.53173388 | -0.68198005 | 79.8005 | 54154.7807060185 | 54155.7432291667 | 401099010 | 40618.9 | 38000 | 40626.9 | 40618.9 | 0 | 40626.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34647.9 | 34647.9 | 83155.9 | 0 | PROCESSED | 54327.1666550926 | 54528 | 54160.3931944444 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 012042 | The hard (Gamma=2.0) TeV source HESS J1731-347 discovered in the H.E.S.S. Galactic plane survey has an intriguing possible counterpart seen in ROSAT survey data. The X-ray data show an unidentified, extended nebular structure with a hard spectrum, in close coincidence to the TeV source. It is plausible to assume that the same energetic particle population is responsible for the emission in both bands. Suzaku is optimally suited to establish the likely non-thermal nature of the X-ray spectrum and to search for the high-energy end of the emitting particle spectrum, which is likely visible in the HXD domain. The observations will help to clarify the nature of HESS J1731-347, which may be a new type of Galactic particle accelerator. | GALACTIC POINT SOURCES | 4 | A | PUEHLHOFER | GERD | NULL | NULL | EUR | 1 | AO1 | THE HIGH ENERGY PARTICLE SPECTRUM OF THE TEV/X-RAY NEBULA HESS J1731-347 | XIS | N | | 1E 1841-045 | 280.3141 | -4.8735 | 27.4352849 | 0.03686802 | 77.3227 | 53844.4525462963 | 53847.1328009259 | 401100010 | 97962.2 | 100000 | 97962.2 | 97970.2 | 97970.9 | 97970.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 63474 | 63474 | 231539.9 | 2 | PROCESSED | 54328.5835185185 | 54401 | 53907.2806597222 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 014204 | Anomalous X-ray Pulsars are young radio-quiet pulsars with unconventional properties challenging conventional wisdom on neutron star formation and evolution. Their slow rotation periods, unprecedented for their apparent youth, point to enormous surface magnetic fields, a thousand times stronger than the typical inferred radio-pulsar field. The origin of the X-ray emission from these pulsars is still being debated. The recent discovery of a hard nonthermal pulsed X-ray emission from 1E 1841-045 with RXTE well beyond 10keV, can probably be explain by a magnetospheric origin and should extend above 100keV. The HXD onboard Suzaku gives us a unique opportunity to characterize the high-energy part of the emission with the added advantage to use the XIS to characterize the lower energy data. | GALACTIC POINT SOURCES | 4 | A | HARRUS | ILANA | NORII | MIKIO | USJ | 1 | AO1 | SUZAKU OBSERVATIONS OF THE ANOMALOUS X-RAY PULSAR 1E~1841-045 IN THE SNR KES 73 | HXD | N | | HESSJ1813-178 | 273.3946 | -17.7704 | 12.87014503 | 0.01155473 | 90.9367 | 54160.8999768518 | 54162.2814699074 | 401101010 | 63839.1 | 65000 | 63847.1 | 63839.1 | 0 | 63847.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57756.1 | 57756.1 | 119351.9 | 1 | PROCESSED | 54326.8273726852 | 54736 | 54167.6346990741 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 014214 | Radio and X-ray observations towards the VHE gamma-ray source HESS J1813-178, initially dubbed being a dark accelerator , suggested its association with a SNR. However, a recent XMM observation confirmed earlier ASCA findings of an extended, center-filled X-ray source, not resembling the contours of the radio-detected SNR. We propose hard X-ray observations to investigate the alternatively plerionic origin of HESS J1813-178, given the wide spectral coverage possible by XIS/HXD. This will clarify the discrepancy between ASCA and recent INTEGRAL data. Constructing a valid spectral energy distribution will enable us to constrain the age and field strength of the particle accelerator powering the synchrotron emission and accurately model the radiation processes up to VHE energies. | GALACTIC POINT SOURCES | 4 | B | REIMER | OLAF | EBISAWA | KEN | USJ | 1 | AO1 | IS THE ASSOCIATION OF HESS J1813-178/SNR G12.8-0.0 CONCEALING ITS TRUE PLERIONIC NATURE? | HXD | Y | | EX HYA | 193.0706 | -29.2994 | 303.15288952 | 33.57198642 | 300.0004 | 54299.8912152778 | 54302.4377199074 | 402001010 | 100515.7 | 100000 | 100523.7 | 100515.7 | 0 | 100523.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91113.5 | 91113.5 | 219959.9 | 1 | PROCESSED | 54339.478912037 | 54707 | 54339.5139467593 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020008 | The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS. | GALACTIC POINT SOURCES | 4 | A | ISHIDA | MANABU | NULL | NULL | JAP | 2 | AO2 | MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS | HXD | Y | | V1223 SGR | 283.7445 | -31.105 | 5.0082738 | -14.31987205 | 79.9528 | 54203.4803240741 | 54204.9418055556 | 402002010 | 60706 | 60000 | 60706 | 60706 | 0 | 60706 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46286.1 | 46286.1 | 126271.9 | 2 | PROCESSED | 54327.481412037 | 54744 | 54210.6596875 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020008 | The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS. | GALACTIC POINT SOURCES | 4 | A | ISHIDA | MANABU | NULL | NULL | JAP | 2 | AO2 | MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS | HXD | Y | | 1RXSJ174459.5-172640 | 266.2467 | -17.4406 | 9.76958181 | 6.08973572 | 101.0461 | 54555.6304050926 | 54556.5834953704 | 402003010 | 43579.3 | 40000 | 43595.3 | 43579.3 | 0 | 43603.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29591.6 | 29591.6 | 82343.9 | 1 | PROCESSED | 54570.1429282407 | 54937 | 54570.1529282407 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 020015 | We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, which were detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the Suzaku fine spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test acrretion disk theories at intermediate mass accretion rates. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 2 | AO2 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | | 1RXSJ165256.3-264503 | 253.236 | -26.7533 | 355.1420085 | 10.81079439 | 277.5876 | 54337.0024421296 | 54338.0419444444 | 402004010 | 49582.2 | 40000 | 49582.2 | 49582.2 | 0 | 49582.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46662.1 | 46662.1 | 89777.9 | 2 | PROCESSED | 54404.494212963 | 54723 | 54350.4155092593 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020015 | We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, which were detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the Suzaku fine spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test acrretion disk theories at intermediate mass accretion rates. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 2 | AO2 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | | 1RXS J070407.9+26250 | 106.0341 | 26.4126 | 190.27497025 | 14.29877104 | 282.0717 | 54548.4868865741 | 54549.9862384259 | 402008010 | 58315.7 | 50000 | 58323.7 | 58315.7 | 0 | 58323.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 49476.6 | 49476.6 | 129527.8 | 0 | PROCESSED | 54566.3128240741 | 54933 | 54566.326712963 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 020029 | Soft Intermediate Polar (IP) is a small group of IPs whose X-ray spectrum is extremely soft compared with general IPs. Recent observations reveal that some soft IPs harbor a soft blackbody component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand possible evolutionary link from IPs to polars, the origin of the soft excess in polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure their temperature and flux systematically. | GALACTIC POINT SOURCES | 4 | C | ISHIDA | MANABU | NULL | NULL | JAP | 2 | AO2 | OBSERVATIONS OF SOFT INTERMEDIATE POLARS | XIS | Y | | 1RXS J180340.0+40121 | 270.932 | 40.2098 | 66.8583442 | 25.77561005 | 157.538 | 54478.0290972222 | 54479.1877777778 | 402009010 | 53090.7 | 50000 | 53090.7 | 53090.7 | 0 | 53090.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 44348.9 | 44348.9 | 100095.9 | 3 | PROCESSED | 54490.0612847222 | 54864 | 54490.0707291667 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020029 | Soft Intermediate Polar (IP) is a small group of IPs whose X-ray spectrum is extremely soft compared with general IPs. Recent observations reveal that some soft IPs harbor a soft blackbody component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand possible evolutionary link from IPs to polars, the origin of the soft excess in polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure their temperature and flux systematically. | GALACTIC POINT SOURCES | 4 | C | ISHIDA | MANABU | NULL | NULL | JAP | 2 | AO2 | OBSERVATIONS OF SOFT INTERMEDIATE POLARS | XIS | Y | | 4U 0142+61 | 26.4803 | 61.7944 | 129.32255084 | -0.39946076 | 40.959 | 54325.1695949074 | 54327.5209259259 | 402013010 | 99674.4 | 100000 | 99674.4 | 99674.4 | 0 | 99674.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 101609.6 | 101609.6 | 203129.7 | 4 | PROCESSED | 54404.5831944445 | 54730 | 54347.6221296296 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020058 | Recently, high energy pulsed x-ray emissions from anomalous x-ay pulsears have been founded. This emissions extend to neary 100 keV with photon index ~1, and the emission mechanism is unknown. In order to trace this enigmatic component, we propose the observation of the anomalous x-ray pulsar 4u 0142+61 with 100 ksec exposures. The main aim of this observation is to examine how high energy this emission extend to. Because the these emissions are almost 100% pulsed component, so using the pulse on-off method, we can achive the ultimate sensitivity not depending on the reproducibility of the background but depending only on the photon statistics. If the spectrum have the strong break neary ~250 keV, this emissions have originated as the compton scatterd photons in the star surface. | GALACTIC POINT SOURCES | 4 | A | ENOTO | TERUAKI | NULL | NULL | JAP | 2 | AO2 | THE PULSED HARD X-RAY EMISSION FROM ANOMALOUS X-RAY PULSAR 4U 0142+61 | HXD | Y | | PSR B1259-63 | 195.6821 | -63.8856 | 304.1741357 | -1.04108664 | 280.935 | 54288.622025463 | 54289.062662037 | 402014010 | 21863.4 | 20000 | 21871.4 | 21863.4 | 0 | 21871.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26860 | 26860 | 38063.9 | 1 | PROCESSED | 54328.4817361111 | 54696 | 54328.4884722222 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | | PSR B1259-63 | 195.6782 | -63.8867 | 304.17237227 | -1.04211039 | 282.6534 | 54290.6852083333 | 54291.1876041667 | 402014020 | 19481.7 | 20000 | 19481.7 | 19481.7 | 0 | 19481.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26911.1 | 26911.1 | 43378 | 1 | PROCESSED | 54328.4960416667 | 54696 | 54328.5032060185 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | | PSR B1259-63 | 195.6777 | -63.8873 | 304.1721261 | -1.04270018 | 282.6527 | 54292.6291319444 | 54293.1910763889 | 402014030 | 22721.7 | 20000 | 22721.7 | 22721.7 | 0 | 22721.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24280.8 | 24280.8 | 48545.9 | 0 | PROCESSED | 54339.0197106482 | 54707 | 54339.0273842593 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | | PSR B1259-63 | 195.6732 | -63.8823 | 304.17036556 | -1.03761834 | 285.8945 | 54294.6568865741 | 54295.3459953704 | 402014040 | 22914.9 | 20000 | 22914.9 | 22914.9 | 0 | 22914.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21070.6 | 21070.6 | 59495.9 | 1 | PROCESSED | 54339.3026273148 | 54709 | 54339.4142592593 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | | PSR B1259-63 | 195.6556 | -63.8839 | 304.16255435 | -1.03887935 | 293.4832 | 54304.2811226852 | 54304.6877777778 | 402014050 | 19702.3 | 20000 | 19702.3 | 19702.3 | 0 | 19702.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17754.9 | 17754.9 | 35127.9 | 0 | PROCESSED | 54339.2103587963 | 54707 | 54339.2175347222 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | | PSR B1259-63 | 195.6402 | -63.8787 | 304.15600524 | -1.03339065 | 289.9992 | 54315.2640856482 | 54316.0419444444 | 402014060 | 24038.8 | 20000 | 24038.8 | 24038.8 | 0 | 24038.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21580.8 | 21580.8 | 67195.9 | 1 | PROCESSED | 54404.5138425926 | 54722 | 54347.6946527778 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | | PSR B1259-63 | 195.6594 | -63.8834 | 304.16424752 | -1.0384525 | 292.9998 | 54330.0581481482 | 54330.6877777778 | 402014070 | 20481.2 | 20000 | 20481.2 | 20481.2 | 0 | 20482.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19470.3 | 19470.3 | 54364 | 0 | PROCESSED | 54404.5158680556 | 54724 | 54356.2228472222 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | | PSR B1259-63 | 195.6089 | -63.8685 | 304.14267075 | -1.0226082 | 321.9333 | 54348.2308449074 | 54348.6043287037 | 402014080 | 18332.7 | 20000 | 18340.7 | 18348.7 | 0 | 18332.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22351.3 | 22351.3 | 32260 | 0 | PROCESSED | 54404.5153356482 | 54724 | 54356.1999537037 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | | LS 5039 | 276.5633 | -14.9109 | 16.82651822 | -1.31880921 | 270.412 | 54352.6780555556 | 54358.4725 | 402015010 | 203239.9 | 200000 | 203239.9 | 203239.9 | 0 | 203239.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 181095 | 181095 | 442087.9 | 4 | PROCESSED | 54384.6553009259 | 54745 | 54384.7259027778 | 2.1.6.14 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020062 | The periodicity of TeV gamma-rays from the Galactic microquasar LS 5039 has recently been detected by the HESS Cherenkov telescope. We propose to conduct a simultaneous X-ray/VHE gamma-ray observations for a total of 200 ks of the microquasar with Suzaku XIS and HXD in conjuction with the HESS telescope. A full orbital period of 3.9 days is planned to be covered with Suzaku and HESS. The goal of this program is to study a possible correlation of X-TeV fluxes and spectral changes as a function of orbital phase, thereby shedding a new light on the origin of high-energy radiation from the microquasar system. | GALACTIC POINT SOURCES | 4 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 2 | AO2 | SIMULTANEOUS SUZAKU AND HESS OBSERVATIONS OF THE TEV GAMMA-RAY MICROQUASAR LS 5039 | HXD | Y | | HETEJ1900.1-2455 | 285.0506 | -24.9802 | 11.25454685 | -12.90928139 | 259.4192 | 54389.5913425926 | 54390.5071064815 | 402016010 | 41759.1 | 40000 | 41778.8 | 41759.1 | 0 | 41775.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39906.3 | 39906.3 | 79105.8 | 1 | PROCESSED | 54403.1128935185 | 54771 | 54403.1292708333 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020068 | We propose a 40 ks observation of the accreting millisecond pulsar HETE J1900.1-2455, which was discovered by HETE-2 only recently. Good sensitivity in 10-100keV and enough timing resolution of HXD on Suzaku allow us to measure the light curve and the phase resolved spectra of its hard X-ray pulsation, with which we study the physical parameters of the Comptonizing plasma that is considered as the source of the hard X-ray emission of accreting millisecond pulsars. With XIS, we study the radiation from the accretion disk and the neutron star surface, and search for spectral features such as emission lines or absorption edges, which will provide information on the binary environment. | GALACTIC POINT SOURCES | 4 | B | SUZUKI | MOTOKO | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY PULSATION OF ACCRETION-DRIVEN MILLISECOND PULSAR HETE J1900.1-2455 | HXD | Y | | 4U 1700+24 | 256.6316 | 23.9071 | 45.07419011 | 32.98144858 | 280.149 | 54334.7787615741 | 54335.875162037 | 402023010 | 50244.5 | 50000 | 50252.5 | 50260.5 | 0 | 50244.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45326.8 | 45326.8 | 94715.8 | 2 | PROCESSED | 54404.5649884259 | 54723 | 54350.4606481482 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020105 | We propose the observation of Neutron Star Low Mass X-ray Binary (LMXB) system 4U 1700+24.This system would be Advection Dominant Accretion Flow (ADAF) and we research the hard-tail in hard X-ray region. Though the X-ray intensity in a Low Hard state is very faint, $sim$10$^{33}$ erg/s we can obtain the energy spectrum of 10-100keV for the first time using Suzaku 50ksec observation because it is the nearest LMXB. If we know the extension of hard-tail in low luminosity state, we can understand the physical state of electron in the accretion disk and/or compact object. Suzaku is the best satellite to research the faint emission around 100keV. | GALACTIC POINT SOURCES | 4 | B | NAGAE | OSAMU | NULL | NULL | JAP | 2 | AO2 | STUDY OF MASS ACCRETION FLOW IN ADAF FOR LOW LUMINOUS X-RAY BINARY 4U 1700+24 | HXD | Y | | CYG OB2 ASSOCIATION | 308.2175 | 41.2935 | 80.16491027 | 0.83267098 | 220.3949 | 54452.9185532407 | 54453.843912037 | 402030010 | 41114.7 | 40000 | 41114.7 | 41114.7 | 0 | 41114.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37918.1 | 37918.1 | 79943.9 | 0 | PROCESSED | 54460.6387962963 | 54828 | 54460.6521643518 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020150 | Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku. | GALACTIC POINT SOURCES | 4 | C | KITAMOTO | SHUNJI | NULL | NULL | JAP | 2 | AO2 | STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130 | XIS | Y | | TEVJ2032+4130 | 308.0461 | 41.5016 | 80.25613164 | 1.05964615 | 221.0839 | 54451.984212963 | 54452.9176157407 | 402031010 | 40043.9 | 40000 | 40043.9 | 40043.9 | 0 | 40043.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37309.1 | 37309.1 | 80641.9 | 1 | PROCESSED | 54460.6387384259 | 54828 | 54460.6569675926 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020150 | Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku. | GALACTIC POINT SOURCES | 4 | C | KITAMOTO | SHUNJI | NULL | NULL | JAP | 2 | AO2 | STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130 | XIS | Y | | EV LAC | 341.7127 | 44.3232 | 100.60502245 | -13.08073089 | 256.1601 | 54432.9692013889 | 54434.4655208333 | 402032010 | 68949.3 | 100000 | 68949.3 | 69133.3 | 0 | 69127.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 65011.3 | 65011.3 | 129232.8 | 2 | PROCESSED | 54441.0700231482 | 54808 | 54441.0876851852 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021013 | We propose a 100 ks Suzaku XIS observation of the dMe flare star EV Lac to measure coronal element abundances during quiescence and flares of different sizes. EV Lac undergoes frequent small flares, and is known to have undergone a very large flare at ~300 times the quiescent count rate in 2000. Coronal abundance changes shed light on the process of chromospheric evaporation under conditions different to those on the Sun. Depending on the size and spectrum of the flare, we may also be able to detect a hard burst of emission that would serve as a time marker for particle acceleration during the flare. | GALACTIC POINT SOURCES | 4 | C | HWANG | UNA | NULL | NULL | USA | 2 | AO2 | FLARE AND QUIESENT CONORAL ELEMENT ABUNDANCES IN EV LAC | XIS | Y | | SIGMA GEM | 115.843 | 28.9438 | 191.13214337 | 23.30670736 | 104.4403 | 54394.4090162037 | 54397.9690162037 | 402033010 | 142889.7 | 125000 | 142889.7 | 142993.6 | 0 | 142985.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 124447.1 | 124447.1 | 307541.6 | 1 | PROCESSED | 54407.7917824074 | 54776 | 54407.830474537 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021014 | Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission on RS CVn binaries. We propose a 125 ksec (3-4 day elapsed time) observation of the RS CVn binary Sigma Gem. Our goals are i) to better characterize its hard (>10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data, and iv) compare long duration flares on Sigma Gem with the 6 hour flares of Sigma2 CrB. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability at 10-25 keV provided by HXD. | GALACTIC POINT SOURCES | 4 | C | BROWN | ALEXANDER | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL STRUCTURE ON THE RS CVN BINARY SIGMA GEM (K0III +?) | HXD | Y | | HD432 | 2.3072 | 59.1394 | 117.5327944 | -3.28915956 | 247.7181 | 54469.7038310185 | 54470.5154513889 | 402034010 | 38240.6 | 40000 | 38248.6 | 38240.6 | 0 | 38248.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35050.3 | 35050.3 | 70120 | 1 | PROCESSED | 54542.2134722222 | 54908 | 54483.4635532407 | 2.2.7.18 | 4 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021016 | Suzaku XIS spectra of three "X-ray deficient" Hertzsprung gap giants will explore why they display anomalous coronal behavior compared with cooler giants only slightly further advanced in their evolution. The apparent sharp transition in coronal properties on the way to helium flash might be caused by disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. A key discriminator is the coronal energy distribution, especially enhanced and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution; all three have supporting high resolution UV spectra. Expanding the sample of high quality, high energy information on this key class of objects is essential for probing their odd behavior. | GALACTIC POINT SOURCES | 4 | C | AYRES | THOMAS | NULL | NULL | USA | 2 | AO2 | ANOMALOUS CORONAE OF HERTZSPRUNG GAP GIANTS | XIS | Y | | HD432 | 2.3079 | 59.1397 | 117.53319828 | -3.2889222 | 246.0535 | 54471.6956944444 | 54472.297349537 | 402034020 | 26984.4 | 27000 | 26984.4 | 26984.4 | 0 | 26984.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24601 | 24601 | 51975.9 | 0 | PROCESSED | 54483.3790740741 | 54871 | 54483.3863773148 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021016 | Suzaku XIS spectra of three "X-ray deficient" Hertzsprung gap giants will explore why they display anomalous coronal behavior compared with cooler giants only slightly further advanced in their evolution. The apparent sharp transition in coronal properties on the way to helium flash might be caused by disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. A key discriminator is the coronal energy distribution, especially enhanced and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution; all three have supporting high resolution UV spectra. Expanding the sample of high quality, high energy information on this key class of objects is essential for probing their odd behavior. | GALACTIC POINT SOURCES | 4 | C | AYRES | THOMAS | NULL | NULL | USA | 2 | AO2 | ANOMALOUS CORONAE OF HERTZSPRUNG GAP GIANTS | XIS | Y | | ZETA OPH | 249.2878 | -10.5628 | 6.28378927 | 23.59180747 | 94.9452 | 54540.8758912037 | 54543.8543287037 | 402038010 | 105583.7 | 100000 | 105591.7 | 105591.7 | 0 | 105583.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79981.3 | 79981.3 | 257317.8 | 2 | PROCESSED | 54553.3433217593 | 54922 | 54553.3785300926 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021022 | Zeta Oph is a well known optical and UV variable star and is now known to displays both short (hours) and long (years) term X-ray variability. The short term variability has different periods for the soft and hard X-ray bands. The soft period being identical with the UV DAC reoccurrence period. The hard period is 40 percent smaller than the soft period and the source of it's variability is thus far unclear. Zeta Oph has been observed by several X-ray telescopes over a 22 year time span and the observations show significant variations in the total observed X-ray flux. We are requesting an XIS observation of this star to develop: 1) a greater understanding of the hard X-ray emission; 2) confirm the hard and soft periodicities, and; 3) provide further monitoring of the long term variability. | GALACTIC POINT SOURCES | 4 | C | WALDRON | WAYNE | NULL | NULL | USA | 2 | AO2 | MULTIPLE X-RAY EMISSION PERIODICITY IN THE RAPIDLY ROTATING O-STAR, ZETA OPH | XIS | Y | | ETA CARINAE | 161.2181 | -59.7282 | 287.59637986 | -0.67920855 | 289.0006 | 54274.2459259259 | 54275.9015509259 | 402039010 | 58396.1 | 50000 | 58404.1 | 58396.1 | 0 | 58404.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51552 | 51552 | 143009.9 | 1 | PROCESSED | 54322.4959953704 | 54695 | 54322.5140856482 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021026 | XMM-Newton observations in 2003 suggest that X-ray emission from Eta Carinae has a hard X-ray component above 10 keV in addition to the thermal emission with kT ~3-5 keV. The excess is apparently strongest near the 2-10 keV X-ray maximum, and possibly produced by very hot plasma or 1st-order Fermi acceleration of particles which then inverse Compton-upscatter UV seed photons from the stellar photospheres. We propose a 50 ksec observation of Eta Carinae with the Suzaku telescope during AO2, compare the X-ray spectrum with earlier observations and determine the level of emission at E >9 keV. | GALACTIC POINT SOURCES | 4 | B | HAMAGUCHI | KENJI | NULL | NULL | USA | 2 | AO2 | HARD X-RAY EMISSION FROM ETA CARINAE | HXD | Y | | RT CRU | 188.7055 | -64.6161 | 301.15157727 | -1.80180428 | 281.609 | 54283.5270023148 | 54284.2433333333 | 402040010 | 50880.6 | 50000 | 50880.6 | 50880.6 | 0 | 50880.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42850.6 | 42850.6 | 61887.9 | 0 | PROCESSED | 54328.4465972222 | 54695 | 54328.4668055556 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021102 | Symbiotic stars are interacting binaries in which a white dwarf (WD) accretes from the wind of a red giant. Their X-ray emission is typically very soft. Recently, however, 4 symbiotics have been detected out to almost 100 keV. Suzaku observations of two of these sources revealed that the hard X-rays emanated from an extremely hot thermal plasma. One means of producing such hot gas is accretion onto a near Chandrasekhar-mass WD. We propose to use the unique capabilities of Suzaku to test this hypothesis. We will use broad-band X-ray spectral fitting to determine the temperature of the hot plasma, hard X-ray timing studies to search for or constrain rapid variations due to either magnetic or non-magnetic accretion, and Fe line diagnostics to investigate the role of scattering. | GALACTIC POINT SOURCES | 4 | B | SOKOLOSKI | JENNIFER | NULL | NULL | USA | 2 | AO2 | ARE HARD X-RAY SYMBIOTICS PROGENITORS OF TYPE IA SUPERNOVAE? | HXD | Y | | VY AQR | 318.0426 | -8.8307 | 41.59091784 | -35.22055705 | 252.6652 | 54414.6528587963 | 54415.3855787037 | 402043010 | 25447.3 | 20000 | 25447.3 | 25447.3 | 0 | 25447.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22360.5 | 22360.5 | 63299.9 | 2 | PROCESSED | 54423.1616203704 | 54790 | 54423.1702314815 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021105 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 2 | AO2 | BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE | XIS | Y | | SW UMA | 129.1769 | 53.4845 | 164.80593722 | 36.96002764 | 98.2716 | 54410.2367708333 | 54410.6252199074 | 402044010 | 16899.1 | 20000 | 16907.1 | 16899.1 | 0 | 16907.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13896.9 | 13896.9 | 33551.9 | 1 | PROCESSED | 54417.6038657407 | 54784 | 54417.2697569444 | 2.1.6.16 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021105 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 2 | AO2 | BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE | XIS | Y | | SS AUR | 93.3423 | 47.7333 | 166.0127795 | 13.79596984 | 289.1089 | 54529.7508796296 | 54530.180775463 | 402045010 | 19471.4 | 20000 | 19471.4 | 19471.4 | 0 | 19471.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17378 | 17378 | 37135.9 | 0 | PROCESSED | 54539.2152083333 | 54905 | 54539.2223726852 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021105 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 2 | AO2 | BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE | XIS | Y | | BZ UMA | 133.4243 | 57.801 | 159.01672768 | 38.83001001 | 307.4767 | 54549.9926388889 | 54550.4446064815 | 402046010 | 29746.6 | 20000 | 29754.6 | 29754.6 | 0 | 29746.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24921.2 | 24921.2 | 39045.9 | 0 | PROCESSED | 54566.2147800926 | 54933 | 54566.2225231482 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021105 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 2 | AO2 | BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE | XIS | Y | | GX17+2 | 274.0087 | -14.1006 | 16.37694194 | 1.24456043 | 269.7113 | 54362.2773032407 | 54362.8543402778 | 402050010 | 19095.9 | 20000 | 19095.9 | 19104.4 | 0 | 19095.9 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 16044.5 | 16044.5 | 49849.9 | 0 | PROCESSED | 54384.4371527778 | 54751 | 54384.4487037037 | 2.1.6.14 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021111 | Z sources are bright low-mass X-ray binaries with variable spectra that describe a characteristic "Z" shape in an X-ray color-color plot. The forces driving the spectral shape and variability of the Z sources are not well understood, as there are few detectors with the necessary capabilities. GX17+2 is a Sco-type Z sources with an unusual time-varying hard X-ray tail whose origin is uncertain. Bright X-ray sources also illuminate the interstellar medium. Highly absorbed X-ray sources show halos due to dust scattering as well as absorption features. These will allow us to place constraints on interstellar dust and gas models. Suzaku can address all of these issues with simultaneous observations of the hard X-ray continuum and the dust-scattered X-ray halo. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 2 | AO2 | OBSERVING THE SPECTRUM AND HALO OF GX17+2 | HXD | Y | | GX17+2 | 274.0098 | -14.0991 | 16.37876929 | 1.24433559 | 268.3778 | 54370.5988078704 | 54371.2502199074 | 402050020 | 23011.7 | 20000 | 23019.7 | 23025.8 | 0 | 23011.7 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 19048.8 | 19048.8 | 56276 | 0 | PROCESSED | 54402.3354976852 | 54769 | 54402.3511921296 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021111 | Z sources are bright low-mass X-ray binaries with variable spectra that describe a characteristic "Z" shape in an X-ray color-color plot. The forces driving the spectral shape and variability of the Z sources are not well understood, as there are few detectors with the necessary capabilities. GX17+2 is a Sco-type Z sources with an unusual time-varying hard X-ray tail whose origin is uncertain. Bright X-ray sources also illuminate the interstellar medium. Highly absorbed X-ray sources show halos due to dust scattering as well as absorption features. These will allow us to place constraints on interstellar dust and gas models. Suzaku can address all of these issues with simultaneous observations of the hard X-ray continuum and the dust-scattered X-ray halo. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 2 | AO2 | OBSERVING THE SPECTRUM AND HALO OF GX17+2 | HXD | Y | | 4U1705-44 | 257.2319 | -44.0961 | 343.32770356 | -2.34122442 | 265.637 | 54348.6112847222 | 54349.0140509259 | 402051010 | 13343.6 | 15000 | 13343.6 | 13343.6 | 0 | 13343.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9370.6 | 9370.6 | 34791.9 | 1 | PROCESSED | 54404.5443865741 | 54773 | 54356.2627430556 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021113 | We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2 | X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS | XIS | Y | | 4U1705-44 | 257.2347 | -44.0965 | 343.32858118 | -2.34307771 | 294.8341 | 54381.763275463 | 54382.2015509259 | 402051020 | 21971.3 | 15000 | 21979.3 | 21981 | 0 | 21971.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15688 | 15688 | 37856 | 1 | PROCESSED | 54402.6262847222 | 54770 | 54402.6586226852 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021113 | We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2 | X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS | XIS | Y | | 4U1705-44 | 257.2244 | -44.1021 | 343.31966899 | -2.34047423 | 86.9924 | 54516.9847569444 | 54517.6182175926 | 402051030 | 25995.6 | 15000 | 26051.6 | 25995.6 | 0 | 26051.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20820.5 | 20820.5 | 54723.9 | 1 | PROCESSED | 54535.186875 | 54901 | 54535.2030439815 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021113 | We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2 | X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS | XIS | Y | | 4U1705-44 | 257.2229 | -44.1035 | 343.31790137 | -2.34044351 | 107.4157 | 54543.8610532407 | 54544.5210532407 | 402051040 | 20074.4 | 15000 | 20074.4 | 20074.4 | 0 | 20082.4 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 13411.3 | 13411.3 | 57017.9 | 1 | PROCESSED | 54553.1792708333 | 54922 | 54553.1912268518 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021113 | We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2 | X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS | XIS | Y | | AQL X-1 | 287.816 | 0.5784 | 35.71219982 | -4.14539755 | 284.0925 | 54371.6493402778 | 54372.062662037 | 402053010 | 13825.2 | 15000 | 13825.2 | 13825.2 | 0 | 13825.2 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 13745 | 13745 | 35704 | 0 | PROCESSED | 54402.3403009259 | 54769 | 54402.3541550926 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | | AQL X-1 | 287.8179 | 0.5789 | 35.71351779 | -4.14685757 | 277.9777 | 54376.9927777778 | 54377.3516087963 | 402053020 | 15132.6 | 15000 | 15140.6 | 15142.3 | 0 | 15132.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11890.8 | 11890.8 | 30999.9 | 1 | PROCESSED | 54403.9097800926 | 54771 | 54403.9157175926 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | | AQL X-1 | 287.8182 | 0.5791 | 35.71383379 | -4.14703266 | 264.9589 | 54382.2112384259 | 54382.6877893518 | 402053030 | 19711.7 | 15000 | 19719.7 | 19727.7 | 0 | 19711.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17552.2 | 17552.2 | 41162 | 0 | PROCESSED | 54402.5631944444 | 54770 | 54402.5719328704 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | | AQL X-1 | 287.8171 | 0.5794 | 35.71359616 | -4.14591745 | 272.6027 | 54388.3395833333 | 54388.7225 | 402053040 | 17915.7 | 15000 | 17915.7 | 17915.7 | 0 | 17915.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17668.2 | 17668.2 | 33080 | 0 | PROCESSED | 54402.3989814815 | 54769 | 54402.4060648148 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | | AQL X-1 | 287.8181 | 0.5776 | 35.7124509 | -4.14763067 | 265.5384 | 54392.3838310185 | 54392.7918287037 | 402053050 | 17889.9 | 15000 | 17889.9 | 17889.9 | 0 | 17889.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16927.8 | 16927.8 | 35231.9 | 1 | PROCESSED | 54402.4102083333 | 54769 | 54402.4178935185 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | | AQL X-1 | 287.8172 | 0.5775 | 35.71194856 | -4.14687642 | 265.833 | 54397.9824074074 | 54398.5072222222 | 402053060 | 21364.8 | 15000 | 21460.8 | 21460.8 | 0 | 21364.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21402.2 | 21402.2 | 45343.9 | 0 | PROCESSED | 54407.3665856482 | 54776 | 54407.3747222222 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | | AQL X-1 | 287.8217 | 0.5796 | 35.71588636 | -4.14991498 | 243.6715 | 54403.2743171296 | 54403.66 | 402053070 | 17536.2 | 15000 | 17584.2 | 17604 | 0 | 17536.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14332.2 | 14332.2 | 33319.9 | 0 | PROCESSED | 54409.1263310185 | 54776 | 54409.1320138889 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y | | 2S 0921-630 | 140.6632 | -63.3 | 281.84517925 | -9.33739383 | 20.5636 | 54340.7614351852 | 54341.8335532407 | 402057010 | 43213.1 | 40000 | 43213.1 | 43221.1 | 0 | 43221.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15856.8 | 15856.8 | 92615.8 | 0 | PROCESSED | 54404.5875231482 | 54721 | 54353.4365625 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021118 | 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | USA | 2 | AO2 | PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 | XIS | Y | | 2S 0921-630 | 140.6643 | -63.2995 | 281.84516955 | -9.33669084 | 18.1705 | 54342.4079166667 | 54343.5134722222 | 402058010 | 45693.7 | 40000 | 45693.7 | 45693.7 | 0 | 45693.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43346.3 | 43346.3 | 95499.8 | 2 | PROCESSED | 54404.5950578704 | 54724 | 54356.2760763889 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021118 | 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | USA | 2 | AO2 | PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 | XIS | Y | | 2S 0921-630 | 140.6655 | -63.298 | 281.84446964 | -9.33525426 | 8.3442 | 54335.887025463 | 54336.9932175926 | 402059010 | 43131 | 40000 | 43131 | 43131 | 0 | 43131 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37162.2 | 37162.2 | 95559.8 | 0 | PROCESSED | 54404.6173263889 | 54721 | 54350.5504861111 | 2.1.6.15 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021118 | 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | USA | 2 | AO2 | PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 | XIS | Y | | 2S 0921-630 | 140.666 | -63.2982 | 281.84477381 | -9.33523447 | 8.344 | 54338.0511226852 | 54339.16 | 402060010 | 40342.3 | 40000 | 40350.3 | 40342.3 | 0 | 40350.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35646.4 | 35646.4 | 95799.9 | 2 | PROCESSED | 54404.6289814815 | 54721 | 54350.5629398148 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021118 | 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | USA | 2 | AO2 | PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 | XIS | Y | | IGR J17544-2619 | 268.6038 | -26.3314 | 3.23518966 | -0.33446224 | 84.5765 | 54544.5263425926 | 54547.2640509259 | 402061010 | 103417.3 | 72000 | 103811.5 | 103827.5 | 0 | 103417.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65565.6 | 65565.6 | 236505.9 | 3 | PROCESSED | 54566.5757175926 | 54933 | 54566.6106134259 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021121 | Supergiant Fast X-ray Transients are a newly-discovered class of x-ray binary with short outbursts and late O to early B supergiant companions. They are not persistently bright, but the nature of their low-level variability is not well known. Similarly short outbursts are also seen in bright HMXBs with supergiant companions such as Cyg X-1 and Vel X-1. The mechanism of these outbursts is unknown in all cases. We propose long pointings to the two best-studied SFXTs and a third object, XTE J1743-363, which seems to be transitional between SFXTs and persistent supergiant HMXBs. We will characterize their variability at low flux levels, both to understand the accretion mechanism and to enable surveys of archival data for new SFXTs. | GALACTIC POINT SOURCES | 4 | C | SMITH | DAVID | NULL | NULL | USA | 2 | AO2 | CHARACTERIZING THE SPECTRUM AND VARIABILITY OF THE SUPERGIANT FAST X-RAY TRANSIENTS | XIS | Y | | IGR J00370+6122 | 9.2836 | 61.3722 | 121.21895683 | -1.4519667 | 87.6081 | 54273.499849537 | 54274.230775463 | 402064010 | 34908.9 | 30000 | 35384.4 | 35400.4 | 0 | 34908.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33804.6 | 33804.6 | 63141.9 | 2 | PROCESSED | 54322.4609259259 | 54695 | 54322.4714236111 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021122 | We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. | GALACTIC POINT SOURCES | 4 | B | TOMSICK | JOHN | NULL | NULL | USA | 2 | AO2 | LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS | XIS | Y | | IGR J16207-5129 | 245.1895 | -51.5038 | 332.45599844 | -1.05021687 | 88.1855 | 54499.8231365741 | 54500.7841898148 | 402065010 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 49595.5 | 49595.5 | 83031.9 | 1 | PROCESSED | 54515.4883333333 | 54883 | 54515.6347800926 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021122 | We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. | GALACTIC POINT SOURCES | 4 | B | TOMSICK | JOHN | NULL | NULL | USA | 2 | AO2 | LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS | XIS | Y | | IGR J16207-5129 | 245.1891 | -51.5041 | 332.45561032 | -1.05025433 | 89.5006 | 54526.8661111111 | 54527.7502199074 | 402065020 | 32612.7 | 30000 | 32709.5 | 32713.3 | 0 | 32612.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28331.2 | 28331.2 | 76375.9 | 0 | PROCESSED | 54535.197974537 | 54901 | 54535.208599537 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021122 | We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. | GALACTIC POINT SOURCES | 4 | B | TOMSICK | JOHN | NULL | NULL | USA | 2 | AO2 | LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS | XIS | Y | | IGR J17391-3021 | 264.795 | -30.3419 | 358.06793122 | 0.44854091 | 89.216 | 54518.4950115741 | 54519.3961226852 | 402066010 | 36465.7 | 30000 | 36545.7 | 36593.7 | 0 | 36465.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31259.1 | 31259.1 | 77819.8 | 1 | PROCESSED | 54525.4924537037 | 54892 | 54525.5064699074 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021122 | We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. | GALACTIC POINT SOURCES | 4 | B | TOMSICK | JOHN | NULL | NULL | USA | 2 | AO2 | LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS | XIS | Y | | 4U 1907+09 | 287.4001 | 9.8965 | 43.79892996 | 0.51344636 | 85.3836 | 54209.4191666667 | 54211.2612731482 | 402067010 | 80628.3 | 65000 | 80628.3 | 80636.3 | 0 | 80636.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73268.5 | 73268.5 | 159147.9 | 2 | PROCESSED | 54329.3797685185 | 54702 | 54216.2674189815 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021123 | The HMXB 4U 1907+09 shows a rich phenomenology: two cyclotron lines, an uncommonly weak iron line, intermittent X-ray fading, and a recent torque reversal. Compared to other persistent supergiant X-ray pulsars it has been less well observed, although it is a prime target to study the interaction of the neutron star's X-rays with the stellar wind and the accretion column. The latter has been confirmed by our 60ks AO1 observation which allowed for the first detection of a soft excess below 2keV as well as the determination of the paramters of the fundamental cyclotron line with unprecedented accuracy. Due to an unusually low source state during the AO1 exposure, however, an additional observation of 65ks is needed to perform the first phase resolved analysis of this interesting source. | GALACTIC POINT SOURCES | 4 | B | POTTSCHMIDT | KATJA | NULL | NULL | USA | 2 | AO2 | THE BROAD BAND SPECTRUM OF 4U 1907+09 | HXD | N | | EXO 2030+375 | 308.0118 | 37.6951 | 77.17399477 | -1.17458429 | 56.3502 | 54234.8591666667 | 54236.1565277778 | 402068010 | 57607.1 | 40000 | 57607.1 | 57607.1 | 0 | 57607.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53395.4 | 53395.4 | 112067.8 | 2 | PROCESSED | 54328.8249768518 | 54702 | 54242.497962963 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021124 | We propose a 40 ks Suzaku observation to confirm EXO 2030+375's recently discovered ~10 keV cyclotron feature and constrain its second harmonic at ~20 keV. EXO 2030+375 is a 42-second Be/X-ray pulsar in an eccentric 46-day orbit. If confirmed the ~10 keV cyclotron feature will be the lowest in energy known for an accreting pulsar and will provide the missing piece to make EXO 2030+375 an ideal candidate to observationally test accretion theory. In addition, we will measure EXO 2030+375's spin frequency, study its pulse shape versus energy, and perform phase resolved spectroscopy. Suzaku will allow these studies to reach lower energies and provide high quality spectra at lower luminosities than in any previous observations. | GALACTIC POINT SOURCES | 4 | A | WILSON | COLLEEN | NULL | NULL | USA | 2 | AO2 | CONSTRAINING CYCLOTRON FEATURES IN A NORMAL OUTBURST OF EXO 2030+375 | HXD | Y | | 4U2206+54 | 331.9811 | 54.5897 | 100.6432606 | -1.04691755 | 90.2357 | 54236.1620949074 | 54237.812662037 | 402069010 | 103976.8 | 100000 | 103984.8 | 103990.6 | 0 | 103976.8 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 99784.2 | 99784.2 | 142581.9 | 1 | PROCESSED | 54327.6385300926 | 54695 | 54242.76625 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021125 | 4U 2206+54 is a high mass X-ray binary which is suspected to contain a neutron star accreting from the wind of its companion BD +53 2790. However, there has been no confirmed detection of X-ray pulsations, and while several authors have reported hints of a cyclotron line in the energy spectra near 30 keV, none have reported significant detections. We propose Suzaku observations to search for long-period pulsations with the XIS, and possible confirmation of the cyclotron line using HXD/PIN. | GALACTIC POINT SOURCES | 4 | A | FINGER | MARK | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THE PECULIAR HMXB 4U 2206+54 | HXD | Y | | CIRCINUS X-1 | 230.1633 | -57.1695 | 322.11384942 | 0.03740334 | 115.206 | 54530.1953240741 | 54531.5523032407 | 402070010 | 46411.3 | 43000 | 46411.3 | 46411.3 | 0 | 46411.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41821.3 | 41821.3 | 117196 | 0 | PROCESSED | 54550.2286226852 | 54916 | 54550.2459953704 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021128 | We propose a 100ks Suzaku observation of Circinus X-1 through the zero (dipping) phase to facilitate 2 important and independent science goals. (1) For the binary, we wish to better understand the viewing geometry, and investigate physical changes in the binary behavior as it relates to observed spectral changes through periastron passage. (2) Conduct a large angle scattering study of the X-ray halo surrounding Circinus X-1 to diagnose ISM grain properties (the line-of-sight position, size distribution, and grain density) near us, in complement with our Chandra halo studies at small angles on grain properties near the source. | GALACTIC POINT SOURCES | 4 | A | LEE | JULIA | NULL | NULL | USA | 2 | AO2 | CIRCINUS X-1 NEAR PERIASTRON: PROBING BINARY PHYSICS AND ISM GRAINS ALONG THE LINE OF SIGHT | XIS | Y | | GRS 1915+105 | 288.7933 | 10.9535 | 45.37037141 | -0.21130356 | 67.354 | 54227.6113657407 | 54229.0717476852 | 402071010 | 65656.8 | 37000 | 65656.8 | 65803.9 | 0 | 65672.8 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 56897.3 | 56897.3 | 126168 | 1 | PROCESSED | 54331.8102083333 | 54702 | 54235.5321759259 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021132 | We have discovered a connection between Fe line strength and QPO phase in RXTE observations of GRS 1915+105. This connection independently ties Fe lines to radii less than 100 R_Schw. QPO-phase-resolved Suzaku spectra will enable us to detect changes in the relativistic line profile (inner radius, equivalent width), to extend the connection to the broadband disk reflection spectrum, and to test models for the Fe line - QPO connection. Moreover, at CCD resolution, the connection can be used to over-constrain disk radii - a first step toward mapping the inner disk. We therefore request a 37 ksec TOO observation of GRS 1915+105. Understanding black hole accretion is fundamental to NASA's "SEU" theme. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | NULL | NULL | USA | 2 | AO2-TOO | THE RELATIVISTIC IRON LINE - QPO CONNECTION IN GRS 1915+105 | XIS | Y | | CYG X-1 | 299.5792 | 35.2719 | 71.39034122 | 3.11120593 | 84.3565 | 54220.8163657407 | 54221.783587963 | 402072010 | 45320.4 | 30000 | 45320.4 | 45328.4 | 0 | 45320.4 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 40187.3 | 40187.3 | 83566 | 2 | PROCESSED | 54405.9677430556 | 54773 | 54228.1718518518 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021133 | We request two additional 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | A | NOWAK | MICHAEL | NULL | NULL | USA | 2 | AO2 | CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA | HXD | Y | | CYG X-1 | 299.5451 | 35.2618 | 71.3671857 | 3.12971485 | 59.9371 | 54237.8204050926 | 54238.6480787037 | 402072020 | 33356.8 | 30000 | 33356.8 | 33364.9 | 0 | 33356.8 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 32563.7 | 32563.7 | 71503.9 | 1 | PROCESSED | 54324.0259143518 | 54695 | 54245.0149884259 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021133 | We request two additional 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | A | NOWAK | MICHAEL | NULL | NULL | USA | 2 | AO2 | CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA | HXD | Y | | SWIFT J1753.5-0127 | 268.3714 | -1.4588 | 24.89300861 | 12.1795145 | 261.3846 | 54362.8585185185 | 54365.4377777778 | 402088010 | 94600.5 | 93000 | 94608.5 | 94616.5 | 0 | 94600.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81739 | 81739 | 222836 | 3 | PROCESSED | 54404.7412268518 | 54743 | 54371.6366319444 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021147 | While the spectrally hard state represents the most common mode of accretion in black hole X-ray binaries, the nature of its accretion flow is poorly understood. We recently discovered cool accretion disks extending close to the innermost stable circular orbit in the hard states of two black hole transients. Such disks could give rise to strong reflection features, but instead these are weak or not detected. We propose a 70 ks Suzaku observation of Swift J1753.5-0127 (one of the two transients), which is currently in a prolonged hard state. Our goal is to put tight constraints on the strength of the reflection features and increase our understanding of the geometry of the spectrally hard component. Understanding accretion onto compact objects is fundamental to NASA's "SEU" theme. | GALACTIC POINT SOURCES | 4 | A | HOMAN | JEROEN | NULL | NULL | USA | 2 | AO2 | CONSTRAINING REFLECTION FEATURES IN THE HARD STATE OF BLACK HOLE X-RAY BINARIES | XIS | Y | | TW HYA | 165.4619 | -34.7081 | 278.67685486 | 22.95004903 | 99.3673 | 54429.0615625 | 54429.6946064815 | 402089020 | 20009.6 | 11000 | 20009.6 | 20017.6 | 0 | 20025.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17550 | 17550 | 54687.9 | 2 | PROCESSED | 54434.1323611111 | 54804 | 54434.1387268518 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 022007 | We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra. | GALACTIC POINT SOURCES | 4 | B | SCHMITT | JURGEN | NULL | NULL | EUR | 2 | AO2 | ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS | XIS | Y | | SU AUR | 73.9934 | 30.5715 | 172.51103259 | -7.93275707 | 85.9197 | 54339.1713541667 | 54340.7502199074 | 402090010 | 57303.4 | 55000 | 57311.4 | 57303.4 | 0 | 57311.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54384.8 | 54384.8 | 136401.8 | 1 | PROCESSED | 54404.664525463 | 54723 | 54350.6381597222 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 022007 | We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra. | GALACTIC POINT SOURCES | 4 | A | SCHMITT | JURGEN | NULL | NULL | EUR | 2 | AO2 | ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS | XIS | Y | | EXO 0748-676 | 117.1051 | -67.7525 | 279.97237585 | -19.82332654 | 158.0884 | 54459.2369560185 | 54460.2919444444 | 402092010 | 45898.8 | 40000 | 45912.6 | 45898.8 | 0 | 45904.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43574.7 | 43574.7 | 91135.8 | 1 | PROCESSED | 54483.1704050926 | 54854 | 54483.1839351852 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 022014 | We propose Suzaku observations of the dipping Low Mass X-ray Binaries (LMXBs) EXO 0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the absorbers and the HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components. This will allow to reliably determine the absolute values of the ionization parameters for each of the sources, which was not possible with XMM due to the lack of contemporaneous high energy spectra, providing for a detailed comparison of the absorbers with source properties such as luminosity. | GALACTIC POINT SOURCES | 4 | C | DIAZ TRIGO | MARIA | NULL | NULL | EUR | 2 | AO2 | BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS | XIS | Y | | SGR 1806-20 | 272.1687 | -20.4711 | 9.94559743 | -0.27498509 | 268.1397 | 54387.2332060185 | 54388.333599537 | 402094010 | 52247.7 | 50000 | 52247.7 | 52271.7 | 0 | 52263.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50089.5 | 50089.5 | 95059.9 | 1 | PROCESSED | 54403.9442361111 | 54771 | 54403.9548611111 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 022016 | Among magnetars, SGR 1806-20 is particularly interesting since it emitted two years ago the most powerful giant flare ever observed. We are performing a long term monitoring in the soft X-rays with XMM-Newton and hard X-rays with INTEGRAL to study how the source evolves back to quiescence. We obtained in AO-1 a Suzaku observation that was carried out simultaneously with XMM-Newton and provided for the first time a broad band spectrum of SGR 1806-20 on a short timescale. A new observation is required to study the spectral variability in the hard X-ray range and possibly the properties of bursts. | GALACTIC POINT SOURCES | 4 | C | MEREGHETTI | SANDRO | NULL | NULL | EUR | 2 | AO2 | CONTINUED MONITORING OF SGR 1806-20 AFTER THE GIANT FLARE WITH SUZAKU AND XMM-NEWTON | HXD | Y | | GT MUS | 174.8799 | -65.348 | 295.52044001 | -3.51633969 | 94.8564 | 54446.4736689815 | 54449.187662037 | 402095010 | 93308.7 | 80000 | 93308.7 | 93308.7 | 0 | 93308.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94696.5 | 94696.5 | 234469.9 | 3 | PROCESSED | 54460.7354976852 | 54828 | 54460.7707060185 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 022020 | We propose to perform broad-band X-ray spectroscopy of the RS CVn-like system GT Muscae, with the aim to study the thermal and non-thermal components of its X-ray emitting plasma. Our target is a known hard X-ray source, detected with Uhuru and recently with Integral/IBIS in the 20-40 keV band, but lacking a dedicated observation with modern X-ray spectrometers. The proposed observation will allow us to investigate both the quiescent and flaring states of this complex (possibly interacting) binary system, by means of a variability study and a time-resolved spectral analysis of its X-ray emission. We aim to detect and constrain the non-thermal hard X-ray emission component, and to search for a possible Fe Kalpha line emission, thanks to the superb broad-band spectral capabilities of Suzaku. | GALACTIC POINT SOURCES | 4 | B | MAGGIO | ANTONIO | NULL | NULL | EUR | 2 | AO2 | BROAD-BAND X-RAY SPECTROSCOPY OF AN EXTREMELY ACTIVE CORONAL SOURCE | HXD | Y | | HD161103 | 266.1888 | -27.2272 | 1.35850162 | 1.05434609 | 105.2351 | 54884.7946643518 | 54886.7057175926 | 403001010 | 71524.9 | 60000 | 71532.9 | 71524.9 | 0 | 71540.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59664.7 | 59664.7 | 165085.8 | 1 | PROCESSED | 54962.5615625 | 55330 | 54903.6732523148 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030005 | We propose Suzaku observations of gamma Cas analogues. The sources in this class are characterized by extremely high thermal temperature and iron fluorescent line. We aim to identify the hard X-ray production site using the XIS's spectral capability at the iron K complex and the wide-band sensitivity combining XIS and HXD PIN. | GALACTIC POINT SOURCES | 4 | B | MIURA | JUNICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUES | XIS | Y | | HD110432 | 190.599 | -63.0744 | 301.908501 | -0.22062002 | 344.9423 | 54718.9065740741 | 54719.7050231482 | 403002010 | 25333.2 | 25000 | 25333.2 | 25333.2 | 0 | 25333.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21343.6 | 21343.6 | 68977.9 | 0 | PROCESSED | 54777.5247337963 | 55148 | 54780.4451736111 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030005 | We propose Suzaku observations of gamma Cas analogues. The sources in this class are characterized by extremely high thermal temperature and iron fluorescent line. We aim to identify the hard X-ray production site using the XIS's spectral capability at the iron K complex and the wide-band sensitivity combining XIS and HXD PIN. | GALACTIC POINT SOURCES | 4 | B | MIURA | JUNICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUES | HXD | Y | | 1RXS J070407.9+26250 | 106.0316 | 26.4199 | 190.26714041 | 14.29962915 | 96.1437 | 54749.1266319444 | 54750.3682175926 | 403003010 | 53551.9 | 50000 | 53551.9 | 53551.9 | 0 | 53551.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41140.5 | 41140.5 | 107231.9 | 0 | PROCESSED | 54780.5096064815 | 55148 | 54780.5445949074 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030009 | Soft Intermediate Polar (IP) is a group of IPs whose X-ray spectra are extremely soft compared with general IPs. Recent observations reveal that some soft IPs have a soft blackbody emission component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand comprehensively the emission characteristics of polars and IPs in the soft X-ray band, and to follow possible evolutionary link from IPs to polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure its temperature and flux systematically. | GALACTIC POINT SOURCES | 4 | B | ISHIDA | MANABU | NULL | NULL | JAP | 3 | AO3 | OBSERVATIONS OF SOFT INTERMEDIATE POLARS | XIS | Y | | 1RXS J062518.2+73343 | 96.3307 | 73.5671 | 140.86801575 | 24.12512545 | 262.0383 | 54570.0388310185 | 54571.1252777778 | 403004010 | 50326.7 | 50000 | 50326.7 | 50326.7 | 0 | 50326.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50125.3 | 50125.3 | 93848.8 | 0 | PROCESSED | 54581.21875 | 54953 | 54581.2328472222 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030009 | Soft Intermediate Polar (IP) is a group of IPs whose X-ray spectra are extremely soft compared with general IPs. Recent observations reveal that some soft IPs have a soft blackbody emission component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand comprehensively the emission characteristics of polars and IPs in the soft X-ray band, and to follow possible evolutionary link from IPs to polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure its temperature and flux systematically. | GALACTIC POINT SOURCES | 4 | B | ISHIDA | MANABU | NULL | NULL | JAP | 3 | AO3 | OBSERVATIONS OF SOFT INTERMEDIATE POLARS | XIS | Y | | 1E 1048.1-5937 | 162.5452 | -59.8394 | 288.24102095 | -0.47209541 | 101.4368 | 54800.9597337963 | 54802.5927083333 | 403005010 | 100423.1 | 100000 | 100443 | 100423.1 | 0 | 100423.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68104.9 | 68104.9 | 141081.9 | 0 | PROCESSED | 54812.030462963 | 55178 | 54812.0471875 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030013 | Observations in soft X-ray through hard X-ray bands are key to understand the emission processes in the magnetosphere of Anomalous X-ray Pulsars (AXPs). We propose to observe the two AXPs, 1E 2259+586 and 1E 1048.1-5937, with SUZAKU. Although no detections of the hard X-ray emissions have been reported, the results of the simulation using XSPEC for HXD indicate that SUZAKU detects the hard X-ray emissions above 20~keV from both AXPs for the first time with a quite high probability. The time resolution of HXD is able to provide the pulse profiles and the phase-resolved spectra in hard X-rays emissions. With these results of the observations, SUZAKU will provide a crucial information to study the emission processes in the magnetosphere of AXPs. | GALACTIC POINT SOURCES | 4 | C | TAKATA | JUMPEI | NULL | NULL | JAP | 3 | AO3 | X-RAY OBSERVATIONS OF ANOMALOUS X-RAY PULSARS WITH SUZAKU | HXD | Y | | MARS-P1 | 102.8773 | 25.1625 | 190.24974394 | 11.19384085 | 298.0037 | 54559.3414814815 | 54559.4099421296 | 403006010 | 2904.8 | 100000 | 2904.8 | 2912.8 | 0 | 2912.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2909.6 | 2909.6 | 5911.9 | 0 | PROCESSED | 54577.0394791667 | 54953 | 54577.0446875 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P2 | 102.9198 | 25.1641 | 190.26475308 | 11.2294146 | 298.0203 | 54559.4100925926 | 54559.493275463 | 403006020 | 4854.6 | 100000 | 4854.6 | 4886.6 | 0 | 4870.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3612.1 | 3612.1 | 7183.9 | 0 | PROCESSED | 54577.0255208333 | 54953 | 54577.0304976852 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P3 | 102.9612 | 25.1565 | 190.28784034 | 11.26022306 | 298.032 | 54559.4933796296 | 54559.5766087963 | 403006030 | 3886 | 100000 | 3886 | 3910 | 0 | 3894 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3113.4 | 3113.4 | 7183.9 | 0 | PROCESSED | 54577.0439236111 | 54953 | 54577.0484259259 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P4 | 103.0016 | 25.1536 | 190.30618657 | 11.29219101 | 298.0476 | 54559.5767592593 | 54559.6599421296 | 403006040 | 2288.2 | 100000 | 2288.2 | 2288.2 | 0 | 2288.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2010 | 2010 | 7183.9 | 0 | PROCESSED | 54577.0485648148 | 54953 | 54577.0528935185 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P5 | 103.045 | 25.1496 | 190.32670814 | 11.32616716 | 298.0638 | 54559.6600462963 | 54559.7432407407 | 403006050 | 1956.2 | 100000 | 1956.2 | 1956.2 | 0 | 1956.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 1992.6 | 1992.6 | 7167.9 | 0 | PROCESSED | 54577.128599537 | 54953 | 54577.1345486111 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P6 | 103.0844 | 25.143 | 190.34808199 | 11.3557719 | 298.0743 | 54559.7434375 | 54559.8265972222 | 403006060 | 1939 | 100000 | 1939 | 1939 | 0 | 1939 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1804.6 | 1804.6 | 7181.9 | 0 | PROCESSED | 54577.1330208333 | 54953 | 54577.1376388889 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P7 | 103.127 | 25.1401 | 190.36726484 | 11.38956433 | 298.0907 | 54559.8267476852 | 54559.9029861111 | 403006070 | 2502.8 | 100000 | 2513.9 | 2510.8 | 0 | 2502.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1650.6 | 1650.6 | 6584 | 0 | PROCESSED | 54577.1437731482 | 54953 | 54577.1486342593 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P8 | 103.1682 | 25.1356 | 190.38738197 | 11.42154102 | 298.1062 | 54559.9031365741 | 54560.0072222222 | 403006080 | 2748.9 | 100000 | 2753.8 | 2757.8 | 0 | 2748.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 2286.4 | 2286.4 | 8984 | 0 | PROCESSED | 54577.1581712963 | 54953 | 54577.1637615741 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P9 | 103.2195 | 25.1275 | 190.41473742 | 11.46031922 | 298.1247 | 54560.0073726852 | 54560.0766666667 | 403006090 | 2150.6 | 100000 | 2150.6 | 2174.6 | 0 | 2150.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1891.9 | 1891.9 | 5975.9 | 0 | PROCESSED | 54577.1380439815 | 54953 | 54577.1428009259 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P10 | 103.2518 | 25.125 | 190.42954859 | 11.48582895 | 298.135 | 54560.0767708333 | 54560.16 | 403006100 | 3771.6 | 100000 | 3795.6 | 3771.6 | 0 | 3796 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4001.4 | 4001.4 | 7183.9 | 0 | PROCESSED | 54577.1489814815 | 54953 | 54577.1537847222 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P11 | 103.2936 | 25.1207 | 190.44969799 | 11.5184009 | 298.1493 | 54560.1601041667 | 54560.2433333333 | 403006110 | 4619.8 | 100000 | 4627.8 | 4619.8 | 0 | 4635.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4074.9 | 4074.9 | 7183.9 | 0 | PROCESSED | 54577.1689930556 | 54953 | 54577.1745023148 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P12 | 103.3358 | 25.1148 | 190.47148034 | 11.55063865 | 298.1645 | 54560.2434837963 | 54560.3266666667 | 403006120 | 3455 | 100000 | 3455 | 3455 | 0 | 3455 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2678 | 2678 | 7175.9 | 0 | PROCESSED | 54577.1742939815 | 54953 | 54577.1789467593 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P13 | 103.3779 | 25.1101 | 190.49210676 | 11.58330245 | 298.1799 | 54560.3267708333 | 54560.41 | 403006130 | 4251.8 | 100000 | 4267.8 | 4251.8 | 0 | 4267.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3529 | 3529 | 7183.9 | 0 | PROCESSED | 54577.924525463 | 54953 | 54577.9292939815 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P14 | 103.4188 | 25.1057 | 190.5119865 | 11.61511049 | 298.1941 | 54560.410150463 | 54560.4933333333 | 403006140 | 4825.2 | 100000 | 4849.2 | 4825.2 | 0 | 4857.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3721.4 | 3721.4 | 7175.9 | 0 | PROCESSED | 54577.9381712963 | 54953 | 54577.9434722222 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P15 | 103.4611 | 25.1019 | 190.53184536 | 11.64832678 | 298.2083 | 54560.4934375 | 54560.5766666667 | 403006150 | 3831 | 100000 | 3839 | 3831 | 0 | 3847 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3192.8 | 3192.8 | 7183.9 | 1 | PROCESSED | 54577.9287268518 | 54953 | 54580.5809837963 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P16 | 103.503 | 25.0968 | 190.55275085 | 11.68067717 | 298.2223 | 54560.5768171296 | 54560.66 | 403006160 | 2326.2 | 100000 | 2326.2 | 2326.2 | 0 | 2326.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 2134 | 2134 | 7179.9 | 0 | PROCESSED | 54577.9426851852 | 54953 | 54577.9478935185 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P17 | 103.5439 | 25.0908 | 190.5741012 | 11.71183533 | 298.237 | 54560.6601041667 | 54560.743287037 | 403006170 | 1978.2 | 100000 | 1978.2 | 1978.2 | 0 | 1978.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1959.6 | 1959.6 | 7182 | 0 | PROCESSED | 54578.0356481482 | 54953 | 54578.0406597222 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P18 | 103.5869 | 25.0943 | 190.58743765 | 11.74868918 | 298.2592 | 54560.7434837963 | 54560.8264351852 | 403006180 | 1861.8 | 100000 | 1861.8 | 1861.8 | 0 | 1861.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1939.6 | 1939.6 | 7153.9 | 0 | PROCESSED | 54578.0477893518 | 54953 | 54578.0530555556 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P19 | 103.6272 | 25.0809 | 190.61541806 | 11.77628093 | 298.2673 | 54560.8266319444 | 54560.9098842593 | 403006190 | 2839.8 | 100000 | 2839.8 | 2848.2 | 0 | 2843.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 1844.1 | 1844.1 | 7190 | 0 | PROCESSED | 54578.0419791667 | 54953 | 54578.0465625 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P20 | 103.6685 | 25.0732 | 190.63848879 | 11.80707935 | 298.2779 | 54560.9100347222 | 54560.9932175926 | 403006200 | 1849 | 100000 | 1849 | 1849 | 0 | 1849 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1222 | 1222 | 7183.9 | 0 | PROCESSED | 54578.0525115741 | 54953 | 54578.0575231482 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P21 | 103.7101 | 25.0688 | 190.65860601 | 11.8395058 | 298.2947 | 54560.9933217593 | 54561.0765509259 | 403006210 | 2880.8 | 100000 | 2880.8 | 2880.8 | 0 | 2880.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3451.6 | 3451.6 | 7183.9 | 0 | PROCESSED | 54578.0568634259 | 54953 | 54578.0612847222 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P22 | 103.7541 | 25.0677 | 190.67657625 | 11.87528798 | 298.3117 | 54561.0767013889 | 54561.1598842593 | 403006220 | 4024.6 | 100000 | 4040.6 | 4024.6 | 0 | 4047.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4102 | 4102 | 7183.9 | 0 | PROCESSED | 54578.0618402778 | 54953 | 54578.0665625 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P23 | 103.7955 | 25.0599 | 190.69976585 | 11.90614711 | 298.325 | 54561.1600347222 | 54561.2432175926 | 403006230 | 4518.8 | 100000 | 4526.8 | 4518.8 | 0 | 4534.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3686.8 | 3686.8 | 7183.9 | 0 | PROCESSED | 54578.1137384259 | 54953 | 54578.1176157407 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P24 | 103.8389 | 25.0556 | 190.72046804 | 11.94011608 | 298.3401 | 54561.2433680556 | 54561.3265509259 | 403006240 | 3423 | 100000 | 3423 | 3423 | 0 | 3423 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2511 | 2511 | 7183.9 | 0 | PROCESSED | 54578.1186226852 | 54953 | 54578.1234375 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P25 | 103.8803 | 25.0503 | 190.74132534 | 11.97202775 | 298.3546 | 54561.3266550926 | 54561.4098842593 | 403006250 | 4261.2 | 100000 | 4269.2 | 4261.2 | 0 | 4269.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3251.1 | 3251.1 | 7183.9 | 0 | PROCESSED | 54578.1278819444 | 54953 | 54578.1323032407 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P26 | 103.921 | 25.0474 | 190.75967691 | 12.00436516 | 298.3671 | 54561.4100347222 | 54561.4932175926 | 403006260 | 4797.6 | 100000 | 4813.6 | 4797.6 | 0 | 4821.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3762.2 | 3762.2 | 7183.9 | 0 | PROCESSED | 54578.132650463 | 54953 | 54578.1374074074 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | MARS-P27 | 103.964 | 25.0399 | 190.78318678 | 12.0366945 | 298.3836 | 54561.4933217593 | 54561.5418171296 | 403006270 | 1099.8 | 100000 | 1107.8 | 1099.8 | 0 | 1115.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1093.5 | 1093.5 | 4183.9 | 0 | PROCESSED | 54578.1206134259 | 54953 | 54578.1251273148 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | | AM HERCULES | 274.126 | 49.8084 | 77.81082077 | 25.81903319 | 234.8814 | 54768.8590162037 | 54771.3043287037 | 403007010 | 108496.5 | 100000 | 108504.5 | 108504.5 | 0 | 108496.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94467.1 | 94467.1 | 211257.7 | 3 | PROCESSED | 54788.3710532407 | 55156 | 54788.4722222222 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030021 | We propose the observation of the proto-type magnetic catacrysmic variables, AM Hercules, to search for possible hard X-ray tail on the thermal emission with Suzaku. To reduce the systematics of the estimation of the GSO background in the analyses, we propose the additional observation of blank sky near the object. | GALACTIC POINT SOURCES | 4 | C | TERADA | YUKIKATSU | NULL | NULL | JAP | 3 | AO3 | NON THERMAL EMISSION FROM THE POLAR AM HERCULES | HXD | Y | | AM HERCULES BGD | 282.0964 | 47.9785 | 77.40285415 | 20.2844947 | 234.9986 | 54771.3072106482 | 54772.3438310185 | 403008010 | 44360.1 | 40000 | 44368.1 | 44360.1 | 0 | 44392.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40411.5 | 40411.5 | 89551.9 | 1 | PROCESSED | 54788.1131018518 | 55154 | 54788.4288541667 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030021 | We propose the observation of the proto-type magnetic catacrysmic variables, AM Hercules, to search for possible hard X-ray tail on the thermal emission with Suzaku. To reduce the systematics of the estimation of the GSO background in the analyses, we propose the additional observation of blank sky near the object. | GALACTIC POINT SOURCES | 4 | C | TERADA | YUKIKATSU | NULL | NULL | JAP | 3 | AO3 | NON THERMAL EMISSION FROM THE POLAR AM HERCULES | XIS | Y | | ARCHES CLUSTER | 266.4808 | -28.778 | 0.16960578 | 0.02569084 | 109.9998 | 54911.0857407407 | 54913.7681712963 | 403009010 | 110793.3 | 100000 | 110793.3 | 110793.3 | 0 | 110793.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91657.8 | 91657.8 | 231741.7 | 3 | PROCESSED | 54962.9976388889 | 55330 | 54924.3822106482 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030029 | We propose to observe a hard X-ray ring which has an emission line around 6.4 keV, located at the north of the Arches cluster. The ring is probably produced by an energetic jet or a supernova explosion. We aim to determine the continuum shape, the center energy of the emission line, and the absorption column to figure out the origin of the ring. | GALACTIC POINT SOURCES | 4 | B | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 3 | AO3 | A 6.4 KEV RING AT THE NORTH OF THE ARCHES CLUSTER | XIS | Y | | GX 339-4 | 255.6944 | -48.7333 | 338.97952784 | -4.28620483 | 84.7264 | 54908.0786226852 | 54908.9613310185 | 403011010 | 43040.8 | 40000 | 43055.4 | 43040.8 | 0 | 43061.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35391.4 | 35391.4 | 76257.9 | 1 | PROCESSED | 54962.5393865741 | 55330 | 54917.4333796296 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030046 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 3 | AO3-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | Y | | GX 339-4 | 255.7293 | -48.7348 | 338.99236079 | -4.30539701 | 107.9544 | 54915.3430555556 | 54916.2711111111 | 403011020 | 39079.2 | 40000 | 39116.5 | 39079.2 | 0 | 39116.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 34785.2 | 34785.2 | 80165.8 | 0 | PROCESSED | 54963.1574537037 | 55330 | 54930.1609490741 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030046 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 3 | AO3-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | Y | | GX 339-4 | 255.7297 | -48.7352 | 338.99220289 | -4.30584956 | 108.3513 | 54920.4773958333 | 54921.5216435185 | 403011030 | 39638.4 | 40000 | 39663.3 | 39638.4 | 0 | 39663.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35068.6 | 35068.6 | 90186 | 0 | PROCESSED | 54962.832349537 | 55330 | 54931.0610416667 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030046 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 3 | AO3-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | Y | | LS I+61 303_1 | 40.1455 | 61.188 | 135.69810374 | 1.0510579 | 270.0003 | 54853.9515856482 | 54854.8648032407 | 403015010 | 40551.4 | 40000 | 40551.4 | 40551.4 | 0 | 40551.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25731.2 | 25731.2 | 78868 | 0 | PROCESSED | 54959.5385185185 | 55329 | 54880.5343865741 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030077 | We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. | GALACTIC POINT SOURCES | 4 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 3 | AO3 | X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 | HXD | Y | | LS I+61 303_2 | 40.1457 | 61.1877 | 135.69831419 | 1.05082335 | 270.0006 | 54856.6966087963 | 54858.1766666667 | 403016010 | 61066.7 | 60000 | 61078.4 | 61066.7 | 0 | 61078.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26659.1 | 26659.1 | 127839.8 | 1 | PROCESSED | 54962.0981481482 | 55329 | 54880.5522106482 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030077 | We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. | GALACTIC POINT SOURCES | 4 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 3 | AO3 | X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 | HXD | Y | | LS I+61 303_3 | 40.2018 | 61.1949 | 135.72005286 | 1.06843757 | 246.2753 | 54872.1842592593 | 54873.7252199074 | 403017010 | 68627.3 | 60000 | 68627.3 | 68627.3 | 0 | 68627.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65068.5 | 65068.5 | 133121.8 | 1 | PROCESSED | 54962.3298958333 | 55330 | 54893.4210300926 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030077 | We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. | GALACTIC POINT SOURCES | 4 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 3 | AO3 | X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 | HXD | Y | | HESS J0632+057 | 98.2456 | 5.8062 | 205.66072349 | -1.43796588 | 289.8173 | 54579.6856828704 | 54580.6877199074 | 403018010 | 44076 | 40000 | 44076 | 44076 | 0 | 44076 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41475.8 | 41475.8 | 86565.8 | 0 | PROCESSED | 54594.1453472222 | 54961 | 54594.1596990741 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030080 | We propose a 40 ks observation on HESS J0632+057, the newly discovered TeV gamma-ray source in the interacting region of Monoceros SNR and Rosette Nebula. Although this point-like source is found inside the error circle of an unidentified EGRET source 3EG J0634+0521, it has no clear counterpart at other wavelengths. Two sources, a weak X-ray source 1RXS J063258.3+05487 and a Be-star MCW 148, are found inside the error circle of HESS. The aim of the Suzaku observation is to obtain a clue to solve the yet feasible three scenarios of the TeV gamma-ray source. | GALACTIC POINT SOURCES | 4 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 3 | AO3 | INVESTIGATION ON HESS J0632+057 IN MONOCEROS/ROSETTE REGION | XIS | Y | | LMC X -3 | 84.7048 | -64.0785 | 273.57060216 | -32.09537201 | 185.5067 | 54822.3015856482 | 54823.8675694444 | 403020010 | 73973.8 | 60000 | 73973.8 | 73981.8 | 0 | 73987.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70050.5 | 70050.5 | 135283.8 | 1 | PROCESSED | 54840.1787615741 | 55206 | 54840.5013310185 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030102 | Ionized iron K absorption lines are commonly observed from high state black hole binaries. Thus the highly ionized plasma are thought to be generally associated with optically thick accretion disks. Huge outflow by the plasma has been confirmed by some of these objects, and thus such plasma is thought to have an important role on accretion flow. In order to establish generality of the plasma by detecting the absorption lines, and to distinguish whether creation mechanism of the plasma is determined by X-ray luminosity or there is another key parameter, we propose Suzaku observation of luminous persistent black hole binary LMC X-3, with exposure of 60ks. This observation will enable us to find critical parameters which determine the creation of the accretion disk wind. | GALACTIC POINT SOURCES | 4 | C | KUBOTA | AYA | NULL | NULL | JAP | 3 | AO3 | SEARCH FOR IRON K ABSORPTION LINES FROM LMC X-3 | XIS | Y | | RX J1712.6-2414 | 258.1492 | -24.2444 | 359.8664305 | 8.74215246 | 94.4586 | 54889.4875925926 | 54892.2710532407 | 403021010 | 110481.3 | 100000 | 110489.3 | 110481.3 | 0 | 110489.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89458.4 | 89458.4 | 240441.8 | 4 | PROCESSED | 54963.440462963 | 55330 | 54908.5588310185 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030106 | We propose to observe a peculiar Intermediate Polar, RX J1712.6-2414, which has no accretion disk around the white dwarf. This source shows the X-ray modulation only at the beat period and broad Fe-K emission lines in the phase-averaged spectrum. Our goal is to obtain a clear picture about the accretion flow geometry, which can explain the timing and spectral properties, utilizing the fine phase-resolved spectra. Furthermore, we examine the non-thermal emission from the source, since the magnetized white dwarf is a promising candidate of particle acceleration sites. | GALACTIC POINT SOURCES | 4 | B | MORI | HIDEYUKI | NULL | NULL | JAP | 3 | AO3 | ACCRETION FLOW AND EMISSION MECHANISM OF A DISKLESS INTERMEDIATE POLAR, RX J1712.6-2414 | XIS | Y | | YY DRA | 175.8686 | 71.6187 | 130.35712902 | 44.51671754 | 282.0676 | 54632.7758217593 | 54633.4098842593 | 403022010 | 29185.1 | 30000 | 29185.1 | 29185.1 | 0 | 29185.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27474.3 | 27474.3 | 54777.9 | 1 | PROCESSED | 54644.1413541667 | 55013 | 54644.1517592593 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030107 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | C | YUASA | TAKAYUKI | NULL | NULL | JAP | 3 | AO3 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | | TV COL | 82.3326 | -32.8641 | 236.83580562 | -30.63495041 | 295.9146 | 54573.7555555556 | 54574.6668634259 | 403023010 | 35836.7 | 40000 | 35836.7 | 35836.7 | 0 | 35836.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30102.3 | 30102.3 | 78729.9 | 0 | PROCESSED | 54587.0541666667 | 54953 | 54587.0666550926 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030107 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | C | YUASA | TAKAYUKI | NULL | NULL | JAP | 3 | AO3 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | | IGR J16194-2810 | 244.8908 | -28.0663 | 349.1669856 | 15.58223604 | 95.1879 | 54867.1762152778 | 54868.4314236111 | 403024010 | 45568.7 | 50000 | 45568.7 | 45573.8 | 0 | 45568.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38785.9 | 38785.9 | 108435.8 | 1 | PROCESSED | 54962.2222685185 | 55329 | 54880.5743518518 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030121 | We propose to observe the weakly magnetized neutron star X-ray binary, IGR J16194-2810. This target object has almost constant luminosity and is expected to be state of ADAF. Assuming that we observe the object using HXD and XIS of the Suzaku for 50ks, we can investigate the soft X-ray emission from the NS and/or the accretion disk and hard X-ray tail. Comparing Black Body and Disk Black Body parameters of this object with that of fainter source, 4U 1700+24, we obtain a picture of accretion disk and accretion flow. If we measure the photon index and cutoff energy of the hard tail, we can reveal the physical condition of corona surrounding the NS or the disk. Only Suzaku can carry out this observation which observe soft-thermal and hard-nonthermal X-ray emission from faint source. | GALACTIC POINT SOURCES | 4 | C | NAGAE | OSAMU | NULL | NULL | JAP | 3 | AO3 | ELUCIDATION OF THE ADAF OBSERVING LOW LUMINOUS NEUTRON STAR X-RAY BINARY IGR J16194-2810 | HXD | Y | | V709 CAS | 7.1951 | 59.3013 | 120.03837674 | -3.44309479 | 84.0816 | 54637.4334837963 | 54638.1542824074 | 403025010 | 35898.2 | 30000 | 35898.2 | 35898.2 | 0 | 35898.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33382.3 | 33382.3 | 62267.9 | 0 | PROCESSED | 54648.0905555556 | 55014 | 54648.3358101852 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030140 | Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y | | IGR J17303-0601 | 262.5864 | -5.9814 | 17.93788623 | 15.02149808 | 100.7922 | 54878.4233217593 | 54879.3355787037 | 403026010 | 32963.5 | 30000 | 32963.5 | 32963.5 | 0 | 32963.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27755.9 | 27755.9 | 78818 | 2 | PROCESSED | 54945.1581712963 | 55325 | 54893.4381018518 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030140 | Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y | | RX J1940.1-1025 | 295.0445 | -10.4193 | 28.98688715 | -15.49869645 | 79.7405 | 54572.8979976852 | 54573.743275463 | 403027010 | 32453.6 | 30000 | 32453.6 | 32453.6 | 0 | 32453.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26465.7 | 26465.7 | 73021.9 | 2 | PROCESSED | 54587.0365740741 | 54953 | 54587.0481481482 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030140 | Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y | | IGR J17195-4100 | 259.8947 | -41.0152 | 346.97641748 | -2.13400756 | 97.0631 | 54880.4607175926 | 54881.3106481482 | 403028010 | 31645.6 | 30000 | 31645.6 | 31645.6 | 0 | 31645.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26917.8 | 26917.8 | 73428 | 0 | PROCESSED | 54962.3079166667 | 55330 | 54895.5494328704 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030140 | Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y | | XSS J12270-4859 | 187.002 | -48.8936 | 298.97017898 | 13.79783482 | 315.9792 | 54686.9674421296 | 54687.6480787037 | 403029010 | 29623.2 | 30000 | 29623.2 | 29623.2 | 0 | 29623.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34580 | 34580 | 58791.9 | 0 | PROCESSED | 54707.1640856482 | 55073 | 54707.1730208333 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030140 | Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y | | WR140 | 305.2159 | 43.8446 | 80.96257668 | 4.11237193 | 190.1825 | 54844.5415162037 | 54846.500162037 | 403030010 | 89406.8 | 80000 | 89406.8 | 89406.8 | 0 | 89406.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78055.7 | 78055.7 | 169196.9 | 1 | PROCESSED | 54959.633275463 | 55328 | 54861.8550115741 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030157 | WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 3 | AO3 | X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 | HXD | Y | | WR140 | 305.211 | 43.8318 | 80.94998516 | 4.10805919 | 199.7371 | 54835.3583449074 | 54836.4252199074 | 403031010 | 47266.4 | 40000 | 47266.4 | 47266.4 | 0 | 47282.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45303 | 45303 | 92161.8 | 0 | PROCESSED | 54959.4302662037 | 55328 | 54850.2164583333 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030157 | WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 3 | AO3 | X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 | HXD | Y | | WR140 | 305.1942 | 43.809 | 80.92425741 | 4.10518752 | 220.5408 | 54812.4360069444 | 54813.5523148148 | 403032010 | 52910.6 | 40000 | 52910.6 | 52910.6 | 0 | 52910.6 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 48260.9 | 48260.9 | 96431.8 | 0 | PROCESSED | 54826.234375 | 55192 | 54826.2481365741 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030157 | WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 3 | AO3 | X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 | HXD | Y | | WR140 | 305.1135 | 43.9272 | 80.98919394 | 4.21991141 | 90.2945 | 54565.231400463 | 54565.7224305556 | 403033010 | 21625.3 | 20000 | 21625.3 | 21625.3 | 0 | 21625.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18605.5 | 18605.5 | 42415.9 | 2 | PROCESSED | 54580.4079513889 | 54953 | 54580.4185648148 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030157 | WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 3 | AO3 | X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 | HXD | Y | | TAU SCO | 248.9714 | -28.2185 | 351.53328031 | 12.80600635 | 277.9748 | 54710.0436689815 | 54710.3697222222 | 403034010 | 14617.1 | 10000 | 14617.1 | 14617.1 | 0 | 14617.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12085.5 | 12085.5 | 28135.9 | 0 | PROCESSED | 54777.4117476852 | 55148 | 54780.4170138889 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y | | TAU SCO | 248.9731 | -28.2173 | 351.53521528 | 12.80565459 | 288.7028 | 54717.0750115741 | 54717.3752777778 | 403034020 | 14521.5 | 10000 | 14529.5 | 14521.5 | 0 | 14537.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9652.4 | 9652.4 | 25935.9 | 1 | PROCESSED | 54777.7685416667 | 55148 | 54780.6118171296 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y | | TAU SCO | 248.9736 | -28.2151 | 351.53721955 | 12.80675658 | 279.3712 | 54723.4207291667 | 54723.8119675926 | 403034030 | 12290.2 | 10000 | 12298.2 | 12298.2 | 0 | 12290.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11028.2 | 11028.2 | 33799.9 | 0 | PROCESSED | 54777.7390393518 | 55148 | 54780.4631597222 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y | | TAU SCO | 248.9733 | -28.218 | 351.53478934 | 12.80506422 | 280.0312 | 54729.4179398148 | 54729.7578009259 | 403034040 | 13971.1 | 10000 | 13971.1 | 13971.1 | 0 | 13971.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12891.2 | 12891.2 | 29350 | 0 | PROCESSED | 54777.8469328704 | 55148 | 54780.4954050926 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y | | TAU SCO | 248.9722 | -28.2177 | 351.53437371 | 12.80599439 | 271.5181 | 54696.3145833333 | 54696.6675810185 | 403034050 | 16313.6 | 10000 | 16350.4 | 16313.6 | 0 | 16358.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13967 | 13967 | 30472 | 0 | PROCESSED | 54713.1859606482 | 55084 | 54713.1924189815 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y | | TAU SCO | 248.9729 | -28.218 | 351.53455344 | 12.80533126 | 274.2608 | 54703.1981597222 | 54703.5447222222 | 403034060 | 15018.3 | 10000 | 15026.3 | 15034.3 | 0 | 15018.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12904.9 | 12904.9 | 29911.9 | 0 | PROCESSED | 54713.2685648148 | 55084 | 54713.2754976852 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y | | ETA CARINAE | 161.2297 | -59.7314 | 287.60304523 | -0.67930865 | 294 | 54627.0775 | 54627.649525463 | 403035010 | 35447.9 | 30000 | 35463.9 | 35447.9 | 0 | 35463.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27210.2 | 27210.2 | 49415.9 | 1 | PROCESSED | 54637.2593518518 | 55003 | 54637.2680092593 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 031124 | X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 3 | AO3 | X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM | HXD | Y | | ETA CARINAE | 161.2769 | -59.635 | 287.57915278 | -0.58292483 | 99.9027 | 54810.21125 | 54811.2084953704 | 403036010 | 48501.6 | 30000 | 48501.6 | 48501.6 | 0 | 48501.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42425.9 | 42425.9 | 86151.8 | 2 | PROCESSED | 54826.1197685185 | 55198 | 54828.3640972222 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 031124 | X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 3 | AO3 | X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM | HXD | Y | | ETA CARINAE | 161.3407 | -59.6518 | 287.61551185 | -0.58277566 | 142.0006 | 54856.1332291667 | 54856.6821064815 | 403037010 | 28805.3 | 30000 | 28805.3 | 28805.3 | 0 | 28805.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17453.9 | 17453.9 | 47407.9 | 0 | PROCESSED | 54961.978599537 | 55328 | 54880.533587963 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031124 | X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 3 | AO3 | X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM | HXD | Y | | ETA CARINAE | 161.3639 | -59.6742 | 287.63630523 | -0.59715454 | 170.6228 | 54877.528287037 | 54878.4119675926 | 403038010 | 35552.5 | 30000 | 35568.5 | 35552.5 | 0 | 35560.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31119.3 | 31119.3 | 76323.9 | 1 | PROCESSED | 54962.3153240741 | 55328 | 54893.4307407407 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031124 | X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 3 | AO3 | X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM | HXD | Y | | ASAS J002511+1217.2 | 6.2997 | 12.2847 | 112.91544003 | -50.07604687 | 234.9156 | 54841.6813773148 | 54842.5468055556 | 403039010 | 33256 | 30000 | 33256 | 33256 | 0 | 33256 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29873 | 29873 | 74752 | 1 | PROCESSED | 54959.7324884259 | 55328 | 54851.4143055556 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031144 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 3 | AO3 | BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3 | XIS | Y | | KT PER | 24.2933 | 50.9468 | 130.24865907 | -11.27406186 | 260.9001 | 54843.8957060185 | 54844.5334953704 | 403041010 | 29195.7 | 20000 | 29195.7 | 29195.7 | 0 | 29195.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28165.8 | 28165.8 | 55089.9 | 0 | PROCESSED | 54959.3597337963 | 55328 | 54854.0547916667 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031144 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 3 | AO3 | BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3 | XIS | Y | | SS73 17 | 152.7399 | -57.7545 | 282.81739372 | -1.29143094 | 80.1552 | 54775.6877430556 | 54776.3072453704 | 403043010 | 24907 | 20000 | 24907 | 24907 | 0 | 24907 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20809.1 | 20809.1 | 53519.9 | 0 | PROCESSED | 54791.5853935185 | 55157 | 54791.6362847222 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 031145 | SS73 17 was an innocuous Mira-type symbiotic star until INTEGRAL and Swift discovered its bright hard X-ray emission. Suzaku observations showed it emits three bright iron lines, with almost no emission in the 0.5-2 keV bandpass. The PI has an approved 100 ksec Chandra HETG observation in 2008 to determine the origin of the iron lines and measure any weak emission lines. With simultaneous Suzaku observations we will also measure the hard X-ray emission from the source, both to constrain the continuum and detect any non-thermal component. The effective areas of the XIS and HXD will constrain the broadband emission process much better than the HETG data. Combined with simultaneous optical observations of the Mira-type star we will determine the origin of this star's unusual emission. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 3 | AO3 | SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS OF THE SYMBIOTIC STAR SS73 17 | HXD | Y | | GX 301-2 | 186.5611 | -62.8021 | 300.05773343 | -0.07103063 | 326.712 | 54703.5522800926 | 54704.0036689815 | 403044010 | 11427.5 | 60000 | 11429.2 | 11430.6 | 0 | 11427.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10714.8 | 10714.8 | 38993.9 | 0 | PROCESSED | 54720.2543981482 | 55218 | 54720.435462963 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 031152 | We propose the first observation of the bright neutron star GX 301-2 with Suzaku. The aim of the proposed 60 ks observation is a study of the broadband spectrum of the source in unprecedented detail and quality. This will allow us to analyze the structure (including density and clumpiness) of the intense wind of the optical companion and the gas stream flowing from Wray 977 to the neutron star. Spectral data will be used to study the evolution of nH and the iron line with very high time resolution. Furthermore, we will perform phase resolved spectroscopy to study the spectral variation of the cyclotron line with pulse phase. | GALACTIC POINT SOURCES | 4 | A | ROTHSCHILD | RICHARD | NULL | NULL | USA | 3 | AO3 | BROAD-BAND STUDY OF GX 301-2 | HXD | Y | | GX 301-2 | 186.689 | -62.7212 | 300.10817936 | 0.01514837 | 109.0098 | 54836.4396296296 | 54838.0419328704 | 403044020 | 61813.6 | 50000 | 61813.6 | 61813.6 | 0 | 61813.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54992.2 | 54992.2 | 138398.1 | 2 | PROCESSED | 54959.4139814815 | 55328 | 54851.4303125 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031152 | We propose the first observation of the bright neutron star GX 301-2 with Suzaku. The aim of the proposed 60 ks observation is a study of the broadband spectrum of the source in unprecedented detail and quality. This will allow us to analyze the structure (including density and clumpiness) of the intense wind of the optical companion and the gas stream flowing from Wray 977 to the neutron star. Spectral data will be used to study the evolution of nH and the iron line with very high time resolution. Furthermore, we will perform phase resolved spectroscopy to study the spectral variation of the cyclotron line with pulse phase. | GALACTIC POINT SOURCES | 4 | A | ROTHSCHILD | RICHARD | NULL | NULL | USA | 3 | AO3 | BROAD-BAND STUDY OF GX 301-2 | HXD | Y | | VELA X-1 | 135.5377 | -40.5514 | 263.06039339 | 3.93722667 | 314.5441 | 54634.1981134259 | 54635.9043287037 | 403045010 | 104709.6 | 100000 | 104723.4 | 104709.6 | 0 | 104715.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96008.9 | 96008.9 | 147389.9 | 1 | PROCESSED | 54644.4374652778 | 55010 | 54644.4687847222 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 031153 | We propose to observe the well-known X-ray pulsar Vela X-1 (4U0900-40) using Suzaku in order to test models for the circumstellar environment by measuring teh spectrum and searching for variability in the iron line. The line is expected to exhibit changes in intensity and centroid energy as the X-ray beam sweeps around the wind an illuminates material with varying column density, ionization state, and vleocity. In addition we will study the variability in the cyclotron feature. We will compare our observations with detailed hydrodynamical simulations of the stellar wind and its interaction with the compact object. | GALACTIC POINT SOURCES | 4 | A | KALLMAN | TIMOTHY | NULL | NULL | USA | 3 | AO3 | SPECTROSCOPY OF VELA X-1 (4U0900-40) AND SEARCHES FOR PULSE PHASE VARIABILITY | XIS | Y | | CENTAURUS X-3 | 170.3244 | -60.5721 | 292.07802241 | 0.38603209 | 97.3521 | 54808.2886111111 | 54810.2085532407 | 403046010 | 97587.1 | 90000 | 97587.1 | 97587.1 | 0 | 97587.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79656.2 | 79656.2 | 165853.7 | 0 | PROCESSED | 54822.5966319444 | 55188 | 54822.6243634259 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 031154 | We ask for a 90 ks observation (which will be performed within typically 180 ks taking Suzaku's duty cycle into account) of the accreting HMXB Centaurus X-3 to conduct the most sensitive study to date of the wide range of changes of its broad band spectrum over one 2.1 binary orbit and with pulse phase. Especially we will determine the evolution of the hydrogen absorption column over the orbit and test whether signatures of the tidal wake observed with RXTE can be confirmed. The variable Fe line complex will be studied. The cyclotron resonance scattering feature of Cen X-3 at ~30 keV is especially well suited to test new physical models describing phase-resolved line profiles, since it is very variable over the pulse, with the line centroid spanning an energy range from 28 to 39 keV. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 3 | AO3 | THE BROAD BAND SPECTRUM OF CEN X-3 OVER ORBIT AND PULSE PHASE | HXD | Y | | 1A1118-61 | 170.3073 | -61.878 | 292.515895 | -0.84430143 | 131.7127 | 54846.5144328704 | 54847.9029976852 | 403049010 | 49667.4 | 45000 | 49667.4 | 49667.4 | 0 | 49667.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46815.9 | 46815.9 | 119953.8 | 0 | PROCESSED | 54959.5419560185 | 55328 | 54858.6603125 | 2.3.12.25 | 4 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031155 | We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku AO3. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line in this system and to determine its broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 3 | AO3-TOO | SEARCHING FOR CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y | | 1A1118-61 | 170.3215 | -61.8847 | 292.5244731 | -0.84831529 | 142.606 | 54859.2344328704 | 54859.8925810185 | 403050010 | 44212.5 | 45000 | 44212.5 | 44212.5 | 0 | 44212.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30915.4 | 30915.4 | 56859.9 | 0 | PROCESSED | 54962.0592708333 | 55328 | 54880.5326273148 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031155 | We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku AO3. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line in this system and to determine its broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 3 | AO3-TOO | SEARCHING FOR CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y | | CEN X-4 | 224.5893 | -31.6684 | 332.24097668 | 23.88258751 | 104.6233 | 54847.9102314815 | 54850.9717939815 | 403057010 | 146670.4 | 150000 | 146687.6 | 146670.4 | 0 | 146691.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 133618.5 | 133618.5 | 264453.9 | 2 | PROCESSED | 54959.9293518518 | 55328 | 54880.5460069444 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031161 | Observations of thermal emission from the surface of quiescent neutron star low-mass X-ray binaries (LMXBs) can be used to measure neutron star radii. However, their quiescent spectra are complicated due to the presence of an additional power-law, and because variability has been seen on timescales as short as 100s. The nearest known neutron star LMXB Cen X-4 gives us the clearest view of these objects. But, the best observation so far lacked the sensitivity to determine the cause of the variability. Yet, the cause has important ramifications for measuring neutron star radii - if it is the thermal (rather than power-law) component that is varying our picture of quiescent emission may be wrong. To solve this critical problem we propose a 150 ksec observation of Cen X-4 with Suzaku. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | USA | 3 | AO3 | UNCOVERING VARIABLE QUIESCENT EMISSION IN THE NEUTRON STAR CEN X-4 | XIS | Y | | GX 340+0 | 251.4463 | -45.6133 | 339.58535361 | -0.07953483 | 81.21 | 54892.2765740741 | 54894.8168287037 | 403060010 | 107312.7 | 100000 | 107314.5 | 107312.7 | 0 | 107314.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86104 | 86104 | 219446.7 | 1 | PROCESSED | 54963.2715162037 | 55329 | 54908.7293055556 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031164 | In this proposal we request to observe accreting neutron stars sources GX 340+0, GX 3+1 and GX 13+1. The observational goal of the observations is to collect high-spectral resolution data in the region of K$_alpha$ iron line. Our scientific motivation is to put the origin of the line emission under additional theoretical scrutiny. We wish to compare the performance of the wind-reprocessing model to relativistic model in as many sources as possible. This proposal is a part of our broader effort to investigate the origin of iron emission line in Galactic X-ray binaries, which includes a parallel proposal to observe WD binaries. | GALACTIC POINT SOURCES | 4 | B | SHAPOSHNIKOV | NIKOLAI | NULL | NULL | USA | 3 | AO3 | IRON KALPHA EMISSION LINE DIAGNOSTICS IN ACCRETING NEUTRON STARS | XIS | Y | | CYG X-2 | 326.1609 | 38.3293 | 87.3271497 | -11.30495752 | 51.1203 | 54648.0669097222 | 54650.6154398148 | 403063010 | 72430.8 | 100000 | 102692.2 | 72430.8 | 0 | 89814.4 | 1 | 1 | 0 | 2 | 1 | 0 | 0 | 88133.1 | 88133.1 | 220167.8 | 0 | PROCESSED | 54664.8983101852 | 55031 | 54665.3170601852 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 031165 | The nature of ultra-dense matter in neutron stars remains enigmatic. To probe this requires accurate neutron star radii and masses. We recently showed that broad iron lines in neutron star low-mass X-ray binaries (LMXBs) constrain the neutron star radius. LMXBs also provide us with another tool, kHz quasi-periodic oscillations (QPOs). Combining the inner disk velocity (from modeling the iron line) and the frequency of the kHz QPOs gives a method to measure the neutron star mass. We propose a 100 ks observation of Cyg X-2 with Suzaku to provide a detailed iron line profile. Combined with simultaneous observations with RXTE to determine the kHz QPO frequency, we will measure the neutron star mass. Cyg X-2 is the perfect test case as it already has a known mass from optical observations. | GALACTIC POINT SOURCES | 4 | B | CACKETT | EDWARD | NULL | NULL | USA | 3 | AO3 | MEASURING NEUTRON STAR MASSES USING BROAD IRON LINES AND KHZ QPOS | XIS | Y | | CYG X-1 | 299.5797 | 35.2714 | 71.39012673 | 3.11059703 | 84.4565 | 54574.6816898148 | 54575.4238425926 | 403065010 | 33943.5 | 30000 | 33943.5 | 33978.2 | 0 | 33970.3 | 1 | 1 | 0 | 2 | 1 | 0 | 0 | 28955.6 | 28955.6 | 64118 | 0 | PROCESSED | 54587.1935416667 | 54957 | 54587.2117476852 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 031172 | We request two 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku brings three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 100-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | A | NOWAK | MICHAEL | NULL | NULL | USA | 3 | AO3 | CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN IN THE SUZAKU ERA | HXD | Y | | GX 339-4 | 255.7095 | -48.7885 | 338.94163546 | -4.32765826 | 281.8009 | 54733.942650463 | 54736.0968055556 | 403067010 | 104994 | 100000 | 105018 | 104994 | 0 | 104994 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 114775.9 | 114775.9 | 186091.7 | 2 | PROCESSED | 54777.5706018518 | 55148 | 54780.5803935185 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 031174 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with our multi-wavelength, radio to X-ray, program, Suzaku observations can constrain theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 3 | AO3-TOO | CONSTRAINING MODELS FOR BLACK HOLE ACCRETION IN THE HARD STATE | XIS | Y | | XTE J1759-220 | 269.9393 | -22.0118 | 7.5831003 | 0.77858469 | 86.479 | 54566.5188773148 | 54567.6460532407 | 403072010 | 48961 | 50000 | 49361 | 49425 | 0 | 48961 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43912.9 | 43912.9 | 97363.9 | 1 | PROCESSED | 54580.4644328704 | 54953 | 54580.4766550926 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 032012 | Dipping low-mass X-ray binaries (LMXBs), a subclass of LMXBs that are viewed close to the disk plane, provide us with a rare opportunity to probe the structure of accretion disks. This was nicely illustrated with the discovery of Fe XXV and Fe XXVI absorption lines in all the dipping LMXBs observed with XMM and Chandra. It revealed the existence of a highly-ionized atmosphere above the disk which is likely present in any LMXB but only detectable in the ones seen close to edge-on. We propose to observe two recently discovered dipping binaries with Suzaku, to constrain the basic astrophysical properties (orbital period, distance, variability, high energy cutoff, etc) of these yet poorly observed sources, and to further investigate the ionized atmosphere in X-ray binaries in general. | GALACTIC POINT SOURCES | 4 | B | BOIRIN | LAURENCE | NULL | NULL | EUR | 3 | AO3 | NEW DIPPING X-RAY BINARIES TO PROBE ACCRETION DISKS AND THEIR IONIZED ATMOSPHER | XIS | Y | | V2129 OPH | 246.9149 | -24.3651 | 353.29078542 | 16.72506486 | 88.3342 | 54866.0202430556 | 54866.5821296296 | 403074010 | 21033.5 | 20000 | 21033.5 | 21033.5 | 0 | 21033.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16533.1 | 16533.1 | 48533.9 | 0 | PROCESSED | 54962.2439583333 | 55329 | 54880.5317708333 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 032022 | We propose to observe the classical T Tauri stars CS Cha, MN Lup, V2129 Oph and XZ Tau with the Suzaku XIS to investigate accretion induced X-ray emission in CTTS as evidenced by the presence of excess emission in the soft X-ray regime. Specifically we intend to utilize Suzaku's sensitivity, low background and the capability of the XIS to resolve the OVIII Ly-alpha line from the OVII triplet. XMM-Newton and Chandra grating spectra provide strong evidence for the presence of accretion induced X-ray emission in CTTS, however, due to low SNR and the presence of absorption an accretion scenario often cannot be probed within reasonable exposure times. With the proposed observations we want to investigate a sample of these CTTS showing additional exceptional properties. | GALACTIC POINT SOURCES | 4 | B | ROBRADE | JAN | NULL | NULL | EUR | 3 | AO3 | ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS | XIS | Y | | ESO 137-G034 | 248.7664 | -58.1298 | 329.07669192 | -7.11373135 | 296.1293 | 54744.462650463 | 54746.6745833333 | 403075010 | 92052.5 | 90000 | 92061.3 | 92058.7 | 0 | 92052.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83661.5 | 83661.5 | 191089.7 | 1 | PROCESSED | 54777.7021759259 | 55148 | 54780.6031828704 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 032025 | Suzaku observations of hard X-ray (> 15 keV) selected, bright AGN discovered by INTEGRAL and Swift have revealed several examples of previously unknown Compton Thick (NH > 1e24 cm-2) AGN in the nearby Universe. Their broad band X-ray spectra show a high degree of complexity and a wide range of the relative intensities of the various components (i.e. scattered/reflected fraction; iron line intensity, etc.). We propose a medium/deep Suzaku observation of a bright source detected by INTEGRAL above 15 keV and optically identified with a nearby Seyfert 2 galaxy. Besides the various soft X-ray components, the flat 2-10 keV spectrum and the strong (EW ~ 1 keV) iron line present in an archival XMM-Newton observation strongly suggest that the nucleus is obscured by Compton-Thick gas. | GALACTIC POINT SOURCES | 4 | B | GILLI | ROBERTO | NULL | NULL | EUR | 3 | AO3 | ANOTHER COMPTON-THICK AGN JUST AROUND THE CORNER | HXD | Y | | GK PER | 52.8202 | 43.8404 | 151.00566373 | -10.1477205 | 257.5144 | 54875.4415277778 | 54876.0899884259 | 403081010 | 30388.8 | 30000 | 30388.8 | 30388.8 | 0 | 30388.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27399.9 | 27399.9 | 55997.9 | 2 | PROCESSED | 54962.3273842593 | 55330 | 54893.4257407407 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 033107 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | C | YUASA | TAKAYUKI | HARRISON | THOMAS | JUS | 3 | AO3 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | | AE AQUARII | 310.0451 | -0.9346 | 45.22328928 | -24.45613885 | 265.1622 | 55120.7618518518 | 55124.2265393518 | 404001010 | 160454.6 | 160000 | 161451.9 | 161720.9 | 0 | 160454.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 136071.5 | 136071.5 | 299327.7 | 3 | PROCESSED | 55134.5131481482 | 55503 | 55134.5588194444 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040032 | As picked up in the NASA press release in 2008, one of the most important results with Suzaku in three years was the first discovery of a possible non-thermal pulsation from a white dwarf AE Aquarii. This job was performed by our group. "Can magnetized white dwarfs accelerate particles like neutron stars?" This is the basic question of this study as a long standing mystery of Cosmic-ray origin for near 100 years. To ensure our result with Suzaku, we triggered the guest observation of AE Aquarii in TeV gamma-ray band with the recent powerful telescope, H.E.S.S., in their first GO program on 2009. Here, we propose the simultaneous observation with Suzaku and H.E.S.S, to distinguish the acceleration site in and/or outer of the binary system using X-ray and TeV gamma-ray flux informations. | GALACTIC POINT SOURCES | 4 | A | TERADA | YUKIKATSU | NULL | NULL | JAP | 4 | AO4 | SUZAKU, H.E.S.S., OPTICAL SIMULTANEOUS OBSERVATION OF THE WHITE DWARF PULSAR, AE AQUARII | HXD | Y | | GS 1826-238 | 277.3735 | -23.8572 | 9.22092987 | -6.12003001 | 267.2862 | 55125.8488310185 | 55127.9502777778 | 404007010 | 102515.4 | 100000 | 102515.4 | 102531.4 | 0 | 102537.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87999.6 | 87999.6 | 181541.8 | 2 | PROCESSED | 55166.3593171296 | 55534 | 55166.4220833333 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040035 | We propose a 100 ksec Suzaku observation of the neutron star (NS) binary GS 1826-238. It is already known that there is a high energy cutoff at around 150 keV in the hard state of black hole candidates (BNCs). Additional non-thermal spectrum above 300 keV has sometimes been verified by gamma-ray observatories. Some NS binaries exhibit a 'hard state' which shows X-ray properties similar to those observed in hard state BHCs. Their cutoff energies (~50 keV) are systematically lower than those of BHCs, but firm detections of non-thermal emissions are not reported so far. This proposal is aimed at the first detection of the non-thermal hard tail from this source in the steady 'hard state', and verification of its possible jet origin via simultaneous radio, near-IR, and optical observations. | GALACTIC POINT SOURCES | 4 | B | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 4 | AO4 | SEARCH FOR A NON-THERMAL HARD TAIL FROM THE NEUTRON STAR BINARY GS 1826-238 | HXD | Y | | UX ARIETIS | 51.6466 | 28.6421 | 159.59610539 | -22.97107378 | 272.6966 | 55229.7116666667 | 55231.7321064815 | 404008010 | 87799.3 | 90000 | 87799.3 | 87799.3 | 0 | 87799.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79742.9 | 79742.9 | 174539.9 | 0 | PROCESSED | 55249.7969212963 | 55616 | 55249.830150463 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040036 | We propose a hard X-ray observation of RS CVn-type active binary UX Arietis. Detection of nonthermal hard X-ray radiation is essentially important to solve the generation mechanism of stellar flares. UX Ari has a high coronal activity with a high temperature of ~2keV, and large stellar flares were frequently observed in the radio, UV, and X-ray band. Therefore, UX Ari is very suitable for hard X-ray observation of stellar flares. Large X-ray flares were observed by BeppoSAX, ASCA and Ginga sattellite, and hard X-ray emission upto ~50keV is detected by BeppoSAX. If a flare is large such as the events of former X-ray observations, we can detect the nonthermal hard X-ray emssion by Suzaku HXD. | GALACTIC POINT SOURCES | 4 | C | ISHIKAWA | SHIN-NOSUKE | NULL | NULL | JAP | 4 | AO4 | STUDY ON GENERATION MECHANISM OF STELLAR FLARES BY HARD X-RAY OBSERVATION OF ACTIVE BINARY UX ARIETIS | HXD | Y | | RXJ0007.0+7302 | 1.8916 | 72.9843 | 119.68700382 | 10.38954096 | 241.7328 | 55204.6112847222 | 55207.0675231482 | 404011010 | 105373.9 | 100000 | 105373.9 | 105373.9 | 0 | 106971.4 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 58564.4 | 58564.4 | 212205.9 | 2 | PROCESSED | 55768.9294097222 | 55587 | 55768.9633333333 | 2.6.16.30 | 2 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 040054 | We propose to observe the gamma-ray pulsar and itswind nebula (PWN) in the supernova remnant CTA1 with SUZAKU. Observations in X-ray wavebands are crucial to study non-thermal processes of PWNe. Its flux and spectral shape provide us important information about the energy distribution of the accelerated particles and the strength of the magnetic field. Observations made by Suzaku-HXD will constrain the X-ray spectrum above 20keV from the PWN for the first time. The high spectral resolution of XIS will allow us to search for metal lines, which tell us circumstance of the emission region. In addition, we will probably able to detect X-ray pulsation, which has notbeen detected yet, using XIS timing mode. | GALACTIC POINT SOURCES | 4 | C | TAKATA | JUMPEI | NULL | NULL | JAP | 4 | AO4 | X-RAY OBSERVATIONS OF GAMMA-RAY PULSAR AND ITS WIND NEBULA IN CTA1 | HXD | N | | U SCO | 245.6288 | -17.8156 | 357.72079613 | 21.90901194 | 93.2747 | 55233.0102430556 | 55234.2918865741 | 404018010 | 46076.4 | 20000 | 46076.4 | 46076.4 | 0 | 46076.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37611.7 | 37611.7 | 110719.9 | 1 | PROCESSED | 55250.138912037 | 55617 | 55250.1559375 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040057 | We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each. | GALACTIC POINT SOURCES | 4 | A | TAKEI | DAI | NULL | NULL | JAP | 4 | AO4-TOO | TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION | HXD | Y | | U SCO | 245.629 | -17.8143 | 357.72199881 | 21.90970563 | 93.274 | 55236.514375 | 55237.1668865741 | 404018020 | 28936.9 | 20000 | 28936.9 | 28936.9 | 0 | 28936.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18328.8 | 18328.8 | 56369.9 | 0 | PROCESSED | 55251.137349537 | 55619 | 55251.1498611111 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040057 | We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each. | GALACTIC POINT SOURCES | 4 | A | TAKEI | DAI | NULL | NULL | JAP | 4 | AO4-TOO | TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION | HXD | Y | | U SCO | 245.6292 | -17.8133 | 357.72295453 | 21.91020567 | 93.2753 | 55239.299224537 | 55239.8259027778 | 404018030 | 26826 | 20000 | 26826 | 26826 | 0 | 26826 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24903.7 | 24903.7 | 45472 | 1 | PROCESSED | 55253.1048263889 | 55619 | 55253.1155671296 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040057 | We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each. | GALACTIC POINT SOURCES | 4 | A | TAKEI | DAI | NULL | NULL | JAP | 4 | AO4-TOO | TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION | HXD | Y | | EUVE J0317-85.5 | 48.9864 | -85.5003 | 299.84736337 | -30.72881529 | 65.46 | 55028.6017476852 | 55030.1460185185 | 404019010 | 63084.3 | 60000 | 63084.3 | 63084.3 | 0 | 63084.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56896.5 | 56896.5 | 133413.8 | 1 | PROCESSED | 55040.2354050926 | 55406 | 55040.2674305556 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040083 | Where is the particle acceleration site in the universe? The Cosmic-ray origin is the long standing mystery for near 100 years. The first discovery of "the white dwarf pulsar" in the AE Aquarii system with Suzaku is one of the most important step in this study, because Suzaku demonstrated the possibility of particle acceleration in white dwarfs. The next important step is to search for the sign of non-thermal emission from a NORMAL white dwarf. Here, we propose the Suzaku observation of an isolated white dwarf EUVE J0317-85.5, which has very high magnetic field strength of 450 MG and very fast rotation period 725 sec among this type of objects. | GALACTIC POINT SOURCES | 4 | B | HARAYAMA | ATSUSHI | NULL | NULL | JAP | 4 | AO4 | FIRST SEARCH FOR NON THERMAL EMISSION FROM AN ISOLATED MAGNETIZED WHITE DWARF | HXD | Y | | V603 AQL | 282.2246 | 0.5976 | 33.17431822 | 0.83751501 | 93.9529 | 55267.0156597222 | 55267.9773032407 | 404020010 | 34917.3 | 30000 | 34930.9 | 34917.3 | 0 | 34930.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30204.5 | 30204.5 | 83077.8 | 1 | PROCESSED | 55279.4289814815 | 55645 | 55279.4471296296 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040095 | The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 4 | AO4 | IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES | XIS | Y | | TT ARI | 31.7181 | 15.2972 | 148.52228749 | -43.79443 | 71.0668 | 55018.4424652778 | 55019.3023611111 | 404021010 | 35742.1 | 35000 | 35742.1 | 35779.6 | 0 | 35787.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31794 | 31794 | 74257.8 | 1 | PROCESSED | 55029.2174884259 | 55399 | 55029.236712963 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040095 | The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 4 | AO4 | IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES | XIS | Y | | Z CAM | 126.2993 | 73.0997 | 141.39550179 | 32.62975748 | 289.0998 | 54931.1187152778 | 54931.9092476852 | 404022010 | 37663 | 35000 | 37663 | 37663 | 0 | 37663 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36532.9 | 36532.9 | 68289.9 | 0 | PROCESSED | 54949.0999074074 | 55324 | 54949.4517824074 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040095 | The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 4 | AO4 | IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES | XIS | Y | | HESS J0632+057 | 98.2448 | 5.8057 | 205.66080027 | -1.43890266 | 289.9631 | 54941.5631944444 | 54944.1542708333 | 404027010 | 100034.3 | 100000 | 100034.3 | 100034.3 | 0 | 100034.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82391.8 | 82391.8 | 223841.9 | 6 | PROCESSED | 54966.4980092593 | 55336 | 54966.5323958333 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040102 | We propose a coordinate observation of HESS J0632+057 with Suzaku and VLA. This source is recently discovered as a fourth gamma-ray binary with HESS and XMM-Newton, and our results obtained in Suzaku AO-3 also confirmed a gradual variety of X-ray intensity, possibly associated with the binary period. With a combined observation with VLA, we will for the first time obtain a "real-time" variety from both of image and spectrum of this interesting source. | GALACTIC POINT SOURCES | 4 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 4 | AO4 | SIMULTANEOUS OBSERVATION OF HESS J0632+057 WITH SUZAKU AND VLA | XIS | Y | | BG CMI | 112.8488 | 9.8847 | 208.51997296 | 13.31865509 | 292.793 | 54932.5078703704 | 54933.5710532407 | 404029010 | 47079.1 | 40000 | 47087.1 | 47079.1 | 0 | 47087.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 45034.6 | 45034.6 | 91808 | 2 | PROCESSED | 54949.3252777778 | 55324 | 54949.5279050926 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040113 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | A | YUASA | TAKAYUKI | NULL | NULL | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | | PQ GEM | 117.7967 | 14.685 | 206.10344887 | 19.72488518 | 295.2889 | 54933.5737037037 | 54934.6329166667 | 404030010 | 46738.7 | 40000 | 46738.7 | 46738.7 | 0 | 46738.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43247.9 | 43247.9 | 91507.9 | 0 | PROCESSED | 54949.3663773148 | 55324 | 54949.5317939815 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040113 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | A | YUASA | TAKAYUKI | NULL | NULL | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | | TX COL | 85.7822 | -41.0648 | 246.79781267 | -29.77494364 | 322.4827 | 54963.6800578704 | 54965.2502199074 | 404031010 | 59781.8 | 40000 | 59789.8 | 59789.8 | 0 | 59781.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51123 | 51123 | 135654 | 0 | PROCESSED | 54978.1891666667 | 55345 | 54978.2105439815 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040113 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | A | YUASA | TAKAYUKI | NULL | NULL | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | | FO AQR | 334.4646 | -8.2931 | 53.06192299 | -49.11309098 | 76.4186 | 54987.3437152778 | 54988.5536921296 | 404032010 | 46084.6 | 40000 | 46084.6 | 46084.6 | 0 | 46084.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33499.3 | 33499.3 | 104529.9 | 0 | PROCESSED | 54998.3063310185 | 55366 | 54998.3271064815 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040113 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | A | YUASA | TAKAYUKI | NULL | NULL | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | | AO PSC | 343.7945 | -3.1271 | 68.69841137 | -53.28578539 | 60.9461 | 55004.4934143518 | 55005.3328587963 | 404033010 | 39654.4 | 40000 | 39654.4 | 39662.4 | 0 | 39662.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35683.4 | 35683.4 | 72517.9 | 0 | PROCESSED | 55018.1524768518 | 55385 | 55018.165474537 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040113 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | A | YUASA | TAKAYUKI | NULL | NULL | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | | HD6903 | 17.4507 | 19.662 | 128.84764567 | -42.9987034 | 70.0004 | 55031.3824305556 | 55032.3578703704 | 404034010 | 36813.5 | 35000 | 36829.5 | 36813.5 | 0 | 36821.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29672.7 | 29672.7 | 84263.9 | 0 | PROCESSED | 55048.2899305556 | 55419 | 55048.3029976852 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041201 | Suzaku XIS spectra of two G0 III Hertzsprung gap giants will complete a multi-observatory survey of the anomalous coronal behavior of this "X-ray deficient" class. The abrupt rise in coronal luminosities from the warmer giants to their cooler cousins, only slightly further advanced in evolution, might signal disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. Key discriminators are the coronal energy distribution, composition (FIP bias), and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution, and both have supporting HST UV spectra. Expanding the high energy sample of this key class of objects is essential for probing their contrary, but perhaps deeply significant, behavior. | GALACTIC POINT SOURCES | 4 | B | AYRES | THOMAS | NULL | NULL | USA | 4 | AO4 | ANOMALOUS CORONAE IN THE MIDST OF THE HERTZSPRUNG GAP | XIS | Y | | HD72779 | 128.8308 | 19.5933 | 205.51018209 | 31.33811175 | 104.3214 | 55141.3245949074 | 55142.9515277778 | 404035010 | 71033.5 | 70000 | 71033.5 | 71033.5 | 0 | 71033.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47461 | 47461 | 140555.9 | 0 | PROCESSED | 55166.1778819444 | 55532 | 55166.2074189815 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041201 | Suzaku XIS spectra of two G0 III Hertzsprung gap giants will complete a multi-observatory survey of the anomalous coronal behavior of this "X-ray deficient" class. The abrupt rise in coronal luminosities from the warmer giants to their cooler cousins, only slightly further advanced in evolution, might signal disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. Key discriminators are the coronal energy distribution, composition (FIP bias), and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution, and both have supporting HST UV spectra. Expanding the high energy sample of this key class of objects is essential for probing their contrary, but perhaps deeply significant, behavior. | GALACTIC POINT SOURCES | 4 | B | AYRES | THOMAS | NULL | NULL | USA | 4 | AO4 | ANOMALOUS CORONAE IN THE MIDST OF THE HERTZSPRUNG GAP | XIS | Y | | YY MEN | 74.6207 | -75.281 | 287.41045099 | -33.23069192 | 7.2587 | 54996.0772916667 | 54998.5606365741 | 404036010 | 106949.8 | 100000 | 106957.8 | 106957.8 | 0 | 106949.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 104090.2 | 104090.2 | 214539.8 | 0 | PROCESSED | 55008.271087963 | 55378 | 55008.2997106482 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041202 | The single K giant YY Men is one of the most active stars within 300 pc of the Sun, having produced 2 of the most powerful radio flares and 1 of the most powerful and long-duration optical flares ever detected. Its corona is one of the hottest and brightest known, with a *typical* X-ray luminosity of 32.0-32.5 (log erg/s) which most other cool stars only reach during major flares. We propose to obtain a 100-ksec observation of this hyperactive star to get a high S/N XIS exposure of its spectrum, particularly in the 5-10 keV region in which the XIS excels. We will study the He- and H-like Fe lines, search for 6.4 keV fluorescent emission, search for the presence of ultrahigh temperature and nonthermal spectral components, and look for correlations with simultaneous ATCA radio observations. | GALACTIC POINT SOURCES | 4 | B | DRAKE | STEPHEN | NULL | NULL | USA | 4 | AO4 | THE EXTREME CORONAL PROPERTIES OF THE HYPERACTIVE K GIANT YY MEN | XIS | Y | | V773 TAU | 63.5591 | 28.1916 | 168.22897578 | -16.34488481 | 264.3183 | 55255.9666550926 | 55258.750162037 | 404037010 | 115405.7 | 120000 | 115405.7 | 115405.7 | 0 | 115405.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95563 | 95563 | 240466.7 | 1 | PROCESSED | 55271.4577083333 | 55637 | 55271.499537037 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041203 | Young stars display magnetic activity at the extreme of that produced in nearby active stars and the Sun, making them useful tools to probe the dominant physical processes controlling such activity. The unique features of V773 Tau's X-ray and radio properties (frequent X-ray flaring of highly energetic flares, extreme nonthermal radio emission) mark it as one of the most active young stars. We seek coordinated Suzaku and mm wavelength observations to probe the interplay between the hot plasma and the stellar environment. We focus on utilizing the unique capabilities of Suzaku, namely the spectral resolution and sensitivity at 5--10 keV, to elucidate the properties of its hot plasma and its potential effects on the stellar environment such as detecting Fe fluorescence. | GALACTIC POINT SOURCES | 4 | C | OSTEN | RACHEL | NULL | NULL | USA | 4 | AO4 | X-RAY EMISSION AND THE STELLAR ENVIRONMENT AROUND THE PRE-MAIN SEQUENCE BINARY V773 TAU | XIS | Y | | ETA CARINAE | 161.2306 | -59.7313 | 287.60339978 | -0.67900846 | 291.9998 | 54992.8234143518 | 54994.2918865741 | 404038010 | 51225.9 | 45000 | 51225.9 | 51233.9 | 0 | 51233.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49118.6 | 49118.6 | 126839.8 | 0 | PROCESSED | 55006.223125 | 55378 | 55006.2447569444 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041204 | The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements. | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 4 | AO4 | HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CAR | HXD | Y | | ETA CARINAE | 161.2575 | -59.6351 | 287.57052339 | -0.58758586 | 87.8919 | 55156.1883449074 | 55157.3196643518 | 404039010 | 49388.7 | 45000 | 49388.7 | 49388.7 | 0 | 49388.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34255.3 | 34255.3 | 97720.1 | 0 | PROCESSED | 55176.3471412037 | 55542 | 55176.3651388889 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041204 | The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements. | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 4 | AO4 | HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CAR | HXD | Y | | SKY(270, +25) | 270.2558 | 25.1504 | 50.99920401 | 21.68976417 | 70.6538 | 55284.5620023148 | 55285.2994791667 | 404041010 | 1701.9 | 25000 | 1926.6 | 2094.4 | 0 | 1701.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 5621.1 | 5621.1 | 63713.9 | 1 | PROCESSED | 55369.1451273148 | 55284 | 55301.2652314815 | 2.5.16.28 | 2 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 041222 | Suzaku has recently revealed relativistically broadened Fe Kalpha emission lines in the spectra of neutron star low-mass X-ray binaries (LMXBs). We have now seen these lines in 10 neutron star LMXBs that we have examined, allowing measurements of the inner accretion disk radius, and hence an upper limit on the neutron star radius in all these objects. Only with the sensitivity of Suzaku, its high effective area in the Fe K band, and its broad bandpass has it been possible to robustly determine the shape of the lines. With a longer-term aim of completing a census of iron lines in neutron star LMXBs, we request a total of 200 ks to observe 5 neutron star low-mass X-ray binaries to study the relativistic broadening in the Fe Kalpha emission line profiles. | GALACTIC POINT SOURCES | 4 | C | CACKETT | EDWARD | NULL | NULL | USA | 4 | AO4 | AN FE KALPHA EMISSION LINE SURVEY OF NEUTRON STAR LMXBS | HXD | Y | | 4U 1608-52 | 243.1847 | -52.3651 | 330.96850701 | -0.81056533 | 96.6085 | 55266.077650463 | 55267.0072222222 | 404044010 | 34010.1 | 30000 | 34010.1 | 34010.1 | 0 | 34010.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30194 | 30194 | 80297.8 | 0 | PROCESSED | 55279.4317592593 | 55647 | 55279.4591666667 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041223 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | USA | 4 | AO4-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | HXD | Y | | 4U 1608-52 | 243.1805 | -52.3646 | 330.96698106 | -0.80844416 | 94.0316 | 55270.6937615741 | 55271.6668287037 | 404044020 | 32718.1 | 30000 | 32718.1 | 32726.1 | 0 | 32718.1 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 26988 | 26988 | 84055.8 | 1 | PROCESSED | 55285.1012268518 | 55651 | 55285.1175462963 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041223 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | USA | 4 | AO4-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | HXD | Y | | 4U 1608-52 | 243.2309 | -52.3757 | 330.98178647 | -0.83761569 | 125.7606 | 55273.9986689815 | 55274.9154166667 | 404044030 | 31756.8 | 30000 | 31756.8 | 31756.8 | 0 | 31756.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15309.4 | 15309.4 | 79193.8 | 0 | PROCESSED | 55286.243587963 | 55652 | 55286.259849537 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041223 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | USA | 4 | AO4-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | HXD | Y | | 4U 1608-52 | 243.1735 | -52.4241 | 330.92310685 | -0.84886634 | 127.9983 | 55277.989849537 | 55278.9140393518 | 404044040 | 16072.8 | 30000 | 16072.8 | 16072.8 | 0 | 16072.8 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 15655.7 | 15655.7 | 79843.9 | 2 | PROCESSED | 55298.7005902778 | 55665 | 55299.4128819444 | 2.5.16.28 | 2 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 041223 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | USA | 4 | AO4-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | HXD | Y | | A 0535+26 | 84.7195 | 26.3786 | 181.38803208 | -2.61609461 | 86.1856 | 55067.9626273148 | 55069.1599421296 | 404054010 | 51866.8 | 45000 | 51870.6 | 51870.6 | 0 | 51866.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42078 | 42078 | 103429.8 | 1 | PROCESSED | 55078.2009722222 | 55448 | 55078.219837963 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041232 | We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku's AO-4. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line(s) in this system and to constrain its broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 4 | AO4-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y | | A 0535+26 | 84.7291 | 26.2457 | 181.50526016 | -2.67952465 | 272.2555 | 55292.5024074074 | 55293.7029282407 | 404055010 | 3177.9 | 45000 | 3177.9 | 3460.4 | 0 | 3177.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34392.8 | 34392.8 | 103715.8 | 1 | PROCESSED | 55323.348287037 | 55689 | 55323.4435532407 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 041232 | We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku's AO-4. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line(s) in this system and to constrain its broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 4 | AO4-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y | | IGRJ16393-4643 | 249.7688 | -46.7009 | 338.00177501 | 0.07896045 | 111.6627 | 55267.9865740741 | 55269.4508564815 | 404056010 | 50540 | 50000 | 50564 | 50540 | 0 | 50564 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42256.5 | 42256.5 | 126467.8 | 1 | PROCESSED | 55279.4391898148 | 55647 | 55279.4686689815 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041234 | Stellar winds play a critical role in several as yet poorly understood astrophysical processes. One of the best laboratories for studying winds is in wind fed Supergiant High Mass X-ray binaries. Using the neutron star (NS) as a backlight, variable absorption in X-rays measures column density variations in the secondary star wind. A recent explosion in the number of known HMXBs has defined two additional subclasses of HMXBs, potentially related through geometry and wind properties: 1) heavily obscured sources and 2) so-called Supergiant Fast X-ray Transients (SFXTs). We propose observations of 2 obscured sgHMXBs and 2 SFXTs to monitor the column density. This will test wind models and probe whether these subclasses are related to one another and to classical HMXBs through wind parameters. | GALACTIC POINT SOURCES | 4 | C | MORRIS | DAVID | NULL | NULL | USA | 4 | AO4 | PROBING DONOR STAR WIND STRUCTURE IN HMXBS THROUGH VARIABLE ABSORPTION | XIS | Y | | GS 2023+338 | 306.0444 | 33.8015 | 73.0785131 | -2.14854563 | 252.4521 | 55142.9636805556 | 55144.0550810185 | 404059010 | 42324.6 | 40000 | 42348.6 | 42324.6 | 0 | 42356.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29140.4 | 29140.4 | 94283.9 | 1 | PROCESSED | 55155.0909837963 | 55531 | 55155.1065625 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041243 | The quiescent state is the dominant accretion mode for black holes on all mass scales. Our knowledge of the X-ray spectrum is limited due to the characteristic low luminosity in this state. Here, we propose a 40 ks observation of the most luminous quiescent stellar mass black hole GS 2023+338 (V404 Cyg). These observations will allow us to detect hard X-ray emission from a quiescent stellar mass black hole for the first time, providing unique contraints on the nature of the accretion flow in this low luminosity state. | GALACTIC POINT SOURCES | 4 | B | REYNOLDS | MARK | NULL | NULL | USA | 4 | AO4 | CONSTRAINING THE QUIESCENT ACCRETION FLOW AROUND A BLACK HOLE WITH SUZAKU | HXD | Y | | GRS 1758-258 | 270.2971 | -25.679 | 4.56169204 | -1.32563061 | 89.3817 | 55263.8983333333 | 55266.0711111111 | 404060010 | 82682.7 | 80000 | 82682.7 | 82682.7 | 0 | 82682.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71178.9 | 71178.9 | 187709.7 | 1 | PROCESSED | 55279.5119560185 | 55647 | 55279.5468402778 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041244 | We propose an 80 ks observation to obtain a broadband spectrum of the Galactic microquasar GRS 1758-258 while in the low-hard state with Suzaku. Here we aim to constrain the nature and geometry of the accretion flow via measurements of the various disc reflection features, which are detectable for the first time due to the unique capabilities of Suzaku. As this system is known to power large radio jets, its study will also aid our understanding of the conditions necessary for the formation of relativistic outflows and how these relate to the accretion geometry in the low-hard state. | GALACTIC POINT SOURCES | 4 | B | REYNOLDS | MARK | NULL | NULL | USA | 4 | AO4 | CONSTRAINING DISC REFLECTION IN THE MICROQUASAR GRS 1758-258 | HXD | Y | | LMC X-1 | 84.947 | -69.7479 | 280.20680376 | -31.50316575 | 10.0004 | 55033.776724537 | 55036.8953587963 | 404061010 | 129867.9 | 120000 | 129867.9 | 129867.9 | 0 | 129867.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132597.6 | 132597.6 | 269395.6 | 4 | PROCESSED | 55048.6041319444 | 55419 | 55048.6509143518 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041245 | We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability. | GALACTIC POINT SOURCES | 4 | A | MCCLINTOCK | JEFFREY | NULL | NULL | USA | 4 | AO4 | MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINE | XIS | Y | | LMC X-3 | 84.7128 | -64.0821 | 273.5746003 | -32.09166858 | 184.4521 | 55186.5265162037 | 55190.9105555556 | 404062010 | 154424.2 | 150000 | 154434 | 154434 | 0 | 154424.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 101172.1 | 101172.1 | 352145.8 | 2 | PROCESSED | 55218.635787037 | 55587 | 55218.7384375 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041245 | We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability. | GALACTIC POINT SOURCES | 4 | C | MCCLINTOCK | JEFFREY | NULL | NULL | USA | 4 | AO4 | MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINE | XIS | Y | | XTE J1710-281 | 257.5483 | -28.1282 | 356.35839186 | 6.92613447 | 86.2275 | 55278.9207638889 | 55281.1460300926 | 404068010 | 76138.5 | 75000 | 76138.5 | 76146.5 | 0 | 76146.5 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 23656.5 | 23656.5 | 192239.7 | 3 | PROCESSED | 55301.4782291667 | 55668 | 55301.5227662037 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 042003 | We propose to observe XTE J1710-281, a low-mass X-ray binary showing bursts, eclipses and dips. We want to determine the nature of the X-ray emission in this yet poorly-studied system and exploit the fact it is viewed close to edge-on to probe the structure of the disk and of the ionized plasma located above it. The broad-band coverage of Suzaku XIS and HXD will allow us to determine the overall shape of the ionizing continuum, which is a key parameter to infer the properties of the warm absorber whose narrow spectral signatures will be simultaneously detected thanks to the good spectral resolution of XIS near 6 keV. | GALACTIC POINT SOURCES | 4 | C | BOIRIN | LAURENCE | NULL | NULL | EUR | 4 | AO4 | SUZAKU TO INVESTIGATE A LOW-MASS X-RAY BINARY SHOWING BURSTS, ECLIPSES, AND DIPS | XIS | Y | | 4U 1820-30 | 275.9267 | -30.4234 | 2.73525617 | -7.94773658 | 265.1815 | 55083.1120023148 | 55083.2015740741 | 404069010 | 3517.5 | 20000 | 3525.5 | 3517.5 | 0 | 3525.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3712.4 | 3712.4 | 7738 | 0 | PROCESSED | 55109.0986574074 | 55475 | 55109.4203125 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y | | 4U 1820-30 | 275.9248 | -30.4209 | 2.73676025 | -7.94514519 | 265.9319 | 55088.3645833333 | 55088.8141087963 | 404069020 | 21037.3 | 20000 | 21037.3 | 21037.3 | 0 | 21037.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17170 | 17170 | 38831.9 | 0 | PROCESSED | 55099.5977199074 | 55469 | 55103.4457407407 | 2.4.12.26 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y | | 4U 1820-30 | 275.9316 | -30.4206 | 2.73970623 | -7.95024046 | 261.8755 | 55096.0447453704 | 55096.8335416667 | 404069030 | 29225.4 | 20000 | 29225.4 | 29225.4 | 0 | 29225.4 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 25940.5 | 25940.5 | 68148 | 1 | PROCESSED | 55110.3776736111 | 55477 | 55110.3989699074 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y | | 4U 1820-30 | 275.9314 | -30.4193 | 2.74079847 | -7.94949913 | 261.8762 | 55102.6696759259 | 55103.5002662037 | 404069040 | 28699.4 | 20000 | 28699.4 | 28699.4 | 0 | 28699.4 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 24926.1 | 24926.1 | 71751.9 | 2 | PROCESSED | 55133.2057291667 | 55499 | 55133.2273263889 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y | | 4U 1820-30 | 275.9251 | -30.4172 | 2.74021083 | -7.94370371 | 265.2009 | 55111.1096643518 | 55111.700162037 | 404069050 | 21767.4 | 20000 | 21767.4 | 21767.4 | 0 | 21767.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15674.3 | 15674.3 | 51003.9 | 0 | PROCESSED | 55127.2852777778 | 55496 | 55127.2938194445 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y | | 4U 1820-30 | 275.9218 | -30.4206 | 2.73584989 | -7.94270191 | 269.3964 | 55116.6321064815 | 55117.1759143518 | 404069060 | 24668.7 | 100000 | 0 | 24668.7 | 0 | 24668.7 | 0 | 1 | 0 | 2 | 1 | 0 | 0 | 16950.5 | 16950.5 | 46978 | 0 | PROCESSED | 55131.3551273148 | 55507 | 55131.3693518518 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y | | 4U 1820-30 | 275.9205 | -30.4212 | 2.7347979 | -7.94197311 | 270.4164 | 55124.2356134259 | 55124.7925810185 | 404069070 | 24056.6 | 100000 | 24056.7 | 24072.6 | 0 | 24056.6 | 3 | 1 | 0 | 2 | 1 | 0 | 0 | 18903.5 | 18903.5 | 48107.9 | 0 | PROCESSED | 55134.2286805556 | 55503 | 55134.2427314815 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y | | IGR J08408-4503 | 130.2449 | -45.0216 | 264.03123634 | -1.90203871 | 133.4432 | 55176.7452199074 | 55179.5002199074 | 404070010 | 92566 | 100000 | 92646 | 92566 | 0 | 92630 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69434.4 | 69434.4 | 237989.8 | 2 | PROCESSED | 55200.3555555556 | 55567 | 55200.3941550926 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 042007 | We propose a 100 ks Suzaku observation of a Supergiant Fast X-ray Transient (SFXT) displaying periodic outbursts, IGRJ08408-4503, with the main aim of searching for cyclotron lines in its spectrum.This would be the first direct measurement of the neutron star magnetic field in this recently discovered class of HMXBs, and would be crucial in discriminating between different models for the outburst mechanisms, involving highly magnetized neutron stars (1E14 G) versus more typical magnetic fields of 1E12 G.The source is a SFXT displaying recurrent outbursts on short timescales (flaring every about 11 and 24 days).Because in most SFXTs the outbursts are not predictable, fast and difficult to observe,the SFXT we are proposing is a key system to understand the physical properties of this class. | GALACTIC POINT SOURCES | 4 | C | SIDOLI | LARA | NULL | NULL | EUR | 4 | AO4 | SEARCH FOR CYCLOTRON LINES IN THE X-RAY SPECTRUM OF THE SUPERGIANT FAST X-RAY TRANSIENT IGRJ08408-4503 | HXD | Y | | GX 9+9 | 262.9404 | -16.8929 | 8.57505694 | 9.06920034 | 97.5329 | 55271.6738773148 | 55273.9918981482 | 404071010 | 85187.1 | 75000 | 85208.7 | 85203.1 | 0 | 85187.1 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 61694.2 | 61694.2 | 200263.9 | 0 | PROCESSED | 55285.3728125 | 55652 | 55285.4179513889 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 042011 | We propose two 75 ks Suzaku observations of the bright neutron star low mass X-ray binary (LMXB) GX9+9, spread over six months. We will investigate the presence of X-ray narrow absorption features in the Suzaku spectra, which are a signature of a disk wind. Such features, identified with ions such as Fe XXV and Fe XXVI, have been observed in a number of LMXBs and give us information about the mass outflow rate and the launching mechanism of the wind. We will study the connection of the disk wind to the presence of radio jet emission with simultaneous radio observations. Finally, we will determine if the broad Fe emission line indicated by the XMM-Newton spectrum is relativistically broadened. Variability will be studied as a function of accretion rate in the two proposed observations. | GALACTIC POINT SOURCES | 4 | B | DIAZ TRIGO | MARIA | NULL | NULL | EUR | 4 | AO4 | A STUDY OF THE DISK WIND-JET CONNECTION IN GX9+9 WITH MULTIWAVELENGTH OBSERVATIONS | HXD | Y | | CYGNUS X-1 | 299.5964 | 35.2723 | 71.39800953 | 3.09942804 | 95.8123 | 54924.0537384259 | 54924.5654282407 | 404075010 | 15309.1 | 300000 | 15309.1 | 15318.8 | 0 | 15310.8 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 15537.4 | 15537.4 | 44203.9 | 1 | PROCESSED | 54949.2372685185 | 54922 | 54949.4917824074 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.5895 | 35.2721 | 71.39489928 | 3.10413213 | 91.3103 | 54929.2562847222 | 54929.8224421296 | 404075020 | 21336.1 | 300000 | 21336.1 | 21336.1 | 0 | 21336.1 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 13125.8 | 13125.8 | 48914 | 0 | PROCESSED | 54949.2296180556 | 54922 | 54949.4903125 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.5891 | 35.272 | 71.39464341 | 3.10435878 | 91.3113 | 54935.7650462963 | 54936.1473958333 | 404075030 | 17108.8 | 300000 | 17108.8 | 17116.8 | 0 | 17108.8 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 12986 | 12986 | 33027.9 | 1 | PROCESSED | 54949.3379282407 | 54922 | 54949.5303240741 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.5791 | 35.2719 | 71.39029863 | 3.11127562 | 84.0536 | 54944.1674768518 | 54944.6252777778 | 404075040 | 18014 | 300000 | 18016.6 | 18014 | 0 | 18016.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16327.7 | 16327.7 | 39550 | 0 | PROCESSED | 54966.2993055556 | 54922 | 54966.3125 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.5814 | 35.2712 | 71.39067981 | 3.10930809 | 85.1433 | 54949.7099884259 | 54950.2175925926 | 404075050 | 20521.2 | 300000 | 20529.2 | 20535.4 | 0 | 20521.2 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 12401.3 | 12401.3 | 43845.9 | 0 | PROCESSED | 54976.1928819445 | 54922 | 54976.2030671296 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.5392 | 35.2589 | 71.36219421 | 3.13231837 | 55.3254 | 54957.7006828704 | 54958.1356365741 | 404075060 | 19434.5 | 300000 | 19434.5 | 19450.5 | 0 | 19434.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 15279.5 | 15279.5 | 37557.9 | 0 | PROCESSED | 54976.076875 | 54922 | 54976.0885300926 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.6653 | 35.165 | 71.33570459 | 2.99545336 | 212.8004 | 55182.0619328704 | 55182.5508564815 | 404075070 | 22101.9 | 300000 | 22101.9 | 22109.9 | 0 | 23664 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3460.7 | 3460.7 | 42236 | 0 | PROCESSED | 55200.2251967593 | 54922 | 55200.4490046296 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | N | | CYGNUS X-1 | 299.5434 | 35.2592 | 71.36423878 | 3.12954641 | 57.7977 | 54971.0242592593 | 54971.6043865741 | 404075080 | 21340.4 | 300000 | 21340.4 | 21348.4 | 0 | 21340.4 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 17495.4 | 17495.4 | 50119.9 | 1 | PROCESSED | 54991.970150463 | 54922 | 54992.6546875 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.5373 | 35.2573 | 71.3600172 | 3.13281014 | 53.4895 | 54976.3582060185 | 54976.8259722222 | 404075090 | 20925.2 | 300000 | 20925.2 | 20933.2 | 0 | 20925.2 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 16116.4 | 16116.4 | 40412 | 1 | PROCESSED | 54992.0771527778 | 54922 | 54992.6651736111 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.5337 | 35.2545 | 71.35609035 | 3.13386262 | 50.0944 | 54980.4956712963 | 54981.0586226852 | 404075100 | 28784.5 | 300000 | 28784.5 | 28784.5 | 0 | 28784.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 25738.9 | 25738.9 | 48631.9 | 1 | PROCESSED | 54994.3722569445 | 54922 | 54994.3872800926 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.5294 | 35.2515 | 71.35169447 | 3.13529932 | 46.7675 | 54984.481400463 | 54984.9870833333 | 404075110 | 17450.2 | 300000 | 19037 | 17778.2 | 0 | 17450.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15040.9 | 15040.9 | 43687.9 | 1 | PROCESSED | 54994.3906134259 | 54922 | 54994.4091087963 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.5272 | 35.2497 | 71.34921869 | 3.1358965 | 44.7834 | 54986.8208333333 | 54987.3356944444 | 404075120 | 16873.3 | 300000 | 16881.3 | 16889.4 | 0 | 16873.3 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 6764.7 | 6764.7 | 44477.9 | 1 | PROCESSED | 55000.9993171296 | 54922 | 55001.0163078704 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.6021 | 35.1308 | 71.27949874 | 3.02171591 | 263.2299 | 55125.3772106482 | 55125.8404398148 | 404075130 | 20498.5 | 300000 | 20498.5 | 20506.5 | 0 | 20498.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 15163 | 15163 | 40015.9 | 0 | PROCESSED | 55134.2590509259 | 54922 | 55134.2701967593 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.6086 | 35.1319 | 71.28321336 | 3.01775246 | 259.2069 | 55130.2652314815 | 55130.7481365741 | 404075140 | 23104.2 | 300000 | 23104.2 | 23128.2 | 0 | 23120.2 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 20011 | 20011 | 41716 | 0 | PROCESSED | 55141.3428935185 | 54922 | 55141.3539467593 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.6206 | 35.1339 | 71.29004535 | 3.01042005 | 252.1788 | 55138.8946180556 | 55139.4106365741 | 404075150 | 22616.8 | 300000 | 22616.8 | 22624.8 | 0 | 22616.8 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 14061 | 14061 | 44575.9 | 1 | PROCESSED | 55149.4078703704 | 54922 | 55149.4202199074 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.6277 | 35.1371 | 71.29581116 | 3.00713364 | 246.5433 | 55145.8193981482 | 55146.4377199074 | 404075160 | 26022.2 | 300000 | 26022.2 | 26038.2 | 0 | 26026.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 18250.5 | 18250.5 | 53416 | 0 | PROCESSED | 55176.1865046296 | 54922 | 55176.2027430556 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.6355 | 35.1397 | 71.30136328 | 3.00304649 | 241.2259 | 55152.2855092593 | 55152.9418287037 | 404075170 | 23448.5 | 300000 | 23448.5 | 23888.5 | 0 | 23880.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 18707.1 | 18707.1 | 56691.8 | 3 | PROCESSED | 55162.1854282407 | 54922 | 55162.2019212963 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.6354 | 35.1397 | 71.30132058 | 3.00311627 | 241.1557 | 55159.514224537 | 55160.1328587963 | 404075180 | 21768.5 | 300000 | 21768.5 | 22480.5 | 0 | 22472.5 | 5 | 2 | 0 | 3 | 1 | 0 | 0 | 11406.4 | 11406.4 | 53435.8 | 0 | PROCESSED | 55176.2779976852 | 54922 | 55176.294849537 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.6537 | 35.1518 | 71.31947353 | 2.99665901 | 225.8159 | 55166.2922453704 | 55166.8904398148 | 404075190 | 22415.5 | 300000 | 22415.5 | 22431.5 | 0 | 22423.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 13157.8 | 13157.8 | 51673.9 | 0 | PROCESSED | 55181.275150463 | 54922 | 55181.288912037 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y | | CYGNUS X-1 | 299.6549 | 35.1555 | 71.32314713 | 2.99775182 | 222.7295 | 55173.647349537 | 55174.1043287037 | 404075200 | 20016.6 | 300000 | 20016.6 | 21752.6 | 0 | 21859.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17442.6 | 17442.6 | 39471.9 | 0 | PROCESSED | 55189.2589814815 | 54922 | 55189.2752430556 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | N | | 1E 2259+586 | 345.2716 | 58.9493 | 109.11022544 | -0.92895504 | 86.3239 | 54976.8335300926 | 54978.6446064815 | 404076010 | 122579.1 | 120000 | 122580.9 | 122580.9 | 0 | 122579.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103446.2 | 103446.2 | 156463.8 | 1 | PROCESSED | 54992.1777546296 | 54922 | 54992.6935069444 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 046002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 4 | AO4 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y | | SGR 1900+14 | 286.7986 | 9.3873 | 43.07377535 | 0.80526184 | 82.6704 | 54947.7664814815 | 54949.0807175926 | 404077010 | 53137.4 | 50000 | 53393.4 | 53393.4 | 0 | 53137.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42101.1 | 42101.1 | 113547.9 | 1 | PROCESSED | 54973.2438078704 | 54922 | 54973.4547222222 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 046002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 4 | AO4 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y | | SGR 0501+4516 | 75.2795 | 45.3414 | 161.49568149 | 1.98976538 | 93.3341 | 55060.8485069445 | 55061.8348842593 | 404078010 | 42675.3 | 40000 | 42675.3 | 42955.3 | 0 | 42891.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27487.8 | 27487.8 | 85185.8 | 0 | PROCESSED | 55071.2445138889 | 54922 | 55071.2594328704 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 046002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 4 | AO4 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y | | 4U0142+61 | 26.5176 | 61.8112 | 129.33625727 | -0.37933599 | 61.041 | 55055.0703125 | 55057.3654976852 | 404079010 | 107412.9 | 100000 | 107412.9 | 107420.9 | 0 | 107422.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99757.6 | 99757.6 | 198283.8 | 2 | PROCESSED | 55068.2751157407 | 54922 | 55068.3037268518 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 046002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 4 | AO4 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y | | 1RXS J1708-4009 | 257.2032 | -40.2034 | 346.44001394 | -0.00188973 | 266.4021 | 55066.6841203704 | 55067.9466898148 | 404080010 | 60886.9 | 60000 | 60886.9 | 60894.9 | 0 | 60904.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 51531.3 | 51531.3 | 109075.8 | 1 | PROCESSED | 55078.1617476852 | 54922 | 55078.1751851852 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 046002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 4 | AO4 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y | | PSR J1846-0258 | 281.5972 | -2.9106 | 29.7662115 | -0.20474108 | 86.0001 | 54936.8175578704 | 54939.6779398148 | 404081010 | 104345.1 | 100000 | 104345.1 | 104367.5 | 0 | 104353.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76006.5 | 76006.5 | 247101.8 | 1 | PROCESSED | 54959.4243981482 | 54922 | 54959.5006018518 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 046002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 4 | AO4 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y | | CYG X-1 | 299.59033 | 35.20161 | 71.33499876 | 3.06682766 | -99 | NULL | NULL | 405001010 | -99 | 120000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 050020 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM or MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 5 | AO5-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | XTE J1550-564 | 237.74458 | -56.47667 | 325.88223339 | -1.82706287 | -99 | NULL | NULL | 405002010 | -99 | 120000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 050020 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM or MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 5 | AO5-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | GRO J1655-40 | 253.5 | -39.84581 | 344.98161118 | 2.45630442 | -99 | NULL | NULL | 405003010 | -99 | 120000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 050020 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM or MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 5 | AO5-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | X1630-472 | 248.50458 | -47.39289 | 336.91037296 | 0.25136454 | -99 | NULL | NULL | 405004010 | -99 | 120000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 050020 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM or MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 5 | AO5-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | H1743-322 | 266.25833 | -32.22667 | 357.12592965 | -1.60785557 | -99 | NULL | NULL | 405005010 | -99 | 120000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 050020 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM or MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 5 | AO5-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | IGR J16167-4957 | 244.155 | -49.97986 | 333.05429094 | 0.49667919 | -99 | NULL | NULL | 405006010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 050025 | The all-sky survey in hard X-rays with INTEGRAL has been finding new magnetic Cataclysmic Variables. Among them, we propose Suzaku observations of five Intermediate Polars (IPs) which have no detailed follow-up spectroscopy in the hard X-ray band up to now. The wide-band energy coverage of Suzaku, therefore, is definitely useful to extract physical information from their spectra since, generally, the vFv spectrum of an IP peaks at E=20-50 keV and strong intrinsic absorption (nH=1E22-23 cm-2). By fitting the spectrum with our numerical model, we estimate a plasma temperature and an Fe abundance, and furthermore, a white dwarf mass which is one of the most basic and important parameter of a binary system. | GALACTIC POINT SOURCES | 4 | C | YUASA | TAKAYUKI | NULL | NULL | JAP | 5 | AO5 | ESTIMATE MASSES OF NEWLY-FOUND MAGNETIC WHITE DWARFS BASED ON HARD X-RAY CONTINUUM AND FE EMISSION LINES | XIS | Y | | IGR J15094-6649 | 227.3484 | -66.8278 | 315.91945149 | -7.50109233 | 90.4626 | 55588.7031365741 | 55589.5557638889 | 405007010 | 49461.2 | 50000 | 49483.2 | 49475.2 | 0 | 49461.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48018.5 | 48018.5 | 73659.9 | 0 | PROCESSED | 55621.2159490741 | 55990 | 55621.2282291667 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050025 | The all-sky survey in hard X-rays with INTEGRAL has been finding new magnetic Cataclysmic Variables. Among them, we propose Suzaku observations of five Intermediate Polars (IPs) which have no detailed follow-up spectroscopy in the hard X-ray band up to now. The wide-band energy coverage of Suzaku, therefore, is definitely useful to extract physical information from their spectra since, generally, the vFv spectrum of an IP peaks at E=20-50 keV and strong intrinsic absorption (nH=1E22-23 cm-2). By fitting the spectrum with our numerical model, we estimate a plasma temperature and an Fe abundance, and furthermore, a white dwarf mass which is one of the most basic and important parameter of a binary system. | GALACTIC POINT SOURCES | 4 | C | YUASA | TAKAYUKI | NULL | NULL | JAP | 5 | AO5 | ESTIMATE MASSES OF NEWLY-FOUND MAGNETIC WHITE DWARFS BASED ON HARD X-RAY CONTINUUM AND FE EMISSION LINES | XIS | Y | | V773TAU | 63.5571 | 28.1952 | 168.22500409 | -16.34364304 | 260.6557 | 55610.1581712963 | 55611.9815277778 | 405011010 | 82246.3 | 80000 | 82254.3 | 82246.3 | 0 | 82254.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72828.7 | 72828.7 | 157525.8 | 2 | PROCESSED | 55621.2758680556 | 55990 | 55621.2978703704 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050033 | We propose a Suzaku observation of the pre-main sequence binary system V773 Tau with the high sensitivity of HXD. The empirical Lx-Lr relation (Benz-G"udel relation) and radio flux variation predict that this source can have a flare with a peak luminosity Lx=10^34 ergs s-1, seven orders of magnitude larger than that of the Sun, when it is just before the periastron passage. We will observe this target simultaneously with radio band using VLBI network. Our goal is (1) to test whether the gigantic flare is still on the empirical relation (2) to detect inpulsive non-thermal emission at the most powerful stellar flare (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band. | GALACTIC POINT SOURCES | 4 | B | TSUBOI | YOHKO | NULL | NULL | JAP | 5 | AO5 | NON-THERMAL EMISSION AT THE MOST POWERFUL STELLAR FLARE | XIS | Y | | PSR J1429-5911 | 217.5051 | -59.1899 | 315.26780851 | 1.30018252 | 101.124 | 55588.2265625 | 55588.7001157407 | 405012010 | 30382.4 | 30000 | 30390.4 | 30398.4 | 0 | 30382.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 28792.3 | 28792.3 | 40903.9 | 0 | PROCESSED | 55602.1319328704 | 55968 | 55602.1404513889 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050047 | Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC POINT SOURCES | 4 | C | KAWAI | NOBUYUKI | NULL | NULL | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | PSR J1044-5737 | 161.1338 | -57.616 | 286.57019106 | 1.16750605 | 109.1973 | 55542.2984259259 | 55542.7292939815 | 405013010 | 22630 | 30000 | 22630 | 22630 | 0 | 22635.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21960.3 | 21960.3 | 37200 | 0 | PROCESSED | 55550.9573726852 | 55917 | 55550.9648148148 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050047 | Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC POINT SOURCES | 4 | C | KAWAI | NOBUYUKI | NULL | NULL | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | PSR J0614-33 | 93.5386 | -33.5015 | 240.50300829 | -21.83180137 | 119.1484 | 55498.9719675926 | 55499.6140740741 | 405014010 | 31210.9 | 30000 | 31210.9 | 31210.9 | 0 | 31210.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27331.4 | 27331.4 | 55449.9 | 0 | PROCESSED | 55509.025625 | 55875 | 55509.0359722222 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050047 | Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC POINT SOURCES | 4 | C | KAWAI | NOBUYUKI | NULL | NULL | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | PSR J2055+2539 | 313.957 | 25.6505 | 70.67687842 | -12.53222207 | 262.3229 | 55498.1479398148 | 55498.9578356482 | 405015010 | 31106.9 | 30000 | 31106.9 | 31106.9 | 0 | 31106.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21458.1 | 21458.1 | 69967.9 | 0 | PROCESSED | 55523.9823611111 | 55890 | 55523.9927314815 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050047 | Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC POINT SOURCES | 4 | C | KAWAI | NOBUYUKI | NULL | NULL | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | PSR J1957+5036 | 299.4354 | 50.5474 | 84.58480161 | 10.99652902 | 216.5649 | 55543.4586689815 | 55544.0842939815 | 405016010 | 32469 | 30000 | 32485 | 32469 | 0 | 32485 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25313.9 | 25313.9 | 54033.9 | 2 | PROCESSED | 55592.9227893518 | 55959 | 55592.9341782407 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050047 | Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC POINT SOURCES | 4 | C | KAWAI | NOBUYUKI | NULL | NULL | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | LS5039 | 276.56263 | -14.84822 | 16.88169314 | -1.28903495 | -99 | NULL | NULL | 405019010 | -99 | 80000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 050049 | LS5039 belongs to a newly established category, gamma-ray binary. LS5039 shows striking orbital modulation in the photon index and the flux at TeV energies. We discovered that the X-ray emission is non-thermal due to Synchrotron emission. LS5039 is the first object that shows non-thermal X-ray emission modulated with the orbital period. We also discovered that the shape of the light curve resembles that of TeV gamma-ray. By using the archival data, we found that even fine structures in the light curve seems to repeat every orbit of the system. We propose to observe the source for 80 ks to confirm whether LS5039 shows exactly same non-thermal features in different orbits. | GALACTIC POINT SOURCES | 4 | C | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 5 | AO5 | STUDY OF ORBITAL MODULATION OF GAMMA-RAY BINARY LS5039 | HXD | N | | V4641 SGR | 274.84013 | -25.40717 | 6.77395378 | -4.7890572 | -99 | NULL | NULL | 405020010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 050058 | We propose a 100 ksec Suzaku observation of the Galactic microquasar V4641 Sgr in an outburst. V4641 Sgr has many unique charactersitics:1)giant X-ray outbursts with fast rise and decay times, 2)violent variability in X-ray and optical bands, and 3)remarkable iron-K disk-line profiles in the X-ray spectrum. However, it is hardly understood due to the poor X-ray coverage which results from its short outburst duration and rapid intensity variations. Hence, we collaborate closely with VSNET, RXTE/ASM and Swift/BAT team for a rapid trigger. The moderate energy resolution and wideband energy coverage of Suzaku enable us to clarify the radiation mechanisms of V4641 Sgr. This observation is now planed simultaneously with RXTE, Fermi, AGILE and many radio and optical/NIR observatories. | GALACTIC POINT SOURCES | 4 | A | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 5 | AO5-TOO | THE LARGEST-EVER CAMPAIGN OF THE GALACTIC MICROQUASAR V4641 SGR | HXD | N | | V2487 OPH | 262.9946 | -19.3061 | 6.53905762 | 7.73892052 | 274.1277 | 55478.2880439815 | 55479.5827893518 | 405021010 | 56307.6 | 50000 | 56315.6 | 56307.6 | 0 | 56323.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51358 | 51358 | 111832 | 2 | PROCESSED | 55488.1606018518 | 55854 | 55488.179224537 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050059 | Suzaku discovery of the first white dwarf pulsar, AE Aqr (Terada et.al 2008) had a great impact on the studies of the cosmic-ray origin, since white dwarfs were not recognized as a particle accelerator. The next step is to check whether this phenomenon is common or not. In order to search for the second white dwarf pulsar, we picked up hard objects among the INTEGRAL and Swift sample, and propose the Suzaku observation of the best two objects, V2487 Oph and IGRJ00234+6141. | GALACTIC POINT SOURCES | 4 | A | TERADA | YUKIKATSU | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR NON-THERMAL EMISSION FROM HARD WHITE DWARFS WITH SUZAKU | HXD | Y | | IGR J00234+6141 | 5.7092 | 61.7549 | 119.55446517 | -0.92914674 | 80.286 | 55372.004375 | 55373.2397569445 | 405022010 | 81880 | 80000 | 81880 | 81880 | 0 | 81880 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70036.4 | 70036.4 | 106697.9 | 1 | PROCESSED | 55414.1609375 | 55780 | 55414.1791666667 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050059 | Suzaku discovery of the first white dwarf pulsar, AE Aqr (Terada et.al 2008) had a great impact on the studies of the cosmic-ray origin, since white dwarfs were not recognized as a particle accelerator. The next step is to check whether this phenomenon is common or not. In order to search for the second white dwarf pulsar, we picked up hard objects among the INTEGRAL and Swift sample, and propose the Suzaku observation of the best two objects, V2487 Oph and IGRJ00234+6141. | GALACTIC POINT SOURCES | 4 | A | TERADA | YUKIKATSU | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR NON-THERMAL EMISSION FROM HARD WHITE DWARFS WITH SUZAKU | HXD | Y | | W43 | 281.9 | -1.94264 | 30.76557057 | -0.03224669 | -99 | NULL | NULL | 405023010 | -99 | 90000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 050082 | We propose to observe a young stellar cluster W43 with Suzaku. This program aims to examine the possibility of new particle acceleration mechanism by powerful stellar wind. The immediate goals of this program are two-fold: (1) to detect super hard X-rays for the first time, and (2) to compare non-thermal X-ray luminosity with VHE gamma-ray luminosity. | GALACTIC POINT SOURCES | 4 | C | SUGAWARA | YASUHARU | NULL | NULL | JAP | 5 | AO5 | THE FIRST DETECTION OF SUPERHARD X-RAYS FROM YOUNG STELLAR CLUSTER W43 | HXD | N | | 1E 1547.0-5408 | 237.7284 | -54.3676 | 327.20000551 | -0.18012949 | 271.1663 | 55415.1611921296 | 55415.9633796296 | 405024010 | 51672.8 | 50000 | 51672.8 | 51792.8 | 0 | 52152.9 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 42781.2 | 42781.2 | 69299.9 | 0 | PROCESSED | 55427.2331828704 | 55793 | 55427.247025463 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050099 | Recently, hard X-ray tails have been detected by INTEGRAL at least up to 150 keV from ~5 magnetars. Suzaku has observed some magnetars during Key Project (AO-4) and ToO observations. As a result, soft X-ray emissions and hard X-ray tails have been detected from ~10 magnetars. This peculiar spectrum is seem to be common in all the magnetars, and we discovered the spectral evolution of magnetars. The remaining problem is to study the spectral difference between the active and quiescent states. Transient magnetar 1E 1547.0-540 was observed with Suzaku in 2009 January, and the extremely hard X-ray tail was detected up to 110 keV with photon index of 1.5, and it is appropriate to study the spectral change. Thus, we propose the observation of 1E 1547.0-5408 with 50 ks. | GALACTIC POINT SOURCES | 4 | B | NISHIOKA | HIROYUKI | NULL | NULL | JAP | 5 | AO5 | OBSERVATION OF THE HARD X-RAY TAIL AND SOFT X-RAY EMISSION OF AXP 1E 1547.0-5408 IN QUIESCENT STATE | HXD | N | | EMS0918 | 211.2948 | -61.3938 | 311.64055354 | 0.22486043 | 106.822 | 55589.5588310185 | 55590.0834837963 | 405025010 | 24542.5 | 20000 | 24550.5 | 24542.5 | 0 | 24558.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23281.1 | 23281.1 | 45309.9 | 1 | PROCESSED | 55602.1924652778 | 55972 | 55602.2015046296 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050104 | Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. | GALACTIC POINT SOURCES | 4 | A | TANAKA | YASUYUKI | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | | EMS1150 | 263.083 | -32.7212 | 355.27740066 | 0.39306698 | 91.2452 | 55611.9964930556 | 55612.6968055556 | 405026010 | 20918.6 | 20000 | 20918.6 | 20918.6 | 0 | 20918.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17263.9 | 17263.9 | 60503.9 | 0 | PROCESSED | 55621.1311921296 | 55988 | 55621.1440740741 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050104 | Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. | GALACTIC POINT SOURCES | 4 | A | TANAKA | YASUYUKI | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | | EMS01095 | 252.3381 | -45.0256 | 340.43907916 | -0.17827348 | 87.5534 | 55603.1544328704 | 55603.7613310185 | 405027010 | 20933.2 | 20000 | 20934.4 | 20934.4 | 0 | 20933.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16976.2 | 16976.2 | 52431.9 | 0 | PROCESSED | 55616.9640972222 | 55983 | 55617.4127430556 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050104 | Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. | GALACTIC POINT SOURCES | 4 | A | TANAKA | YASUYUKI | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | | EMS1308 | 293.0393 | 19.2567 | 54.62289289 | 0.10827332 | 90.0001 | 55313.4365740741 | 55313.9766203704 | 405028010 | 23898.7 | 20000 | 23906.7 | 23906.7 | 0 | 23898.7 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 23209 | 23209 | 46652 | 1 | PROCESSED | 55327.1675231482 | 55693 | 55327.1789930556 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050104 | Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. | GALACTIC POINT SOURCES | 4 | A | TANAKA | YASUYUKI | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | | V1280 SCO | 254.4172 | -32.3368 | 351.33470039 | 6.5596985 | 97.7451 | 55605.3662615741 | 55608.0501851852 | 405029010 | 99683 | 100000 | 99699 | 99683 | 0 | 99699 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86930.6 | 86930.6 | 231873.9 | 2 | PROCESSED | 55617.0939814815 | 55983 | 55617.4142361111 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050110 | We propose a 100 ks observation of the C-rich classical nova V1280 Sco. Using Suzaku's excellent spectral performance in the soft X-ray energy band, we aim to detect and to resolve emission lines from C, N, and O. | GALACTIC POINT SOURCES | 4 | A | TAKEI | DAI | NULL | NULL | JAP | 5 | AO5 | X-RAY SPECTROSCOPY OF THE C-RICH CLASSICAL NOVA V1280 SCO | XIS | Y | | HD125599 | 215.4515 | -48.0762 | 318.15137849 | 12.10713587 | 289.1653 | 55414.6760069444 | 55415.1571990741 | 405030010 | 31048 | 30000 | 31056 | 31056 | 0 | 31048 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24859.9 | 24859.9 | 41567.9 | 0 | PROCESSED | 55427.163912037 | 55793 | 55427.1753819444 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050116 | Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 5 | AO5 | QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION | XIS | Y | | HD130693 | 222.5749 | -24.4173 | 334.71293898 | 31.01917553 | 104.6337 | 55580.6525925926 | 55581.2384375 | 405031010 | 21314.5 | 20000 | 21314.5 | 21314.5 | 0 | 21314.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17462.5 | 17462.5 | 50605.9 | 2 | PROCESSED | 55598.9706134259 | 55965 | 55598.9831597222 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050116 | Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 5 | AO5 | QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION | XIS | Y | | XSS J16537-1905 | 253.8855 | -18.1447 | 2.56699105 | 15.52634316 | 96.7569 | 55602.7046412037 | 55603.1488657407 | 405032010 | 20024.3 | 20000 | 20032.3 | 20040.3 | 0 | 20024.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18152.8 | 18152.8 | 38343.9 | 0 | PROCESSED | 55616.932650463 | 55983 | 55617.4104282407 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050116 | Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 5 | AO5 | QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION | XIS | Y | | XSS J17223-7301 | 259.6949 | -73.4263 | 319.10640118 | -19.70481928 | 106.6643 | 55302.152650463 | 55302.5939467593 | 405033010 | 33386.1 | 30000 | 33386.1 | 33386.1 | 0 | 33386.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25588.9 | 25588.9 | 38127.9 | 0 | PROCESSED | 55326.1356828704 | 55692 | 55326.1437731482 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 050116 | Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 5 | AO5 | QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION | XIS | Y | | EG AND | 11.168 | 40.673 | 121.54657283 | -22.18054863 | 225.2111 | 55597.6281018518 | 55600.0030092593 | 405034010 | 100533.3 | 100000 | 100533.3 | 100541.3 | 0 | 100549.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84658.9 | 84658.9 | 205171.9 | 3 | PROCESSED | 55614.2725 | 55983 | 55614.2972106482 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051211 | The goals of this proposal are to use Suzaku XIS observations to : 1) determine whether EG And, BX Mon, and BF Cyg are members of the recently recognized class of hard X-ray emitting symbiotic stars; and 2) if they are, compare the nature of any absorption, the optical depth of the boundary layer, and the accretion rate to those of the well established hard X-ray symbiotics. Understanding the accretion processes in symbiotic stars is a crucial step in determining the role they play as progenitors of type Ia supernovae. | GALACTIC POINT SOURCES | 4 | C | NELSON | THOMAS | NULL | NULL | USA | 5 | AO5 | EXPLORING THE ACCRETION DISK BOUNDARY LAYERS OF SYMBIOTIC STARS | XIS | Y | | 4 DRA | 187.4841 | 69.1938 | 125.77229084 | 47.81569563 | 339.9969 | 55304.8913773148 | 55305.8557291667 | 405035010 | 42260.2 | 40000 | 42268.2 | 42268.2 | 0 | 42260.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43792 | 43792 | 83277.8 | 1 | PROCESSED | 55327.2043981482 | 55693 | 55327.2173958333 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051212 | The symbiotic star, 4 Dra, has been poorly studied in X-rays. Based on the ROSAT data, we argue that it is a nearby, lower accretion rate analogue of the hard X-ray bright symibiotic stars that have been detected above 10 keV. We propose the first pointed observation of 4 Dra that covers the entire 0.4-10 keV band to test our interpretation: we expect it to be bright above 2 keV, with an optically thin thermal spectrum, likely with a strong and complex intrinsic absorber. If confirmed, 4 Dra may turn out to be a key object in the study of hard X-ray emitting symbiotic stars. | GALACTIC POINT SOURCES | 4 | B | MUKAI | KOJI | NULL | NULL | USA | 5 | AO5 | THE FIRST LOOK AT THE SYMBIOTIC STAR 4 DRA ABOVE 2 KEV | XIS | Y | | V2491 CYG | 295.7679 | 32.3068 | 67.2208484 | 4.33923679 | 253.6206 | 55503.4390162037 | 55505.2709837963 | 405036010 | 74400.4 | 70000 | 74400.4 | 74400.4 | 0 | 74400.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57206.5 | 57206.5 | 158251.9 | 2 | PROCESSED | 55518.384525463 | 55885 | 55518.4178356482 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051213 | We propose to observe again one of the most luminous and intriguing classical novae of the last two years, after it has returned to quiescence. The goala are to understand how accretion is re-estabilished, investigate the claim that the white dwarf an intermediate polar (IP), estimate mass accretion are and white dwarf mass. IP are a class of X-ray sources that Suzaku is ideally suited to study, and we want to study the influence of the magnetic field on the nova evolution. | GALACTIC POINT SOURCES | 4 | C | ORIO | MARINA | NULL | NULL | USA | 5 | AO5 | REVISITING AN X-RAY LUMINOUS NOVA NOVA AFTER THE ERUPTION | XIS | Y | | PSR B1259-63 | 195.6931 | -63.8349 | 304.18120501 | -0.9906484 | 99.8696 | 55566.8369212963 | 55569.3959722222 | 405037010 | 90040.7 | 80000 | 90040.7 | 90040.7 | 0 | 90040.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74450.6 | 74450.6 | 221061.8 | 1 | PROCESSED | 55595.2265856482 | 55961 | 55595.2642939815 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051221 | We propose to observe a gamma-ray binary PSR B1259-63 during the pulsar's second disk crossing after periastron passage. PSR B1259-63 is a young radio pulsar orbiting around a B2e star with a highly eccentric 3.4 yr orbit. Suzaku XIS+HXD measurements of the hard continuum emission from the binary system allow us to investigate particle acceleration in a highly variable environment as a result of interactions between the relativistic wind of the pulsar and the circumstellar disk of the Be star. With the advent of the Fermi Gamma-ray Space Telescope, we will be able to simultaneously observe X-rays and GeV gamma-rays during the disk transit for the first time. The observations of PSR B1259-63 will give us a unique opportunity to study the physics of pulsar winds on AU-scale. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | USA | 5 | AO5 | SUZAKU BROADBAND OBSERVATIONS OF A GAMMA-RAY BINARY PSRB1259-63 DURING THE POST-PERIASTRON FLARE IN 2011 | XIS | Y | | PSR B1259-63 | 195.6913 | -63.8356 | 304.18038114 | -0.9913128 | 117.5773 | 55594.1927662037 | 55594.4487731482 | 405038010 | 21478.1 | 20000 | 21494.1 | 21478.1 | 0 | 21494.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15677.4 | 15677.4 | 22111.9 | 0 | PROCESSED | 55607.1219212963 | 55974 | 55607.1295601852 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051221 | We propose to observe a gamma-ray binary PSR B1259-63 during the pulsar's second disk crossing after periastron passage. PSR B1259-63 is a young radio pulsar orbiting around a B2e star with a highly eccentric 3.4 yr orbit. Suzaku XIS+HXD measurements of the hard continuum emission from the binary system allow us to investigate particle acceleration in a highly variable environment as a result of interactions between the relativistic wind of the pulsar and the circumstellar disk of the Be star. With the advent of the Fermi Gamma-ray Space Telescope, we will be able to simultaneously observe X-rays and GeV gamma-rays during the disk transit for the first time. The observations of PSR B1259-63 will give us a unique opportunity to study the physics of pulsar winds on AU-scale. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | USA | 5 | AO5 | SUZAKU BROADBAND OBSERVATIONS OF A GAMMA-RAY BINARY PSRB1259-63 DURING THE POST-PERIASTRON FLARE IN 2011 | XIS | Y | | 4U 0115+63 | 19.63292 | 63.74 | 125.92365665 | 1.02574493 | -99 | NULL | NULL | 405039010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051231 | We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 5 | AO5-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | N | | CEP X-4 | 324.878 | 56.98611 | 99.01219478 | 3.31239245 | -99 | NULL | NULL | 405040010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051231 | We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 5 | AO5-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | N | | XTE J1946+274 | 296.4201 | 27.2906 | 63.14511565 | 1.35338176 | 267.925 | 55480.9086805556 | 55482.2446064815 | 405041010 | 50731.7 | 45000 | 50731.7 | 50731.7 | 0 | 50731.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46557.1 | 46557.1 | 115373.9 | 1 | PROCESSED | 55491.0811226852 | 55867 | 55491.1017476852 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051231 | We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 5 | AO5-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y | | V 0332+53 | 53.7495 | 53.17319 | 146.05199466 | -2.19402959 | -99 | NULL | NULL | 405042010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051231 | We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 5 | AO5-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | N | | A 0535+26 | 84.7275 | 26.31581 | 181.44506907 | -2.64343705 | -99 | NULL | NULL | 405043010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051231 | We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 5 | AO5-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | N | | 4U 1626-67 | 248.0734 | -67.4643 | 321.7866399 | -13.09493758 | 285.8172 | 55445.5409259259 | 55446.2376273148 | 405044010 | 20033.5 | 20000 | 20033.5 | 20057.5 | 0 | 20045.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19537.2 | 19537.2 | 60179.9 | 0 | PROCESSED | 55456.2165162037 | 55822 | 55456.2336574074 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051234 | Recent X-ray observations by Fermi/GBM and Swift/BAT of 4U 1626-67 discovered a new torque reversal of this source after 18 years of steady spinning down. Centered on Feb 4 2008, a dramatic increase in the X-ray flux was also observed. The lack of correlation between the X-ray flux and the torque applied to the neutron star before the transition, challenges our understanding of the physical mechanisms operating in this system. The main goal of this proposal is to look for changes in the long term flux behavior, energy spectra, pulse profile, line features and power spectra with the current evolution in 4U1626-67 s spin-up rate. In addition, we wish to determine whether the absence of the QPO observed just after the torque reversal persist. | GALACTIC POINT SOURCES | 4 | A | FINGER | MARK | NULL | NULL | USA | 5 | AO5 | THE ACCRETING X-RAY PULSAR 4U 1626-67 AFTER A NEW TORQUE REVERSAL | XIS | Y | | 4U 1210-64 | 183.3036 | -64.8719 | 298.88624165 | -2.30082607 | 98.4956 | 55553.1591550926 | 55555.1488194444 | 405045010 | 79347.6 | 80000 | 79347.6 | 79347.6 | 0 | 79356.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70751.2 | 70751.2 | 171879.9 | 0 | PROCESSED | 55595.0570717593 | 55961 | 55595.085474537 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051236 | 4U 1210-64 is a high mass X-ray binary with a stable 6.7 day period when the long-term (RXTE ASM) light curve is analyzed. However, we observed strong aperiodic variability in a series of pointed observations with the RXTE PCA, to the point of masking this 6.7 day period. Moreover, we have not detected a spin period, even though the accretor is most likely a neutron star. The strong variability is suggestive of accretion from a clumpy wind. We propose a 2-day Suzaku observation of this object (1) to search for unequivocal evidence for a neutron star, such as the spin period and cyclotron features; and (2) to measure the spectral shapes at different flux levels, to investigate the cause of the strong aperiodic variability. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 5 | AO5 | 4U 1210-64: A HIGHLY VARIABLE X-RAY BINARY | XIS | Y | | 4U 0614+091 | 94.28042 | 9.13694 | 200.87736381 | -3.36351731 | -99 | NULL | NULL | 405046010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051241 | Suzaku has recently revealed relativistically broadened Fe K emission lines in the spectra of neutron star low-mass X-ray binaries (LMXBs). We have now seen these lines in 10 neutron star LMXBs, allowing measurements of the inner accretion disk radius, and hence an upper limit on the neutron star radius in all these objects. Both the sensitivity and broadband capability of Suzaku, make it possible to robustly determine the line shape. Here, we propose to observe two sources where no Fe K line was previously detected with older missions. Both sources are accreting at low Eddington fractions (<1%), hence we can test whether Fe K emission lines are ubiquitous in neutron star LMXBs at all luminosities, and explore whether the inner accretion disk is truncated at low Eddington fractions. | GALACTIC POINT SOURCES | 4 | C | CACKETT | EDWARD | NULL | NULL | USA | 5 | AO5 | ARE FE KALPHA EMISSION LINES UBIQUITOUS IN NEUTRON STAR LMXBS? | XIS | N | | GX13+1 | 273.63192 | -17.15589 | 13.51807927 | 0.10669908 | -99 | NULL | NULL | 405047010 | -99 | 30000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051243 | We recently proposed physical mechanisms to explain the 3 branches and 2 vertices of the accreting neutron stars known as Z sources. This work defines how the Eddington limit operates in the inner disk, and there is a need to investigate the inferred mass loss using other techniques. In parallel, we have used spectral analyses to reclassify GX13+1 as a Z source (Cyg X-2 sub-group). GX13+1 has exhibited strong, blue-shifted absorption lines (Chandra) and a moderate Fe emission line (RXTE). Observations of GX13+1 with Suzaku are intended: to refine the spectral model, to further test the models for each Z branches, to measure the profile and variations of the Fe emission line, and, most importantly, to determine whether the properties of the disk wind vary with position along the Z. | GALACTIC POINT SOURCES | 4 | C | REMILLARD | RONALD | NULL | NULL | USA | 5 | AO5 | SPECTRAL EVOLUTION AND THE DISK WIND IN GX13+1 | XIS | N | | 4U 1728-34 | 262.9799 | -33.9051 | 354.23908298 | -0.18221646 | 278.0266 | 55473.517349537 | 55475.6876967593 | 405048010 | 50547.2 | 100000 | 50652.2 | 50547.2 | 0 | 50652.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95360.6 | 95360.6 | 187467.8 | 3 | PROCESSED | 55487.4216898148 | 55867 | 55487.4662615741 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051244 | Fe K-alpha lines have been detected in ten NS-LMXBs. Under the commonly accepted interpretation, they can be used to set tight constrains on the accretion disk geometry. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kHz QPOs. We have recently shown that simultaneous measurements of Fe lines and kHz QPOs in a NS-LMXB appear to contradict this picture. We propose to observe 4U 1728-34 with Suzaku five times for 20 ks, simultaneously with RXTE and ATCA. This program will allow us to study and compare the dynamics of the inner edge of the disk as inferred from the Fe line and the kHz QPOs, as well as the relation of both observables with the jet radio emission. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | USA | 5 | AO5 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y | | 4U 1608-52 | 243.17917 | -52.42306 | 330.92633867 | -0.85047716 | -99 | NULL | NULL | 405049010 | -99 | 120000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051245 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | USA | 5 | AO5-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | XIS | N | | AQL X-1 | 287.81687 | 0.58494 | 35.71842844 | -4.14317601 | -99 | NULL | NULL | 405050010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051246 | Long term optical/X-ray monitoring of X-ray binaries has revealed that the accretion flow pattern can be remarkably different during different outbursts of the same source, challenging standard disk-instability models. Of particular interest is the Low-Intensity State (LIS) in Aql X-1, where the optical-to-X-ray flux ratio is about a factor of 7 higher than that during normal outbursts explainable using the disk-instability model. Suzaku data, along with contemporaneous optical/IR and radio observations, will allow probing the nature of accretion flow in the LIS of Aql X-1. We request a 100 ksec ToO observation of Aql X-1 during a LIS to achieve our science goals. The observation will test the predictions of ADIOS models and constrain disk--jet coupling. | GALACTIC POINT SOURCES | 4 | A | MAITRA | DIPANKAR | NULL | NULL | USA | 5 | AO5-TOO | SUZAKU OBSERVATIONS OF AQL X-1 DURING ITS LOW-INTENSITY STATE | HXD | N | | 4U 1630-47 | 248.5034 | -47.402 | 336.90313759 | 0.24577164 | 279.8256 | 55432.911724537 | 55435.6134259259 | 405051010 | 99937.3 | 100000 | 99937.3 | 99937.3 | 0 | 99937.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90451.2 | 90451.2 | 233397.6 | 2 | PROCESSED | 55449.390162037 | 55815 | 55449.4369560185 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051252 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 5 | AO5-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | Y | | XTE J1752-223 | 268.06288 | -22.34233 | 6.42317982 | 2.11424017 | -99 | NULL | NULL | 405052010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051252 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 5 | AO5-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | N | | XTE J1118+480 | 169.54542 | 48.03694 | 157.66026546 | 62.32060029 | -99 | NULL | NULL | 405053010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051252 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 5 | AO5-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | N | | XTE J1550-564 | 237.74458 | -56.47667 | 325.88223339 | -1.82706287 | -99 | NULL | NULL | 405054010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051252 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 5 | AO5-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | N | | 4U 1543-47 | 236.78583 | -47.66944 | 330.91865964 | 5.42579106 | -99 | NULL | NULL | 405055010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051252 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 5 | AO5-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | N | | GRS 1915+105 | 288.79833 | 10.94556 | 45.36563993 | -0.21936861 | -99 | NULL | NULL | 405056010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 051253 | We propose a 25ks on-source (100ks total) ToO to observe a soft state of GRS 1915+105 at L<30% L Edd. This ToO will address several important science goals: (1) a measurement of the black hole spin via two independent methods (X-ray continuum fitting and broad iron line analysis), (2) the determination of the accretion disk-corona geometry via studies of fluorescence lines and Compton reflection components, and (3) investigation of the broad-band spectrum for input into photoionization models. | GALACTIC POINT SOURCES | 4 | A | LEE | JULIA | NULL | NULL | USA | 5 | AO5-TOO | MEASURING THE GRS 1915+105 BLACK HOLE SPIN AND BROADBAND CONTINUUM PROPERTIES | XIS | N | | 4U 1957+11 | 299.8426 | 11.72 | 51.31417386 | -9.31797438 | 71.6227 | 55320.4377777778 | 55321.4168055556 | 405057010 | 35796 | 35000 | 35804 | 35804 | 0 | 35796 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30869.2 | 30869.2 | 84580 | 0 | PROCESSED | 55371.2334722222 | 55741 | 55375.7567013889 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051254 | We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. | GALACTIC POINT SOURCES | 4 | B | NOWAK | MICHAEL | NULL | NULL | USA | 5 | AO5 | 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? | XIS | Y | | 4U 1957+11 | 299.8418 | 11.7197 | 51.31351001 | -9.31745051 | 63.9325 | 55333.5190277778 | 55334.4675 | 405057020 | 34935.3 | 35000 | 34943.3 | 34951.3 | 0 | 34935.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28262.5 | 28262.5 | 81911.8 | 0 | PROCESSED | 55347.2287037037 | 55714 | 55347.2466898148 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051254 | We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. | GALACTIC POINT SOURCES | 4 | B | NOWAK | MICHAEL | NULL | NULL | USA | 5 | AO5 | 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? | XIS | Y | | 4U 1957+11 | 299.8589 | 11.6979 | 51.30303986 | -9.34292333 | 251.3459 | 55501.8275462963 | 55502.7001157407 | 405057030 | 35349.1 | 35000 | 35357.1 | 35349.1 | 0 | 35357.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27169.7 | 27169.7 | 75362 | 0 | PROCESSED | 55515.2803125 | 55881 | 55515.3015046296 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 051254 | We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. | GALACTIC POINT SOURCES | 4 | B | NOWAK | MICHAEL | NULL | NULL | USA | 5 | AO5 | 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? | XIS | Y | | HER X-1 | 254.4936 | 35.2712 | 58.06646448 | 37.48255114 | 250.0637 | 55467.7830208333 | 55468.2362962963 | 405058010 | 21356.7 | 20000 | 21356.7 | 21356.7 | 0 | 21503.4 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 18932.3 | 18932.3 | 39159.9 | 0 | PROCESSED | 55477.2114930556 | 55843 | 55477.2237152778 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 052001 | We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? | GALACTIC POINT SOURCES | 4 | B | STAUBERT | R DIGER | NULL | NULL | EUR | 5 | AO5 | VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 | HXD | N | | HER X-1 | 254.4925 | 35.2707 | 58.06565994 | 37.48335671 | 250.2455 | 55468.7003356482 | 55469.2258912037 | 405058020 | 24303 | 20000 | 24303 | 24322.3 | 0 | 24467.7 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 22483.7 | 22483.7 | 45405.9 | 0 | PROCESSED | 55482.1187037037 | 55848 | 55482.4726967593 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 052001 | We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? | GALACTIC POINT SOURCES | 4 | B | STAUBERT | R DIGER | NULL | NULL | EUR | 5 | AO5 | VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 | HXD | N | | HER X-1 | 254.4632 | 35.2657 | 58.05457552 | 37.50615868 | 268.4858 | 55461.0002083333 | 55461.4494675926 | 405058030 | 19924 | 20000 | 19924 | 19924 | 0 | 20243.8 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 17507.3 | 17507.3 | 38811.9 | 0 | PROCESSED | 55470.1317708333 | 55836 | 55470.1508796296 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 052001 | We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? | GALACTIC POINT SOURCES | 4 | B | STAUBERT | R DIGER | NULL | NULL | EUR | 5 | AO5 | VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 | HXD | N | | HER X-1 | 254.4619 | 35.2659 | 58.05460857 | 37.50723847 | 268.3041 | 55461.7937037037 | 55462.2467476852 | 405058040 | 21740 | 20000 | 21740 | 21796 | 0 | 21870.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19803 | 19803 | 39135.9 | 0 | PROCESSED | 55474.0823958333 | 55840 | 55474.0995486111 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 052001 | We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? | GALACTIC POINT SOURCES | 4 | B | STAUBERT | R DIGER | NULL | NULL | EUR | 5 | AO5 | VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 | HXD | N | | MU COL | 86.4962 | -32.3107 | 237.28985275 | -27.10600903 | 93.5874 | 55455.752337963 | 55456.3113541667 | 405059010 | 25961 | 20000 | 25961 | 25961 | 0 | 25961 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21873.4 | 21873.4 | 48287.9 | 0 | PROCESSED | 55469.2321759259 | 55836 | 55469.2452314815 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 052005 | We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models. | GALACTIC POINT SOURCES | 4 | A | OSKINOVA | LIDIA | NULL | NULL | EUR | 5 | AO5 | STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKU | XIS | Y | | 10 LAC | 339.8111 | 39.0619 | 96.65409432 | -16.97165842 | 81.7456 | 55344.5001967593 | 55345.0690162037 | 405060010 | 25028.4 | 25000 | 25028.4 | 25028.4 | 0 | 25028.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21743.1 | 21743.1 | 49135.9 | 2 | PROCESSED | 55365.1720601852 | 55731 | 55365.1824305556 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 052005 | We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models. | GALACTIC POINT SOURCES | 4 | A | OSKINOVA | LIDIA | NULL | NULL | EUR | 5 | AO5 | STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKU | XIS | Y | | IGR J17348-2045 | 263.737 | -20.747 | 5.68701621 | 6.37961854 | -99 | NULL | NULL | 405061010 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 052010 | Soft gamma repeaters (SGRs) and the Anomalous X-ray pulsars (AXPs) constitute a small class of X-ray sources which are currently believed to host an ultra-magnetized neutron star, or magnetar. In this framework their bursting and persistent emission is powered by the decay of the ultra-strong field. Magnetar sources are rare (~15 known at present). Enlarging the sample of these objects is vital as it allows to test further models for their activity and as it will shed light on the links/differences among magnetars and other classes of isolated neutron stars. Our aim is to identify the two most promising magnetar candidates, selected among numerous unidentified INTEGRAL sources, because of their hard and peculiar X-ray spectrum and closeness to the galactic plane. | GALACTIC POINT SOURCES | 4 | C | PAVAN | LUCIA | NULL | NULL | EUR | 5 | AO5 | CATCHING MAGNETAR CANDIDATES AMONG UNIDENTIFIED INTEGRAL SOURCES WITH SUZAKU | XIS | N | | GX 339-4 | 255.7015 | -48.7852 | 338.94105133 | -4.32146688 | 83.6944 | 55603.7634722222 | 55604.2349421296 | 405063010 | 22459.4 | 100000 | 22459.4 | 22459.4 | 0 | 22483.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19328.7 | 19328.7 | 40727.9 | 0 | PROCESSED | 55616.9623032407 | 55983 | 55617.4120601852 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | Y | | GX 339-4 | 255.7013 | -48.7848 | 338.94128957 | -4.32111913 | 86.3597 | 55608.9686111111 | 55609.6501967593 | 405063020 | 21015.7 | 20000 | 21015.7 | 21015.7 | 0 | 21015.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17595.8 | 17595.8 | 58883.9 | 0 | PROCESSED | 55621.143125 | 55988 | 55621.1561342593 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | Y | | GX 339-4 | 255.7016 | -48.7831 | 338.94276391 | -4.32024293 | 90.1024 | 55616.8233680556 | 55617.4487268518 | 405063030 | 19182 | 20000 | 19190 | 19198 | 0 | 19182 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15684 | 15684 | 54025.9 | 1 | PROCESSED | 55628.1548032407 | 55996 | 55628.1679976852 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | Y | | GX 339-4 | 255.7013 | -48.7851 | 338.94105066 | -4.32130146 | 91.6296 | 55620.1778703704 | 55620.8022569445 | 405063040 | 21799 | 20000 | 21799 | 21807 | 0 | 21816.8 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 18850.2 | 18850.2 | 53923.9 | 0 | PROCESSED | 55642.1146527778 | 56009 | 55642.1310300926 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | Y | | GX 339-4 | 255.7041 | -48.783 | 338.94384752 | -4.32149031 | 92.8952 | 55627.5468518518 | 55628.0320138889 | 405063050 | 16992.5 | 20000 | 16992.5 | 20269.3 | 0 | 20269.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15985.1 | 15985.1 | 41874.1 | 2 | PROCESSED | 55645.1978935185 | 56015 | 55645.2088078704 | 2.5.16.29 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | Y | | XTE J1817-330 | 274.43142 | -33.01883 | 359.81722428 | -7.99557413 | -99 | NULL | NULL | 405064010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | N | | GRO J1655-40 | 253.5 | -39.84581 | 344.98161118 | 2.45630442 | -99 | NULL | NULL | 405065010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | N | | XTE J1550-564 | 237.74458 | -56.47667 | 325.88223339 | -1.82706287 | -99 | NULL | NULL | 405066010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | N | | XTE J1118+480 | 169.54542 | 48.03694 | 157.66026546 | 62.32060029 | -99 | NULL | NULL | 405067010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | N | | J1832-084 | 278.15417 | -8.45111 | 23.27208255 | 0.29793506 | -99 | NULL | NULL | 405068010 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 052021 | The Galactic TeV sky is dominated by extended sources. Of the identified sources, only young pulsar wind nebulae (PWN) and binary systems are unresolved. TeV gamma-ray emission from these systems probes high energy particles very close to their acceleration sites. Binary systems offer additional diagnostic tools, e.g. through the modulation and the high density of the target photon field involved in the TeV-emitting Inverse Compton process. We propose Suzaku observations of a few TeV sources detected in ongoing H.E.S.S. observations of the Galactic plane, where a binary system counterpart is a plausible scenario for the TeV emission. The Suzaku data are necessary to confirm the nature of these new objects. | GALACTIC POINT SOURCES | 4 | C | PUEHLHOFER | GERD | NULL | NULL | EUR | 5 | AO5 | TEV BINARIES: A COMMON PHENOMENON? | XIS | N | | IGR J16318-4848 | 247.967 | -48.808 | 335.62953228 | -0.44925356 | -99 | NULL | NULL | 405072010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 052023 | IGR J16318-4848 is a high mass X-ray binary with a column density of the order of 10^{24} cm^{-2}, which makes it one of the most extremely absorbed galactic objects. The absorption is strongly variable and thus mostly intrinsic to the source. The compact object (whose nature is still unknown) is deeply embedded in the stellar wind of its sgB | GALACTIC POINT SOURCES | 4 | C | BARRAGAN | LAURA | NULL | NULL | EUR | 5 | AO5 | THE MYSTERIOUS SOURCE IGR J16318-4848 | XIS | N | | 4U 1909+07 | 287.7097 | 7.5883 | 41.89273161 | -0.82371888 | 247.9131 | 55502.7037847222 | 55503.4337731482 | 405073010 | 29298.2 | 25000 | 29298.2 | 29298.2 | 0 | 29298.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21391.1 | 21391.1 | 63051.9 | 0 | PROCESSED | 55515.2723032407 | 55882 | 55515.2869328704 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 052024 | We propose the first observation of the neutron star HMXB 4U 1909+07 with Suzaku. The aim of the proposed 25 ksec observation is to study the broadband spectrum of the source. The data will provide information about the structure and ionization state of the accreted medium, as well as of the geometry of the accretion column and the strength of the magnetic field. No high-resolution CCD spectra of this source have been published so far. The source shows flaring behavior, so the wind is expected to be strongly clumped, which could be probed by studying the evolution of N_H and the iron line with high time resolution. Furthermore we will perform phase resolved spectroscopy to study the spectral variation with pulse phase and perform a detailed search for a CRSF. | GALACTIC POINT SOURCES | 4 | A | FUERST | FELIX | NULL | NULL | EUR | 5 | AO5 | STUDYING ACCRETION IN THE UNCELEBRATED HMXB 4U 1909+07 | XIS | Y | | FU ORIONIS | 86.34333 | 9.07 | 197.10930446 | -10.25127964 | -99 | NULL | NULL | 405074010 | -99 | 150000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 052025 | Fluorescent 6.4 keV iron K alpha lines provide information on both the cool matter in the vicinity of bright X-ray sources and the sources themselves. The fluorescent line is a strong indicator of disk ionization, which is a pre-requisite for the efficient work of the magneto-rotational instability as the driver of the protostellar mass accretion process. We propose to obtain a deep Suzaku spectrum of FU Ori, the prototype of the young, strongly accreting eruptive stars called FUors. Our goal is to unambiguously detect the 6.4 keV fluorescent line and study the possible origin of the line in the circumstellar environment. Our results may provide evidence for a connection between disk ionization and accretion, supporting the role of MRI in young protostellar disks. | GALACTIC POINT SOURCES | 4 | C | ABRAHAM | PETER | NULL | NULL | EUR | 5 | AO5 | STUDYING CIRCUMSTELLAR DISK IONIZATION IN A RAPIDLY-ACCRETING YOUNG STELLAR OBJECT VIA X-RAY FLUORESCENCE | XIS | N | | SGR 0501+4516 | 75.2625 | 45.3425 | 161.48747118 | 1.98100999 | 82.3996 | 55459.7272569444 | 55460.9897337963 | 405075010 | 59720.5 | 50000 | 59808.5 | 59812.3 | 0 | 59720.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 52935.7 | 52935.7 | 109065.8 | 0 | PROCESSED | 55470.1283449074 | 55287 | 55470.1458449074 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 056002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 5 | AO5 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y | | 1RXS J1708-4009 | 257.2038 | -40.2142 | 346.43162325 | -0.00870489 | 267.1357 | 55466.6124074074 | 55467.7738425926 | 405076010 | 62810.9 | 60000 | 62818.9 | 62822.6 | 0 | 62810.9 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 59511.4 | 59511.4 | 100323.9 | 1 | PROCESSED | 55477.2603009259 | 55287 | 55477.2762268518 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 056002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 5 | AO5 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y | | GX 1+4 | 263.0071 | -24.816 | 1.87675865 | 4.75818757 | 273.1727 | 55471.2801273148 | 55473.5140509259 | 405077010 | 99670 | 100000 | 99670.4 | 99670 | 0 | 99670.4 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 96525.9 | 96525.9 | 192609.1 | 0 | PROCESSED | 55487.3194444444 | 55287 | 55487.4199537037 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 056002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 5 | AO5 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y | | 4U 1538-522 | 235.59708 | -52.38611 | 327.41949089 | 2.163702 | -99 | NULL | NULL | 405078010 | -99 | 160000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 55287 | NULL | NULL | NULL | NULL | 051232 | Observations of accreting pulsars in High Mass X-ray Binaries (HMXBs) provide us with important information about the physical processes in the stellar wind of the high mass donar star, the coupling between the accreting material and the neutron star's magnetic field, and the physics of the strongly magnetized accretion column above the neutron star magnetic poles. In this proposal we request four, non-time constrained, 40 ks observations of the accreting HMXB 4U1538-522 to conduct the most sensitive study to date of the wide range of changes of the broad band (0.1-100 keV) spectrum with respect to both binary and pulse phase. | GALACTIC POINT SOURCES | 4 | C | ROTHSCHILD | RICHARD | NULL | NULL | USA | 5 | AO5 | THE FIRST SUZAKU OBSERVATIONS OF 4U 1538-522 | HXD | N | | GX 339-4 | 255.70583 | -48.78961 | 338.93927787 | -4.32641254 | -99 | NULL | NULL | 406001010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | GX 339-4 | 255.70583 | -48.78961 | 338.93927787 | -4.32641254 | -99 | NULL | NULL | 406001020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | GX 339-4 | 255.70583 | -48.78961 | 338.93927787 | -4.32641254 | -99 | NULL | NULL | 406001030 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | XTE J1550-504 | 237.74458 | -56.47667 | 325.88223339 | -1.82706287 | -99 | NULL | NULL | 406002010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | XTE J1550-504 | 237.74458 | -56.47667 | 325.88223339 | -1.82706287 | -99 | NULL | NULL | 406002020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | XTE J1550-504 | 237.74458 | -56.47667 | 325.88223339 | -1.82706287 | -99 | NULL | NULL | 406002030 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | GRO J1655-40 | 253.5 | -39.84581 | 344.98161118 | 2.45630442 | -99 | NULL | NULL | 406003010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | GRO J1655-40 | 253.5 | -39.84581 | 344.98161118 | 2.45630442 | -99 | NULL | NULL | 406003020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | GRO J1655-40 | 253.5 | -39.84581 | 344.98161118 | 2.45630442 | -99 | NULL | NULL | 406003030 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | X1630-472 | 248.50458 | -47.39289 | 336.91037296 | 0.25136454 | -99 | NULL | NULL | 406004010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | X1630-472 | 248.50458 | -47.39289 | 336.91037296 | 0.25136454 | -99 | NULL | NULL | 406004020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | X1630-472 | 248.50458 | -47.39289 | 336.91037296 | 0.25136454 | -99 | NULL | NULL | 406004030 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | H1743-322 | 266.25833 | -32.22667 | 357.12592965 | -1.60785557 | -99 | NULL | NULL | 406005010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | H1743-322 | 266.25833 | -32.22667 | 357.12592965 | -1.60785557 | -99 | NULL | NULL | 406005020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | H1743-322 | 266.25833 | -32.22667 | 357.12592965 | -1.60785557 | -99 | NULL | NULL | 406005030 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060005 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | N | | V4641 SGR | 274.84013 | -25.40717 | 6.77395378 | -4.7890572 | -99 | NULL | NULL | 406006010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060006 | We propose a 100 ksec Suzaku observation of the Galactic microquasar V4641 Sgr in an outburst. V4641 Sgr has many unique characteristics:1)giant X-ray outbursts with fast rise and decay times, 2)violent variability in X-ray and optical bands, and 3)remarkable iron-K disk-line profiles in the X-ray spectrum. However, it is hardly understood due to the poor X-ray coverage which results from its short outburst duration and rapid intensity variations. Hence, we collaborate closely with VSNET, RXTE/ASM+PCA, MAXI and Swift/XRT+BAT team for a rapid trigger. The moderate energy resolution and wideband energy coverage of Suzaku enable us to clarify the radiation mechanisms of V4641 Sgr. This observation is now planed simultaneously with Swift, RXTE, many radio and optical/NIR observatories. | GALACTIC POINT SOURCES | 4 | A | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 6 | AO6-TOO | THE LARGEST-EVER CAMPAIGN OF THE GALACTIC MICROQUASAR V4641 SGR | XIS | N | | 1FGL J2339.7-0531 | 354.9077 | -5.5469 | 81.34836456 | -62.4702773 | 67.4026 | 55741.5915625 | 55743.8092361111 | 406007010 | 104091.4 | 100000 | 104091.4 | 104091.4 | 0 | 104099.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92902.2 | 92902.2 | 191583.7 | 2 | PROCESSED | 55775.3742939815 | 56144 | 55775.4025925926 | 2.6.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060007 | We propose to observe an unidentified Fermi source (1FGL J2339.7-0531) in the first-year Fermi catalog to search for the first ``radio-quiet'' Gamma-ray emitting millisecond pulsar. The Fermi source has a candidate X-ray counterpart from Chandra data and its X-ray and Gamma-ray properties are consistent with known Gamma-ray pulsars. This system is likely in a low-mass X-ray binary system based on optical observations. Both X-ray and optical observations show clear variability. We propose to observe the Chandra source with Suzaku to search for the possible orbital period and to study its X-ray spectrum in detail. The results will provide a better insight into the high-energy emission processes in the magnetosphere of millisecond pulsars. | GALACTIC POINT SOURCES | 4 | A | KONG | ALBERT | KATAOKA | JUN | JAP | 6 | AO6 | REVEALING THE NATURE OF AN UNIDENTIFIED FERMI SOURCE | XIS | Y | | 4U1812-12 | 273.8053 | -12.0935 | 18.04900466 | 2.37362039 | 267.159 | 55838.1400347222 | 55839.9168981482 | 406008010 | 62014.3 | 60000 | 62014.3 | 62014.3 | 0 | 62014.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53544.1 | 53544.1 | 153509.9 | 1 | PROCESSED | 55858.2838194444 | 56226 | 55858.3124768518 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060012 | Low-Mass X-ray binaries (LMXBs) are known to have soft and hard states, like black hole binaries. Through an analysis of archival Suzaku data of the LMXB Aql X-1 in the hard state, we obtained a clear picture of its accretion geometry; a truncated accretion disk, and a hot corona that Comptonize blackbody photons from the neutron star surface. In order to investigate whether this picture also applies to other LMXBs in the low/hard state, and to better constrain the accretion geometry in comparison with those of black hole binaries, we propose a 60 ksec Suzaku observation of the LMXB 4U 1812-12. This is a valuable object,which is known to reside almost always in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | SAKURAI | SOKI | NULL | NULL | JAP | 6 | AO6 | REVEALING THE ACCRETION GEOMETRY OF THE LOW/HARD STATE LMXB 4U 1812-12 WITH SUZAKU | XIS | Y | | VW HYI | 62.2833 | -71.2901 | 284.88594452 | -38.13999051 | 181.9815 | 55894.1004513889 | 55895.1821759259 | 406009010 | 70083.4 | 60000 | 70091.4 | 70083.4 | 0 | 70091.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64970.1 | 64970.1 | 93446.8 | 1 | PROCESSED | 55907.142025463 | 56274 | 55907.1562615741 | 2.7.16.31 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060023 | SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 6 | AO6-TOO | TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE | XIS | Y | | VW HYI | 62.3036 | -71.2936 | 284.88553906 | -38.13260514 | 212.7427 | 55924.6383796296 | 55925.1806828704 | 406009020 | 16159.3 | 20000 | 16159.3 | 16159.3 | 0 | 16159.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13758.7 | 13758.7 | 46851.9 | 0 | PROCESSED | 55945.9016087963 | 56313 | 55945.9133912037 | 2.7.16.31 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060023 | SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 6 | AO6-TOO | TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE | XIS | Y | | VW HYI | 62.3086 | -71.2914 | 284.88209314 | -38.1323503 | 276.4367 | 55986.5687962963 | 55987.2501273148 | 406009030 | 20109.7 | 20000 | 20109.7 | 20109.7 | 0 | 20109.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20571.2 | 20571.2 | 58857.9 | 1 | PROCESSED | 56018.9310185185 | 56385 | 56018.9417824074 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060023 | SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 6 | AO6-TOO | TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE | XIS | Y | | VW HYI | 62.29746 | -71.29481 | 284.88814052 | -38.13367962 | -99 | NULL | NULL | 406009040 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060023 | SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 6 | AO6-TOO | TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE | XIS | Y | | AQL X-1 | 287.8271 | 0.5745 | 35.71381986 | -4.15705073 | 244.5264 | 55852.1545486111 | 55853.110625 | 406010010 | 9494.8 | 40000 | 9596.8 | 9494.8 | 0 | 9596.8 | 2 | 1 | 0 | 1 | 1 | 0 | 0 | 35325 | 35325 | 82587.8 | 1 | PROCESSED | 55873.1044212963 | 56240 | 55873.1222337963 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060036 | We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object. | GALACTIC POINT SOURCES | 4 | A | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 6 | AO6-TOO | SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE | XIS | Y | | AQL X-1 | 287.8264 | 0.5741 | 35.71314195 | -4.15661165 | 244.5268 | 55855.5357986111 | 55856.4599884259 | 406010020 | 9940.6 | 40000 | 10041 | 9940.6 | 0 | 10041 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 37845.1 | 37845.1 | 79846 | 1 | PROCESSED | 55873.267037037 | 56241 | 55873.3025578704 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060036 | We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object. | GALACTIC POINT SOURCES | 4 | A | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 6 | AO6-TOO | SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE | XIS | Y | | AQL X-1 | 287.8278 | 0.5718 | 35.71173466 | -4.15890942 | 243.2618 | 55858.7269328704 | 55859.5786921296 | 406010030 | 8495 | 40000 | 8495 | 9538.3 | 0 | 9556.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 36476.8 | 36476.8 | 73581.9 | 2 | PROCESSED | 55874.1121759259 | 56241 | 55874.1380555556 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060036 | We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object. | GALACTIC POINT SOURCES | 4 | A | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 6 | AO6-TOO | SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE | XIS | Y | | OAO1657-415 | 255.2026 | -41.6667 | 344.36019061 | 0.31327103 | 285.9012 | 55830.3988425926 | 55832.6667939815 | 406011010 | 84729.9 | 80000 | 84733.7 | 84729.9 | 0 | 84741.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74588.5 | 74588.5 | 195929.7 | 2 | PROCESSED | 55858.2466550926 | 56226 | 55858.2768518518 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060037 | We propose Suzaku observation of accretion-powered pulsar OAO 1657-415 to study matter accretion onto the neutron star. This object is a unique high mass X-ray binary (HMXB) that shows intermediate characteristics between wind-fed accretion pulsars and disk-fed accretion pulsars. High S/N spectra obtained by XIS, HXD-PIN/GSO with short exposure time (1 ks) allow us to investigate short-time variability of physical states of the accretion column, which is close to the neutron star surface. The proposed observation also reveals the matter distribution in the HMXB by using a 6.4-keV iron fluorescence line and hard X-rays. The data at the phase of eclipse egress provide essential information about the stellar wind and atmosphere of the companion star to constrain its stellar type in question. | GALACTIC POINT SOURCES | 4 | B | ODAKA | HIROKAZU | NULL | NULL | JAP | 6 | AO6 | WIDE-BAND X-RAY OBSERVATION OF HIGH MASS X-RAY BINARY PULSAR OAO 1657-415 | XIS | Y | | PSR J0726-2612 | 111.531 | -26.2114 | 240.07877209 | -4.64696128 | 117.9984 | 55881.5691782407 | 55882.6252546296 | 406012010 | 43757 | 100000 | 43757 | 43792 | 0 | 43792 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39728.8 | 39728.8 | 91227.8 | 0 | PROCESSED | 55895.2231597222 | 56264 | 55895.2388078704 | 2.7.16.31 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060041 | To study the origin of magnetars, a unique opportunity is provided by detecting an excess of thermal radiation in the radio pulsars which has dipolar magnetic fields as high as magnetars. The excess is caused by field decay as seen in magnetars. A question is raised whether the rotation powered pulsars can have active magnetic flux similar to magnetars. PSR J0726-2612 is a nearby (3kpc) radio pulsar with magnetic field as high as 10^13.5 G, and therefore is an ideal target. We propose 100ksec observation of this pulsar to discover magnetar-like thermal radiation, and determine the structure of the active magnetic flux tubes by phase alignment of rotational modulation of the X-ray radiation with radio pulses. | GALACTIC POINT SOURCES | 4 | C | SHIBATA | SHINPEI | NULL | NULL | JAP | 6 | AO6 | CAN HIGH MAGNETIC FIELD RADIO PULSARS BE THE MAGNETAR ? | XIS | Y | | CYG X-1 | 299.5916 | 35.1745 | 71.31236822 | 3.05181611 | 279.5001 | 55839.9245023148 | 55840.9169328704 | 406013010 | 3702.7 | 40000 | 3832 | 3702.7 | 0 | 8031.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32962.5 | 32962.5 | 85733.9 | 1 | PROCESSED | 55964.282662037 | 56226 | 55964.3073032407 | 2.7.16.31 | 2 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060057 | We achieved 0.1 s time resolution with enough statistics on accumulating profiles of source brightening and made clear that electron temperature decreases and optical depth increases at the peak of brightness by using the XIS data of Psum mode. Progress to understanding the nature of fast time variability, which has been a mystery for 40 years since its discovery, connected with spectral properties is being made now. However, this property is not confirmed yet in other observations having different time scales of variability and spectral shapes, lacking the XIS data in Psum mode. We propose here another observation of Cyg X-1 with XIS0 1/8 window no burst, XIS1 1/4 window 0.5 s burst,and XIS3 Psum mode for a exposure of 40 ks. | GALACTIC POINT SOURCES | 4 | A | YAMADA | SHIN'YA | NULL | NULL | JAP | 6 | AO6 | REVEALING THE NATURE OF FAST TIME VARIABILITY OF CYG X-1 WITH SHOT ANALYSIS | XIS | Y | | RXJ2056.6+4940 | 314.1926 | 49.6559 | 89.31769097 | 2.74712249 | 241.0011 | 55887.7886805556 | 55888.5355208333 | 406014010 | 42373.1 | 40000 | 42381.1 | 42373.1 | 0 | 42373.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44666.5 | 44666.5 | 64524 | 1 | PROCESSED | 55897.0875925926 | 56264 | 55897.0994791667 | 2.7.16.31 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060065 | There are a total 1451 gamma-ray emitting objects in the Fermi 11-month survey catalogue. About 60% of sources were identified with counterparts in other wavelengths, most of which are extragalactic sources. Among them, XSS J12270-4859 stands out as a very peculiar Galactic source with unusual timing and spectral behaviours in the X-ray band. We aim to search for similar sources among the Fermi sources. | GALACTIC POINT SOURCES | 4 | C | ISO | NAOKI | NULL | NULL | JAP | 6 | AO6 | SEARCH FOR GAMMA-RAY BINARIES WITH A LOW-MASS COUNTERPART | XIS | Y | | RXJ0137.7+5814 | 24.46033 | 58.23644 | 129.02406462 | -4.08536809 | -99 | NULL | NULL | 406015010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060065 | There are a total 1451 gamma-ray emitting objects in the Fermi 11-month survey catalogue. About 60% of sources were identified with counterparts in other wavelengths, most of which are extragalactic sources. Among them, XSS J12270-4859 stands out as a very peculiar Galactic source with unusual timing and spectral behaviours in the X-ray band. We aim to search for similar sources among the Fermi sources. | GALACTIC POINT SOURCES | 4 | C | ISO | NAOKI | NULL | NULL | JAP | 6 | AO6 | SEARCH FOR GAMMA-RAY BINARIES WITH A LOW-MASS COUNTERPART | XIS | Y | | RXJJ0131.0+6120 | 22.780167 | 61.342639 | 127.67223223 | -1.16334415 | -99 | NULL | NULL | 406016010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060065 | There are a total 1451 gamma-ray emitting objects in the Fermi 11-month survey catalogue. About 60% of sources were identified with counterparts in other wavelengths, most of which are extragalactic sources. Among them, XSS J12270-4859 stands out as a very peculiar Galactic source with unusual timing and spectral behaviours in the X-ray band. We aim to search for similar sources among the Fermi sources. | GALACTIC POINT SOURCES | 4 | C | ISO | NAOKI | NULL | NULL | JAP | 6 | AO6 | SEARCH FOR GAMMA-RAY BINARIES WITH A LOW-MASS COUNTERPART | XIS | N | | 4U0114+65 | 19.4873 | 65.3067 | 125.69846298 | 2.57745686 | 71.642 | 55763.4307291667 | 55764.9453472222 | 406017010 | 106492.5 | 100000 | 106550.8 | 106558.8 | 0 | 106492.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88506.1 | 88506.1 | 130821.9 | 1 | PROCESSED | 55785.0199652778 | 56152 | 55785.0443981482 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060071 | We propose to observe an X-ray pulsar, 4U 0114+65 for 100 ks. This object is known to be a neutron star binary with an orbital period of 12 days and a long pulse priod of 10 ks. Our goals are to obtain time-averaged spectra of the XIS and HXD, and to quantify spectral changes between flare and quiescense phases, and to search for a cyclotron absorption line around ~ 60 keV. We also study pulse-phase resolved spectra. With these pieces of information, we aim at clarifying whether this source is a magnetar descendent or a neutron star with ordinary magnetic fields. | GALACTIC POINT SOURCES | 4 | A | SASANO | MAKOTO | NULL | NULL | JAP | 6 | AO6 | SEARCH FOR HIGH MAGNETIC NEUTRON STARS IN HIGH-MASS X-RAY BINARIES | XIS | Y | | 1RXSJ171405.2-202747 | 258.52167 | -20.46306 | 3.21688369 | 10.61566491 | -99 | NULL | NULL | 406018010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060085 | We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test accretion disk theories at intermediate mass accretion rates. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 6 | AO6 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | N | | 1RXSJ175911.0-344921 | 269.7922 | -34.8194 | 356.38251758 | -5.46102238 | 72.1205 | 55993.9029513889 | 55994.912650463 | 406019010 | 40181.3 | 40000 | 40181.3 | 40181.3 | 0 | 40181.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34751 | 34751 | 87233.9 | 1 | PROCESSED | 56016.4702083333 | 56385 | 56016.6680787037 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060085 | We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test accretion disk theories at intermediate mass accretion rates. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 6 | AO6 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | | 1RXSJ170047.8-314442 | 255.19917 | -31.745 | 352.21410507 | 6.39819107 | -99 | NULL | NULL | 406020010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060085 | We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test accretion disk theories at intermediate mass accretion rates. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 6 | AO6 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | N | | 24M2791 | 334.9577 | 63.2629 | 106.81877019 | 5.23758822 | 230.0008 | 55947.3704513889 | 55948.0926388889 | 406023010 | 34601.7 | 30000 | 34617.7 | 34601.7 | 0 | 34609.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35059.5 | 35059.5 | 62391.9 | 0 | PROCESSED | 55973.1002430556 | 56340 | 55973.1102893518 | 2.7.16.31 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060087 | We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object. | GALACTIC POINT SOURCES | 4 | C | OHNO | MASANORI | NULL | NULL | JAP | 6 | AO6 | SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES | XIS | Y | | 1FGL J1715.2-3319 | 258.713 | -33.4282 | 352.62684601 | 3.01774525 | 99.0737 | 56002.5629166667 | 56003.3750810185 | 406024010 | 32165 | 30000 | 32165 | 32165 | 0 | 32165 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27984.8 | 27984.8 | 70166 | 0 | PROCESSED | 56019.2392013889 | 56386 | 56019.2516435185 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060087 | We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object. | GALACTIC POINT SOURCES | 4 | C | OHNO | MASANORI | NULL | NULL | JAP | 6 | AO6 | SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES | XIS | Y | | 24M2216 | 272.27 | -20.083 | 10.33112365 | -0.1699965 | -99 | NULL | NULL | 406025010 | -99 | 30000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060087 | We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object. | GALACTIC POINT SOURCES | 4 | C | OHNO | MASANORI | NULL | NULL | JAP | 6 | AO6 | SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES | XIS | N | | SGR 1900+14 | 286.80933 | 9.322 | 43.02065561 | 0.7658283 | -99 | NULL | NULL | 406028010 | -99 | 60000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060092 | We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI. | GALACTIC POINT SOURCES | 4 | A | NAKAGAWA | YUJIN | NULL | NULL | JAP | 6 | AO6-TOO | A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS | HXD | N | | AXP 1E 2259+586 | 345.28454 | 58.87903 | 109.08734924 | -0.99573332 | -99 | NULL | NULL | 406029010 | -99 | 60000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060092 | We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI. | GALACTIC POINT SOURCES | 4 | A | NAKAGAWA | YUJIN | NULL | NULL | JAP | 6 | AO6-TOO | A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS | HXD | N | | AXP 1RXS J1708-4009 | 257.20417 | -40.15278 | 346.48106604 | 0.02773557 | -99 | NULL | NULL | 406030010 | -99 | 60000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060092 | We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI. | GALACTIC POINT SOURCES | 4 | A | NAKAGAWA | YUJIN | NULL | NULL | JAP | 6 | AO6-TOO | A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS | HXD | N | | AXP 4U 0142+614 | 26.5682 | 61.7591 | 129.37061357 | -0.42523158 | 40.384 | 55811.6552314815 | 55812.5731134259 | 406031010 | 38649.7 | 60000 | 38649.7 | 38649.7 | 0 | 38682.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42196.4 | 42196.4 | 79292 | 0 | PROCESSED | 55848.166412037 | 56218 | 55851.4406828704 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060092 | We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI. | GALACTIC POINT SOURCES | 4 | A | NAKAGAWA | YUJIN | NULL | NULL | JAP | 6 | AO6-TOO | A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS | XIS | Y | | AXP 1E 1048.1-5937 | 162.53721 | -59.88886 | 288.25965957 | -0.51808465 | -99 | NULL | NULL | 406032010 | -99 | 60000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 060092 | We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI. | GALACTIC POINT SOURCES | 4 | A | NAKAGAWA | YUJIN | NULL | NULL | JAP | 6 | AO6-TOO | A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS | HXD | N | | RS OPH | 267.5535 | -6.6951 | 19.81011082 | 10.37967032 | 94.9072 | 55987.2608796296 | 55988.855 | 406033010 | 69386 | 100000 | 69386 | 69386 | 0 | 69386 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60089.9 | 60089.9 | 137719.8 | 0 | PROCESSED | 56008.3049421296 | 56375 | 56008.324224537 | 2.7.16.31 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060096 | We propose a 100 ks observation of a recurrent novae remnant RS Ophiuchi. Using Suzaku's wide-energy coverage and excellent spectral performance, we aim to diagnose plasma and to discover non-thermal emission at a recurrent novae remnant. | GALACTIC POINT SOURCES | 4 | C | TAKEI | DAI | NULL | NULL | JAP | 6 | AO6 | OBSERVATION OF A RECURRENT NOVA REMNANT RS OPHIUCHI | XIS | Y | | 1RXSJ013106.4+612035 | 22.7619 | 61.3591 | 127.66105316 | -1.14841945 | 76.8129 | 55765.7032175926 | 55766.0182060185 | 406034010 | 13296.3 | 20000 | 13296.3 | 13296.3 | 0 | 13296.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15882.9 | 15882.9 | 27199.9 | 0 | PROCESSED | 55784.9815740741 | 56374 | 55784.9886458333 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060097 | We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray. | GALACTIC POINT SOURCES | 4 | B | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES | XIS | Y | | 1RXSJ013106.4+612035 | 22.8032 | 61.3371 | 127.68400105 | -1.16712133 | 215.0025 | 55993.5664930556 | 55993.889837963 | 406034020 | 12173.7 | 8000 | 12173.7 | 12173.7 | 0 | 12173.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17897 | 17897 | 27921.9 | 0 | PROCESSED | 56008.1125231482 | 56374 | 56008.1191782407 | 2.7.16.31 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060097 | We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray. | GALACTIC POINT SOURCES | 4 | B | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES | XIS | Y | | 1RXSJ194246.3+103339 | 295.6976 | 10.5399 | 48.24168916 | -6.37340779 | 280.0002 | 55848.1433564815 | 55848.635625 | 406035010 | 20488.9 | 20000 | 20488.9 | 20488.9 | 0 | 20488.9 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 17142 | 17142 | 42508 | 0 | PROCESSED | 55872.9892939815 | 56240 | 55873.0004861111 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060097 | We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray. | GALACTIC POINT SOURCES | 4 | B | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES | XIS | Y | | 1RXSJ135341.1-664002 | 208.4233 | -66.67 | 309.05087215 | -4.54070575 | 288.5314 | 55774.1593055556 | 55774.6939236111 | 406036010 | 23267.9 | 20000 | 23275.9 | 23267.9 | 0 | 23275.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22424.1 | 22424.1 | 46183.9 | 0 | PROCESSED | 55799.4797569444 | 56166 | 55802.4628472222 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 060097 | We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray. | GALACTIC POINT SOURCES | 4 | B | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES | XIS | Y | | HD162020 | 267.6611 | -40.3282 | 350.73095661 | -6.73195128 | 265.867 | 55808.0919560185 | 55808.4078703704 | 406037010 | 15922.9 | 15000 | 15922.9 | 15922.9 | 0 | 15922.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15940.6 | 15940.6 | 27287.9 | 2 | PROCESSED | 55865.1100462963 | 56232 | 55865.1159953704 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | | HD162020 | 267.6612 | -40.3294 | 350.72995016 | -6.73261971 | 268.3343 | 55816.4132291667 | 55816.727962963 | 406037020 | 15036.2 | 15000 | 15044.2 | 15044.2 | 0 | 15036.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15582.9 | 15582.9 | 27183.9 | 0 | PROCESSED | 55848.161400463 | 56218 | 55851.4394444444 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | | HD162020 | 267.6618 | -40.3275 | 350.73183598 | -6.73206134 | 259.9987 | 55824.6498958333 | 55825.1632407407 | 406037030 | 16230 | 15000 | 16238 | 16238 | 0 | 16230 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13378.4 | 13378.4 | 44345.9 | 1 | PROCESSED | 55848.2738194444 | 56218 | 55851.4474884259 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | | HD162020 | 267.6661 | -40.3245 | 350.73610578 | -6.73339029 | 259.9986 | 55833.0255208333 | 55833.4279513889 | 406037040 | 16729.7 | 15000 | 16737.7 | 16737.7 | 0 | 16729.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15728.6 | 15728.6 | 34749.9 | 0 | PROCESSED | 55858.1306597222 | 56225 | 55858.1397453704 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | | HD162020 | 267.6583 | -40.31833 | 350.73847221 | -6.72514943 | -99 | NULL | NULL | 406038010 | -99 | 10000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | | HD162020 | 267.6599 | -40.3316 | 350.72753331 | -6.73286722 | 269.5018 | 55820.4672453704 | 55820.6918634259 | 406038020 | 8896 | 10000 | 8896 | 8896 | 0 | 8896 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7851.9 | 7851.9 | 19399.9 | 0 | PROCESSED | 55848.2500810185 | 56218 | 55851.4444097222 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | | HD162020 | 267.6631 | -40.3218 | 350.73730077 | -6.73005667 | 259.9987 | 55829.424212963 | 55829.6543865741 | 406038030 | 11481 | 10000 | 11481 | 11481 | 0 | 11481 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8540.2 | 8540.2 | 19879.9 | 0 | PROCESSED | 55858.0724768518 | 56225 | 55858.0790162037 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y | | ETA CARINAE | 161.2639 | -59.6881 | 287.59810122 | -0.63296206 | 310.0122 | 55766.0329398148 | 55766.9286226852 | 406039010 | 42030.2 | 50000 | 42030.2 | 42030.2 | 0 | 42030.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 49093.7 | 49093.7 | 77383.9 | 0 | PROCESSED | 55785.0159837963 | 56163 | 55785.0281712963 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061205 | Eta Car is the nearest highly unstable extremely massive star and a key object for understanding how mass and angular momentum change as an extremely massive star heads towards hypernova. Periodic minima in X-rays and other wavebands show it as an extremely eccentric binary with a massive companion. A surprising change in the X-ray emission during the January 2009 X-ray minimum probably indicates a large-scale variation in the LBV primary's mass loss rate. We propose a Suzaku observation in AO6 to monitor the change of the absorption column in the line of sight and the non-thermal emission above 10 keV. The observation will help to study geometry of the binary orbit of Eta Car and the mechanism of the non-thermal emission. | GALACTIC POINT SOURCES | 4 | B | HAMAGUCHI | KENJI | NULL | NULL | USA | 6 | AO6 | MONITORING DYNAMICAL MASS LOSS FROM ETA CAR WITH SUZAKU: APASTRON | XIS | Y | | GAMMA CASSIOPEIAE | 14.1598 | 60.7356 | 123.56796459 | -2.12972511 | 72.5084 | 55755.0038888889 | 55756.333587963 | 406040010 | 55394 | 50000 | 55394 | 55394 | 0 | 55394 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56216.4 | 56216.4 | 114877.8 | 0 | PROCESSED | 55816.6477546296 | 56183 | 55816.6655208333 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061207 | We propose a 50 ks Suzaku observation to obtain for the first time the hard X-ray spectrum of the classical Be star Gamma Cas. This star is a prototype of the "Gamma Cas stars" class, whose nature is not yet understood. Earlier XMM-Newton and Swift BAT observations gave a hint of the presence of the hard X-ray emission above 10 keV. The broadband Suzaku spectrum will allow to establish its X-ray emission mechanism - non-thermal emission or reflection of thermal emission from a neutral surface. On this basis, we will be able to discriminate the mechanisms between the magnetic disk dynamo and the accretion on a compact star. These new data will be pivotal in solving the enigma of Gamma Cas and revealing the true nature of this astrophysically important object. | GALACTIC POINT SOURCES | 4 | C | HAMAGUCHI | KENJI | NULL | NULL | USA | 6 | AO6 | SUZAKU'S HARD LOOK AT GAMMA CASSIOPEIAE | XIS | Y | | 4 DRA | 187.5655 | 69.216 | 125.72551845 | 47.79722512 | 145.5318 | 55874.1707291667 | 55875.0619328704 | 406041010 | 42258 | 40000 | 42258 | 42258 | 0 | 42258 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39792.5 | 39792.5 | 76998 | 2 | PROCESSED | 55890.4815972222 | 56260 | 55890.6961458333 | 2.7.16.31 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061212 | 4 Dra is a weakly symbiotic star that exhibited strong variability in ROSAT observations. Our Suzaku Cycle 5 observation confirms it to be an absorbed hard X-ray source, powered by accretion. It is thus a nearby, lower accretion rate analogue of the hard X-ray bright symbiotic stars such as T CrB and CH Cyg. During Suzaku Cycle 6, 4 Dra is near apastron and near the inferior conjunction of the accreting white dwarf: both these should reduce the absorption due to the M giant, while absorption by the accretion flow near the white dwarf should remain roughly comparable. We therefore propose a second Suzaku observation of 4 Dra to constrain the relative contributions of these two X-ray absorbers, and to obtain a high signal-to-noise spectrum of a symbiotic star boundary layer near 1 keV. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 6 | AO6 | A SUZAKU OBSERVATION OF 4 DRA NEAR INFERIOR CONJUNCTION | XIS | Y | | V1082 SGR | 286.8363 | -20.7721 | 15.88147607 | -12.67535412 | 81.3818 | 56009.1848148148 | 56010.4459375 | 406042010 | 39460.5 | 40000 | 39460.5 | 39460.5 | 0 | 39460.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36017.1 | 36017.1 | 108924 | 2 | PROCESSED | 56023.1382986111 | 88068 | 56023.1564236111 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061217 | V1082 Sgr is a BAT-detected cataclysmic variable with a 20 hr orbital period that exhibits high and low states. The high X-ray luminosity and the presence of the HeII 4686 lines in its optical spectrum have led to the suggestion that this is an intermediate polar (IP). We propose an exploratory 40 ks Suzaku observation with the aim of establishing if it is indeed an IP. If it is, then this system may provide a unique opportunity to study an IP in a low state, which has not been possible with other IPs. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 6 | AO6 | AN UNUSUAL BAT-DETECTED CATACLYSMIC VARIABLE, V1082 SGR | XIS | Y | | AQL X-1 | 287.81687 | 0.58494 | 35.71842844 | -4.14317601 | -99 | NULL | NULL | 406043010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061221 | Long term optical/X-ray monitoring of X-ray binaries has revealed that the accretion flow pattern can be remarkably different during different outbursts of the same source, challenging standard disk-instability models. Of particular interest is the Low-Intensity State (LIS) in Aql X-1, where the optical-to-X-ray flux ratio is about a factor of 7 higher than that during normal outbursts explainable using the disk-instability model. Suzaku data, along with contemporaneous optical/IR and radio observations, will allow probing the nature of accretion flow in the LIS of Aql X-1. We request a 100 ksec ToO observation of Aql X-1 during a LIS to achieve our science goals. The observation will test the predictions of ADIOS models and constrain disk-jet coupling. | GALACTIC POINT SOURCES | 4 | A | MAITRA | DIPANKAR | NULL | NULL | USA | 6 | AO6-TOO | SUZAKU OBSERVATIONS OF AQUILA X-1 DURING ITS LOW-INTENSITY STATE | XIS | N | | SERPENS X-1 | 279.98958 | 5.03583 | 36.11795416 | 4.84231882 | -99 | NULL | NULL | 406044010 | -99 | 250000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061222 | Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries. Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects at the inner accretion disk. But, the nature of these lines is still hotly debated. Recent work has suggested that pile-up can artificially broaden lines, while several narrow lines have been claimed in one source. To address these critical issues, we propose Suzaku and Chandra observations of Serpens X-1. Fast clocking modes will be used to achieve pile-up free spectra. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe line, while the high-resolution gratings spectra from Chandra will reveal any narrow components. | GALACTIC POINT SOURCES | 4 | C | MILLER | JON | NULL | NULL | USA | 6 | AO6 | THE NATURE OF BROAD FE K EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES | XIS | N | | 4U 1624-490 | 247.01179 | -49.1985 | 334.91501997 | -0.26313779 | -99 | NULL | NULL | 406045010 | -99 | 75000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061223 | We propose a 75~ks (on-source, 165~ks total) Suzaku observation of the ``Big Dipper'' 4U~1624-490 to facilitate four important science goals: (1) determine the origin(s) of the persistent X-ray emission, (2) the properties and evolution of the obscuration local to 4U 1624-490, (3) study its broad Fe line properties to determine origin and possibly source geometry, and (4) a large angle scattering study of the X-ray halo to diagnose ISM grain properties (the line-of-sight position, size distribution and density of grains) near us in complement with our work with Chandra on halo studies at small angles to determine grain properties near the source. | GALACTIC POINT SOURCES | 4 | C | XIANG | JINGEN | NULL | NULL | USA | 6 | AO6 | A SUZAKU STUDY OF THE BIG DIPPER 4U 1624-490, AND ITS SCATTERING HALO | XIS | N | | 4U 1954+31 | 298.9334 | 32.0803 | 68.38077131 | 1.91321277 | 261.2562 | 55857.3373263889 | 55858.7203009259 | 406046010 | 60216 | 60000 | 60224 | 60232 | 0 | 60216 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 57900.8 | 57900.8 | 119467.9 | 0 | PROCESSED | 55874.0883796296 | 56241 | 55874.1069328704 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061226 | We propose the first Suzaku observation of a symbiotic X-ray binary 4U 1954+31. This object has an extraordinarily long spin period, ~5 hour, attributed to the neutron star (NS) rotation, making 4U 1954+31 the slowest-rotating accreting NS binary. It raises a question about its binary evolution, since a slowly rotating NS orbiting an M-type giant is quite unique. As to its large variability, the popular clumpy wind model has not yet become a smoking-gun, and we propose an alternative hypothesis that the NS is a magnetar descendent captured by an M-type giant in their closer encounter. Known X-ray properties of 4U~1954+31 will be revisited in a view of gated accretion onto the strongly magnetized NS. A 60 ks Suzaku observation can examine these scenarios. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | USA | 6 | AO6 | THE SLOWEST ROTATING PULSAR 4U 1954+31 | XIS | Y | | 4U1538-522 | 235.59708 | -52.38611 | 327.41949089 | 2.163702 | -99 | NULL | NULL | 406047010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061232 | Observations of accreting pulsars in High Mass X-ray Binaries (HMXBs) provide us with important information about the physical processes in the stellar wind of the high mass donor star, the coupling between the accreting material and the neutron star's magnetic field, and the physics of the strongly magnetized accretion column above the neutron star magnetic poles. In this proposal we request a 40 ks observation of the accreting HMXB 4U1538-522 to conduct the most sensitive study to date of the wide range of changes of the broad band (0.1 -- 100 keV) spectrum with respect to both binary and pulse phases. | GALACTIC POINT SOURCES | 4 | C | ROTHSCHILD | RICHARD | NULL | NULL | USA | 6 | AO6 | THE FIRST SUZAKU OBSERVATION OF 4U 1538-522 | XIS | Y | | 4U 0115+63 | 19.6209 | 63.7559 | 125.91670035 | 1.04099954 | 84.7167 | 55747.0027430556 | 55748.0529976852 | 406048010 | 24279 | 50000 | 24280 | 24279 | 0 | 24283.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45127.2 | 45127.2 | 90727.9 | 1 | PROCESSED | 55777.2688657407 | 56163 | 55778.4298611111 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | Y | | 4U 0115+63 | 19.6139 | 63.7554 | 125.91367385 | 1.04017806 | 82.1235 | 55750.053587963 | 55751.0210763889 | 406049010 | 42274.8 | 45000 | 42274.8 | 42354.8 | 0 | 42354.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42143.2 | 42143.2 | 83577.9 | 1 | PROCESSED | 55777.3219791667 | 56163 | 55778.4311226852 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | Y | | CEP X-4 | 324.878 | 56.98611 | 99.01219478 | 3.31239245 | -99 | NULL | NULL | 406050010 | -99 | 50000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | CEP X-4 | 324.878 | 56.98611 | 99.01219478 | 3.31239245 | -99 | NULL | NULL | 406051010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | XTE J1946+274 | 296.41371 | 27.36539 | 63.20701539 | 1.39576569 | -99 | NULL | NULL | 406052010 | -99 | 50000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | XTE J1946+274 | 296.41371 | 27.36539 | 63.20701539 | 1.39576569 | -99 | NULL | NULL | 406053010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | V 0332+53 | 53.7495 | 53.17319 | 146.05199466 | -2.19402959 | -99 | NULL | NULL | 406054010 | -99 | 50000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | V 0332+53 | 53.7495 | 53.17319 | 146.05199466 | -2.19402959 | -99 | NULL | NULL | 406055010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | MXB 0656-072 | 104.57 | -7.2105 | 220.12826569 | -1.76940259 | -99 | NULL | NULL | 406056010 | -99 | 50000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | MXB 0656-072 | 104.57 | -7.2105 | 220.12826569 | -1.76940259 | -99 | NULL | NULL | 406057010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | 2S 1417-62 | 215.30333 | -62.69833 | 313.02106782 | -1.59841182 | -99 | NULL | NULL | 406058010 | -99 | 65000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061235 | We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES | XIS | N | | GS 1843-02 | 282.07375 | -2.42028 | 30.41972107 | -0.40463814 | -99 | NULL | NULL | 406059010 | -99 | 65000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061235 | We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES | XIS | N | | GX 304-1 | 195.3153 | -61.5986 | 304.10001953 | 1.25086712 | 115.9338 | 55957.437037037 | 55959.1669444444 | 406060010 | 16524.3 | 65000 | 16691.2 | 16524.3 | 0 | 16691.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58712.4 | 58712.4 | 149432.1 | 3 | PROCESSED | 56033.2457407407 | 88068 | 56033.2695023148 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061235 | We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES | XIS | Y | | SAX J2103.5+4545 | 315.89879 | 45.75153 | 87.13025662 | -0.68481282 | -99 | NULL | NULL | 406061010 | -99 | 65000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061235 | We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES | XIS | N | | LSV +44 17 | 70.24717 | 44.53036 | 159.84706366 | -1.27003263 | -99 | NULL | NULL | 406062010 | -99 | 65000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061235 | We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES | XIS | N | | XTE J1550-564 | 237.74458 | -56.47667 | 325.88223339 | -1.82706287 | -99 | NULL | NULL | 406063010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061241 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 6 | AO6-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | N | | 4U 1543-47 | 236.78583 | -47.66944 | 330.91865964 | 5.42579106 | -99 | NULL | NULL | 406064010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061241 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 6 | AO6-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | N | | XTE J1118+480 | 169.54542 | 48.03694 | 157.66026546 | 62.32060029 | -99 | NULL | NULL | 406065010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061241 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 6 | AO6-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | N | | V404 CYG | 306.01596 | 33.86728 | 73.11883543 | -2.09143677 | -99 | NULL | NULL | 406066010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061241 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 6 | AO6-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | N | | A 0620-00 | 95.68542 | -0.34583 | 209.95635423 | -6.53992625 | -99 | NULL | NULL | 406067010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061241 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 6 | AO6-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | N | | GRS 1915+105 | 288.79833 | 10.94556 | 45.36563993 | -0.21936861 | -99 | NULL | NULL | 406068010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 061242 | We propose a 100 ks ToO to observe a soft state of GRS 1915+105 at L<30% L Edd. This ToO will address several important science goals: (1) a measurement of the black hole spin via two independent methods (X-ray continuum fitting and broad iron line analysis), (2) the determination of the accretion disk-corona geometry via studies of fluorescence lines and Compton reflection components, and (3) investigation of the broad-band spectrum for input into photoionization models. | GALACTIC POINT SOURCES | 4 | A | LEE | JULIA | NULL | NULL | USA | 6 | AO6-TOO | MEASURING THE GRS 1915+105 BLACK HOLE SPIN AND BROADBAND CONTINUUM PROPERTIES | XIS | Y | | SGR 1806-20 | 272.1607 | -20.4008 | 10.00344249 | -0.23433657 | 89.0334 | 56010.449837963 | 56012.5314814815 | 406069010 | 70596.4 | 70000 | 70596.4 | 70596.4 | 0 | 70596.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63957.1 | 63957.1 | 179827.9 | 2 | PROCESSED | 56023.2183101852 | 88068 | 56023.2387384259 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 061301 | Recent Suzaku investigations revealed that a broad-band (0.8-70 keV) spectra of known magnetars systematically change depending on their characteristic ages. The hard X-rays of magnetars become weaker but harder for older objects. In order to accomplish this picture, we have to verify that this correlation is rather free from selection effects, and holds even when the sources vary on long time scales. Here we propose a 70 ks observation of SGR 1806-20. If we detect the hard X-rays from this source at a rather intensity, the above correlation will be much reinforced. | GALACTIC POINT SOURCES | 4 | C | ENOTO | TERUAKI | NULL | NULL | USA | 6 | AO6 | VARIABILITY OF HARD X-RAYS FROM MAGNETARS | XIS | Y | | GX 17+2 | 274.0108 | -14.0482 | 16.42401351 | 1.2676957 | 264.7715 | 55853.116099537 | 55855.5287037037 | 406070010 | 6506.9 | 100000 | 6757.2 | 6506.9 | 0 | 6757.2 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 87359.9 | 87359.9 | 208429.7 | 3 | PROCESSED | 55873.2590509259 | 56241 | 55873.2944444445 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 062003 | The behaviour of dense matter in neutron stars remains enigmatic. To probe this requires accurate measurements of neutron star radii and masses. We have recently shown that broad relativistic Fe emission lines in neutron star low-mass X-ray binaries can be used to constrain the neutron star radius. These sources also provide another tool, kHz quasi-periodic oscillations (QPOs). Combining a measurement of the velocity of the gas in the inner disk (from the Fe line) and the frequency of the kHz QPOs provides a method to measure the neutron star mass if kHz QPOs originate at the inner disk. We propose 100 ksec observations of GX 349+2 and GX 17+2 to provide a detailed Fe line profile. Simultaneously, we will also observe with RXTE to detect the kHz QPOs, allowing us to test this technique. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | EUR | 6 | AO6 | EXPLORING THE IRON LINE - KHZ QPO CONNECTION | XIS | Y | | 4U 1543-624 | 236.9719 | -62.5774 | 321.74901084 | -6.34183385 | 299.1939 | 55826.4056828704 | 55827.6217592593 | 406072010 | 49185.1 | 50000 | 49193.1 | 49185.1 | 0 | 49201.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45309.4 | 45309.4 | 105059.9 | 1 | PROCESSED | 55848.3822916667 | 56222 | 55851.4556134259 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 062010 | We propose to observe the ultra-compact X-ray binaries 4U 0614+091 and 4U 1543-624 for 50 ksec each. The aim of these observations is to constrain the inner radius of the accretion disc for both sources using the recently discovered in both sources relativistialy broadened OVIII Ly alpha line at ~0.7 keV. This constrains the radius of the neutron star. The second goal is to constrain the continuum using more physical model than was used in the literature so far. The unique, large energy coverage of Suzaku will enable us to break possible degeneracies between the properties of the broadened lines and the continuum, providing more convidence on the results. | GALACTIC POINT SOURCES | 4 | A | MADEJ | OLIWIA | NULL | NULL | EUR | 6 | AO6 | INVESTIGATING THE ORIGIN OF THE CONTINUUM AND LINE EMISSION IN THE UCXBS 4U 0614+091 AND 4U 1543-624 | XIS | Y | | AX J1818.8-1559 | 274.7184 | -16.0002 | 15.02984997 | -0.2600064 | 265.8517 | 55849.5538888889 | 55852.1474537037 | 406074010 | 95191.2 | 100000 | 99385.9 | 99385.9 | 0 | 95191.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83874.6 | 83874.6 | 224069.9 | 1 | PROCESSED | 55873.9578819445 | 56241 | 55873.993599537 | 2.7.16.30 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 062016 | The Galactic X-ray source AX J1818.8-1559 is a possible new member of the small class of magnetar candidates since a short and soft burst was detected in the 15--100 keV range from this source in 2007 with INTEGRAL. We request a Suzaku pointing of 100 ks in order to carry out a sensitive search for pulsations. This, together with the good quality spectrum, possibly extending in the hard X-ray range, that can be obtained with the Suzaku instruments, will allow us to reveal the nature of AX J1818.8-1559, most likely adding a new member to the small but rapidly increasing family of magnetar candidates | GALACTIC POINT SOURCES | 4 | B | MEREGHETTI | SANDRO | NULL | NULL | EUR | 6 | AO6 | A NEW GALACTIC MAGNETAR CANDIDATE | XIS | Y | | IGR J07193-1233 | 109.83 | -12.556 | 227.26135569 | 0.36077082 | -99 | NULL | NULL | 406075010 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 062017 | The soft gamma repeaters (SGRs) and the Anomalous X-ray pulsars (AXPs) constitute a small class of X-ray sources which are currently believed to host an ultra-magnetized neutron star, or magnetar. Catching new candidates and enlarge the sample of these peculiar objects is vital in two main respects: i) it allows to test further current models for their activity and ii) it will shed light on the (evolutionary) links among magnetars and other classes of isolated neutron stars. The aim of this proposal is to observe with Suzaku the most promising magnetar candidate, IGR J07193-1233, selected among a large number of still unidentified INTEGRAL sources. | GALACTIC POINT SOURCES | 4 | C | PAVAN | LUCIA | NULL | NULL | EUR | 6 | AO6 | CATCHING MAGNETAR CANDIDATES AMONG UNIDENTIFIED INTEGRAL SOURCES WITH SUZAKU | XIS | N | | 4U 1705-44 | 257.2257 | -44.096 | 343.32512852 | -2.33758895 | 104.9955 | 56013.5320486111 | 56016.4231134259 | 406076010 | 100811.2 | 100000 | 100811.2 | 100819.2 | 0 | 100820.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90075.9 | 90075.9 | 249767.7 | 2 | PROCESSED | 56027.1700462963 | 88068 | 56027.2013657407 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 062019 | We propose a ToO Suzaku 100-ks observation of the neutron star X-ray binary 4U 1705-44, to perform a detailed study of its broad-band (0.4-200 keV) X-ray spectrum during a hard state. XIS data will provide important information on the iron K-shell features, and the broad-band spectral capabilities of the HXD will allow to study the hard X-ray spectrum and in particular the Compton reflection bump at 20-50 keV. We plan to fit both the iron features and the reflection bump with a self-consistent model, which will allow to prove (or disprove) a disk origin of the iron line. Moreover the proposed observation will allow to study the correlation between the spectral index of the primary spectrum and the reflection amplitude, which gives important constraints on the geometry of the system. | GALACTIC POINT SOURCES | 4 | A | DI SALVO | TIZIANA | NULL | NULL | EUR | 6 | AO6-TOO | SUZAKU BROAD-BAND OBSERVATION OF 4U 1705-44: PROBING THE DISK ORIGIN OF THE IRON LINE IN THE HARD STATE | XIS | Y | | 4U 0614+091 | 94.28042 | 9.13694 | 200.87736381 | -3.36351731 | -99 | NULL | NULL | 406077010 | -99 | 80000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 067090 | We propose an investigation of the jet from the ultracompact X-ray binary (UCXB) 4U 0614+091 with Suzaku. 4U 0614+091 is one of the 13 UCXBs whose orbital periods (< 1 hour) are determined. By analogy with microquasars, the spectral state of UCXBs would be low/hard, and there is a possibility that UCXBs have jets. Signs of the existence of the jet in 4U 0614+091 from radio and infrared observations are already reported. Existence of the jet can be recognized by a high-sensitivity spectroscopy of the hard X-ray tailing component. If this component is thermal radiation, the origin would be corona with a high temperature. If this is non-thermal radiation, the origin would be the jet. The wide-band observation with Suzaku will clarify what actually happens in the UCXB. | GALACTIC POINT SOURCES | 4 | C | SATO | TAMOTSU | MADEJ | OLIWIA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF THE JET FROM THE ULTRACOMPACT X-RAY BINARY 4U 0614+091 | XIS | N | | IGRJ16479-4514 | 252.0242 | -45.1934 | 340.16807688 | -0.11668459 | 91.5317 | 55980.9438194444 | 55983.5363541667 | 406078010 | 149778.5 | 150000 | 149786.5 | 149778.5 | 0 | 149786.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 154729.5 | 154729.5 | 223981.9 | 0 | PROCESSED | 56062.2569675926 | 88068 | 56062.2788425926 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 068014 | We propose a 100 ks observation of the Supergiant Fast X-ray Transient (SFXT) with the shortest orbital period, the eclipsing IGRJ16479-4514 (3.3 d), with the main aim of probing its X-ray properties along one entire orbital phase with unprecedented sensitivity. The requested net exposure time indeed translates into an observation almost continuously spanning the whole binary system orbit, allowing for the first time an orbital phase resolved investigation of the X-ray emission properties, which will allow us to study the structure of the supergiant companion (its density and ionization state) and to cast light on the outburst mechanism at work in this new class of transients. | GALACTIC POINT SOURCES | 4 | A | SIDOLI | LARA | BODAGHEE | ARASH | EUS | 6 | AO6 | UNVEILING THE MYSTERY OF THE SUPERGIANT FAST X-RAY TRANSIENT WITH THE SHORTEST ORBITAL PERIOD | XIS | Y | | CYG X-1 | 299.59033 | 35.20161 | 71.33499876 | 3.06682766 | -99 | NULL | NULL | 407001010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | CYG X-1 | 299.59033 | 35.20161 | 71.33499876 | 3.06682766 | -99 | NULL | NULL | 407001020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | CYG X-1 | 299.59033 | 35.20161 | 71.33499876 | 3.06682766 | -99 | NULL | NULL | 407001030 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | XTE J1550-564 | 237.74458 | -56.47667 | 325.88223339 | -1.82706287 | -99 | NULL | NULL | 407002010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | XTE J1550-564 | 237.74458 | -56.47667 | 325.88223339 | -1.82706287 | -99 | NULL | NULL | 407002020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | REIS | RUBENS | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | XTE J1550-564 | 237.74458 | -56.47667 | 325.88223339 | -1.82706287 | -99 | NULL | NULL | 407002030 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | GRO J1655-40 | 253.5 | -39.84581 | 344.98161118 | 2.45630442 | -99 | NULL | NULL | 407003010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | GRO J1655-40 | 253.5 | -39.84581 | 344.98161118 | 2.45630442 | -99 | NULL | NULL | 407003020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | GRO J1655-40 | 253.5 | -39.84581 | 344.98161118 | 2.45630442 | -99 | NULL | NULL | 407003030 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | X1630-472 | 248.50458 | -47.39289 | 336.91037296 | 0.25136454 | -99 | NULL | NULL | 407004010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | X1630-472 | 248.50458 | -47.39289 | 336.91037296 | 0.25136454 | -99 | NULL | NULL | 407004020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | X1630-472 | 248.50458 | -47.39289 | 336.91037296 | 0.25136454 | -99 | NULL | NULL | 407004030 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | H1743-322 | 266.25833 | -32.22667 | 357.12592965 | -1.60785557 | -99 | NULL | NULL | 407005010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | H1743-322 | 266.25833 | -32.22667 | 357.12592965 | -1.60785557 | -99 | NULL | NULL | 407005020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | H1743-322 | 266.25833 | -32.22667 | 357.12592965 | -1.60785557 | -99 | NULL | NULL | 407005030 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | N | | NQ GEM | 112.97717 | 24.50306 | 194.63349275 | 19.35254552 | -99 | NULL | NULL | 407006010 | -99 | 30000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 070021 | Hard X-ray emitting symbiotic stars have been identified to emit 6.4 keV iron line with similar equivalent width of the 6.4 keV line of the Galactic Ridge X-ray Emission (GRXE). Only four of such hard X-ray emitting symbiotic stars have been observed with Suzaku. We propose to use Suzaku observations of all the eight newly discovered hard X-ray emitting symbiotic stars to ascertain if they have similar equivalent width of the 6.4 keV line of the GRXE. We will also confirm the emission of hard X-rays above 10 keV using the HXD PIN and use this feature to test for non-thermal emission in these objects. | GALACTIC POINT SOURCES | 4 | C | EZE | ROMANUS | NULL | NULL | JAP | 7 | AO7 | SEARCH FOR 6.4 KEV IRON EMISSION LINE IN THE NEWLY DISCOVERED HARD X-RAY EMITTING SYMBIOTIC STARS | XIS | N | | HEN 3-461 | 159.78625 | -51.40347 | 282.90464688 | 6.25005811 | -99 | NULL | NULL | 407007010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 56018 | NULL | NULL | NULL | NULL | 070021 | Hard X-ray emitting symbiotic stars have been identified to emit 6.4 keV iron line with similar equivalent width of the 6.4 keV line of the Galactic Ridge X-ray Emission (GRXE). Only four of such hard X-ray emitting symbiotic stars have been observed with Suzaku. We propose to use Suzaku observations of all the eight newly discovered hard X-ray emitting symbiotic stars to ascertain if they have similar equivalent width of the 6.4 keV line of the GRXE. We will also confirm the emission of hard X-rays above 10 keV using the HXD PIN and use this feature to test for non-thermal emission in these objects. | GALACTIC POINT SOURCES | 4 | C | EZE | ROMANUS | NULL | NULL | JAP | 7 | AO7 | SEARCH FOR 6.4 KEV IRON EMISSION LINE IN THE NEWLY DISCOVERED HARD X-RAY EMITTING SYMBIOTIC STARS | XIS | N | | MRK 520 | 330.17242 | 10.55219 | 69.39248442 | -34.0304333 | -99 | NULL | NULL | 407014010 | -99 | 80000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070028 | Compton-thick AGNs contribute to the hard X-ray background and are key objects for investigating the cosmological evolution of AGNs. But heavy obscuration under 10 keV, and source misidentification mean that very few sources have been studied in detail. We have developed new infrared and hard X-ray diagnostics of AGN identification, based on which we select one candidate, Mrk 520, which must be very highly obscured and likely Compton-thick. With Suzaku, we will characterize all emission components, not only thermal and scattering components under 10 keV, but also the heavily obscured continuum over 10 keV, and reflection components. | GALACTIC POINT SOURCES | 4 | C | MATSUTA | KEIKO | NULL | NULL | JAP | 7 | AO7 | MRK 520 : A NEW COMPTON-THICK AGN? | XIS | N | | CYG X-1 | 299.59071 | 35.18919 | 71.32454476 | 3.06009128 | -99 | NULL | NULL | 407015010 | -99 | 85000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070030 | We propose to observe Cyg X-1 for 85 ks, utilizing P-sum mode for XIS3. Our aim is to perform shot analysis, which is originally invented by Negoro et al. 1995 with Ginga, and obtain high-quality wide-band spectra for several phases in less than 1 sec; for example, 0.1 sec before the peak, +/- 0.05 sec at the peak, and after the peak. With these spectra, we will quantify changes in five spectral components: hard Comptonization, soft Comptonization, disk emission, Fe-K lines, and reflection. This will be a clue to know long-standing mystery on rapid variability in black holes. | GALACTIC POINT SOURCES | 4 | A | YAMADA | SHINYA | NULL | NULL | JAP | 7 | AO7 | INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1 | XIS | N | | Z CAM | 126.305 | 73.11089 | 141.38213775 | 32.62862284 | -99 | NULL | NULL | 407016010 | -99 | 35000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070038 | Dwarf novae are a subclass of cataclysmic variables, which sometimes show outbursts. In the outbursts, they are considered to emanate disk winds, but observational evidence had been lacking. Recently, our Suzaku observation of Z Cam during a very transition from quiescence to an outburst revealed clear evidence of the disk wind for the first time, and we were able to study characteristics of the disk wind in detail. Z Cam in quiescence, however, has never been observed with high quality instruments. We, therefore, propose an observation of Z Cam in quiescence in order to study entire behavior of the disk wind throughout different phases, combining the existent Suzaku transition phase data and ASCA archival data taken in other phases. | GALACTIC POINT SOURCES | 4 | C | SAITOU | KEI | NULL | NULL | JAP | 7 | AO7 | COMPREHENSIVE STUDY FOR THE DISK WIND OF THE DWARF NOVA Z CAM THROUGH OUTBURST CYCLES WITH AN OBSERVATION IN QUIESCENCE | XIS | N | | V4641 SGR | 274.84013 | -25.40717 | 6.77395378 | -4.7890572 | -99 | NULL | NULL | 407017010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070041 | We propose a 100 ksec Suzaku observation of the Galactic microquasar V4641 Sgr in an outburst. V4641 Sgr has many unique charactersitics: 1)giant X-ray outbursts with fast rise and decay times, 2)violent variability in X-ray and optical bands, and 3)remarkable iron-K disk-line profiles in the X-ray spectrum. However, it is hardly understood due to the poor X-ray coverage which results from its short outburst duration and rapid intensity variations. Hence, we collaborate closely with VSNET, MAXI/GSC, Swift/XRT and Swift/BAT team for a rapid trigger. The moderate energy resolution and wideband energy coverage of Suzaku enable us to clarify the radiation mechanisms of V4641 Sgr. This observation is now planned simultaneously with Swift, many radio and optical/NIR observatories. | GALACTIC POINT SOURCES | 4 | A | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 7 | AO7-TOO | THE LARGEST-EVER CAMPAIGN OF THE GALACTIC MICROQUASAR V4641 SGR | XIS | N | | AX J1622.1-5005 | 245.53333 | -50.095 | 333.60475648 | -0.20613936 | -99 | NULL | NULL | 407018010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070043 | Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 7 | AO7 | ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? | XIS | N | | AX J1846.8-0240 | 281.7182 | -2.6613 | 30.04319345 | -0.19850989 | 89.4057 | 56018.0125115741 | 56019.1146990741 | 407019010 | 37620.9 | 40000 | 37620.9 | 41612.7 | 0 | 39220.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37250 | 37250 | 95219.9 | 0 | PROCESSED | 56033.2221412037 | 88068 | 56033.2323032407 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 070043 | Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 7 | AO7 | ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? | XIS | Y | | AX J1620.7-4942 | 245.19583 | -49.71278 | 333.72073134 | 0.21799808 | -99 | NULL | NULL | 407020010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070043 | Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 7 | AO7 | ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? | XIS | N | | AX J1445.7-5931 | 221.44583 | -59.53167 | 316.97324327 | 0.186216 | -99 | NULL | NULL | 407021010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070043 | Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 7 | AO7 | ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? | XIS | N | | 1FGL J0747.4-3303 | 116.88879 | -33.092 | 248.37397684 | -3.91098782 | -99 | NULL | NULL | 407022010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070051 | We propose to observe two of Fermi/LAT unassociated sourced from 2-year catalog which are located on the Galactic Plane. These two sources are bright in gamma-ray energies and well localized but no counterpart in other wavelength is known so far. We expect to determine which gamma-ray source category the proposed targets belong to, from X-ray morphological and spectral characteristics to be obtained. It will be more interesting that the objects look like known categories since it might mean a discovery of a new class of gamma-ray sources. We hope to promote systematic understandings for the gamma-ray objects in the Galactic Plane. | GALACTIC POINT SOURCES | 4 | C | NAKAMORI | TAKESHI | NULL | NULL | JAP | 7 | AO7 | SEARCH FOR X-RAY COUNTERPARTS FOR FERMI/LAT UNASSOCIATED SOURCES ON THE GALACTIC PLANE | XIS | N | | 1RXSJ171405.2-202747 | 258.52167 | -20.46306 | 3.21688369 | 10.61566491 | -99 | NULL | NULL | 407024010 | -99 | 10000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070052 | We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 7 | AO7 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | N | | 1RXSJ171757.8-332837 | 259.49083 | -33.47694 | 352.96308376 | 2.46029803 | -99 | NULL | NULL | 407025010 | -99 | 12000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070052 | We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 7 | AO7 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | N | | 1RXSJ175219.2-190727 | 268.08 | -19.12417 | 9.20798372 | 3.73361636 | -99 | NULL | NULL | 407026010 | -99 | 12000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070052 | We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 7 | AO7 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | N | | 1RXSJ170047.8-314442 | 255.19917 | -31.745 | 352.21410507 | 6.39819107 | -99 | NULL | NULL | 407027010 | -99 | 12000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070052 | We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 7 | AO7 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | N | | 1RXSJ182853.8-241746 | 277.22417 | -24.29611 | 8.76534346 | -6.19787712 | -99 | NULL | NULL | 407028010 | -99 | 12000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070052 | We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 7 | AO7 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | N | | 1RXSJ173905.2-392615 | 264.77167 | -39.4375 | 350.34867934 | -4.37314858 | -99 | NULL | NULL | 407029010 | -99 | 15000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070052 | We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 7 | AO7 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | N | | 1RXSJ171542.3-243131 | 258.92625 | -24.52528 | 0.04342141 | 8.00113057 | -99 | NULL | NULL | 407030010 | -99 | 15000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070052 | We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 7 | AO7 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | N | | LS 5039 | 276.56275 | -14.84842 | 16.88157018 | -1.28923077 | -99 | NULL | NULL | 407033010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070062 | We propose a 200 ks observation of the gamma-ray binary LS 5039 with Suzaku. Our main aim is to search for pulsation from its compact object. Our analysis of past X-ray data suggests pulsation with parameters typical of magnetars. Addition of new Suzaku data will allow us to confirm the suggested pulsation. If confirmed, the discovery is important both for gamma-ray binary science and for magnetar science. Another aim of the proposed observation is to investigate stability of the X-ray flux and spectral property at each orbital phase. We are particularly interested in testing stability of hour-scale lightcurve structures. New Suzaku data, in combination with the previous data, should provide important clues to understand the emission mechanism. | GALACTIC POINT SOURCES | 4 | C | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 7 | AO7 | REVEALING THE NATURE OF THE COMPACT OBJECT IN LS 5039 | XIS | N | | U GEM IN QUIECSECNCE | 118.77183 | 22.00142 | 199.22315443 | 23.3945234 | -99 | NULL | NULL | 407034010 | -99 | 120000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070065 | It has been believed that the optically thin boundary layer in dwarf novae (DNe) turns into optically thick state in outburst, and, as a result, hard optically thin X-ray emission becomes weaker than in quiescence. This theory was verified in multi-waveband observations of SS Cyg. The DN U Gem, however, does not follow this scenario, and the hard X-ray intensity increases in outburst as well as soft X-ray emission. We propose ToO observations of U Gem both in quiescence and in outburst in order to understand behavior of DNe in X-rays in general, by means of detailed spectroscopy of the soft disk blackbody component, the hard component reflected off the white dwarf, and a 6.4 keV iron line. This study eventually enables us to understand the origin of the Galactic Ridge X-ray Emission. | GALACTIC POINT SOURCES | 4 | B | HAYASHI | TAKAYUKI | NULL | NULL | JAP | 7 | AO7-TOO | OBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURST | XIS | Y | | U GEM IN OUTBURST | 118.7732 | 21.9928 | 199.23241259 | 23.39259554 | 281.117 | 56029.4105324074 | 56030.750162037 | 407035010 | 50254.7 | 50000 | 50254.7 | 50254.7 | 0 | 50254.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47296.7 | 47296.7 | 115707.9 | 1 | PROCESSED | 56044.3683101852 | 88068 | 56044.3887731482 | 2.7.16.32 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 070065 | It has been believed that the optically thin boundary layer in dwarf novae (DNe) turns into optically thick state in outburst, and, as a result, hard optically thin X-ray emission becomes weaker than in quiescence. This theory was verified in multi-waveband observations of SS Cyg. The DN U Gem, however, does not follow this scenario, and the hard X-ray intensity increases in outburst as well as soft X-ray emission. We propose ToO observations of U Gem both in quiescence and in outburst in order to understand behavior of DNe in X-rays in general, by means of detailed spectroscopy of the soft disk blackbody component, the hard component reflected off the white dwarf, and a 6.4 keV iron line. This study eventually enables us to understand the origin of the Galactic Ridge X-ray Emission. | GALACTIC POINT SOURCES | 4 | B | HAYASHI | TAKAYUKI | NULL | NULL | JAP | 7 | AO7-TOO | OBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURST | XIS | Y | | SWIFT J1922.7-1716 | 290.692 | -17.283 | 20.69989276 | -14.55317706 | -99 | NULL | NULL | 407036010 | -99 | 60000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070077 | This proposal aims at a 60 ksec pointing (non time critical) onto the LMXB, Swift J1922.7-1716, which is considered to reside in the hard state. The purpose is to obtain a wide-band spectrum of this object with the XIS, HXD-PIN, and HXD-GSO. The XIS data will allow us to estimate the blackbody radius which underlies the expected Compton hard continuum, while the HXD data can be used to study an enigmatic spectral feature at ~40 keV often seen in this type of sources. Although the source is considered to be relatively bright, the XIS data are expected to be free from pile-up effects. | GALACTIC POINT SOURCES | 4 | C | SAKURAI | SOKI | NULL | NULL | JAP | 7 | AO7 | SUZAKU STUDY OF LOW-MAGNETIC-FIELD NEUTRON STARS VIA THE HARD STATE OF LMXBS | XIS | N | | IGR J17091-3624 | 257.28333 | -36.40667 | 349.52594917 | 2.21189442 | -99 | NULL | NULL | 407037010 | -99 | 120000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070097 | We propose a Suzaku observation of "the second GRS 1915+105" IGR J17091-3624 with a high energy resolution and broadband capability. GRS 1915+105 has been considered to be the unique black hole binary that stays at a high mass accretion rate and shows limit-cycle oscillations, but it was recently discovered that the BHC IGR J17091-3624 has exactly the same X-ray variability patterns as GRS 1915+105. This fact suggests an evidence for common physical mechanism in both system. The Suzaku observation will reveal both similarity and difference with GRS 1915+105 from a point of view of broad-band spectral properties and disk wind, and help us understanding of the accretion flow onto a black hole under a high mass accretion rate. | GALACTIC POINT SOURCES | 4 | B | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 7 | AO7 | SUZAKU BROADBAND OBSERVATION OF "THE SECOND GRS 1915+105" IGR J17091-3624 | XIS | N | | II PEG | 358.76667 | 28.63367 | 108.23244051 | -32.62392433 | -99 | NULL | NULL | 407038010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070102 | We propose a Suzaku observation of the powerful flare star II Peg with the high sensitivity of HXD. MAXI/GSC results from 2009 to 2011 show that this source exhibits the highest flaring activity with the largest luminosities and the largest fluxes. Then detection of the non-thermal emission is the most expected from this source at the on-set of a flare. We are to observe this target simultaneously with radio, infrared, optical, and X-ray bands for the first time. Our goal is (1) to detect impulsive non-thermal emission at the powerful II Peg flare (2) to obtain wide-band SED variability from radio to hard X-ray band, and (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band. | GALACTIC POINT SOURCES | 4 | C | TSUBOI | YOHKO | NULL | NULL | JAP | 7 | AO7 | NON-THERMAL EMISSION ON THE POWERFUL STELLAR FLARE FROM II PEG | XIS | N | | EUVE J1439 +75.0 | 220.02163 | 75.09272 | 114.09811948 | 40.11634493 | -99 | NULL | NULL | 407039010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070112 | The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects. | GALACTIC POINT SOURCES | 4 | B | HARAYAMA | ATSUSHI | NULL | NULL | JAP | 7 | AO7 | SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS | XIS | Y | | PG 1658 +440 | 254.95183 | 44.01775 | 69.12302307 | 38.05451186 | -99 | NULL | NULL | 407040010 | -99 | 50000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 070112 | The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects. | GALACTIC POINT SOURCES | 4 | B | HARAYAMA | ATSUSHI | NULL | NULL | JAP | 7 | AO7 | SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS | XIS | N | | WR140 | 305.11667 | 43.85444 | 80.930231 | 4.1770017 | -99 | NULL | NULL | 407041010 | -99 | 50000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071203 | In the campaign observations of the prototypical colliding wind binary system WR 140 at its last periastron passage in 2009, Suzaku discovered an extremely hard and variable X-ray component. The current best explanation of its origin is inverse-Compton cooling of particles accelerated in the wind-wind collision shock, and if so this would be the first detection of non-thermal X-ray emission from any Wolf-Rayet system. However, other mechanisms cannot be excluded because the observed intensity was stronger than expected from the observed radio luminosity. We propose to re-observe WR 140 near apastron in 2012 with Suzaku to identify the emission mechanism which produces the hard component. | GALACTIC POINT SOURCES | 4 | C | HAMAGUCHI | KENJI | NULL | NULL | USA | 7 | AO7 | MEASURING EXTREMELY HARD X-RAY EMISSION FROM WR140 AT APASTRON | XIS | N | | HEN 3-1591 | 271.88342 | -25.89536 | 5.07306413 | -2.67684889 | -99 | NULL | NULL | 407042010 | -99 | 50000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071211 | The number of symbiotic stars known to be medium energy (2-10 keV) X-ray emitters has increased markedly in the last several years. These are white dwarfs accreting from a giant mass donor, unlike the less common class of symbiotic X-ray binaries in which the accretor is a neutron star. The X-ray spectra of the white dwarf symbiotics can be used to constrain the white dwarf mass and accretion rate. Here we focus on one object, Hen 3-1591, which belongs to a rare subclass of d'-type yellow symbiotic, commonly thought to harbor a young white dwarf. Hen 3-1591 is the first of this subclass to show medium energy X-ray emission, and hence we propose a moderately deep Suzaku observation to characterize its white dwarf and the circum-binary environment. | GALACTIC POINT SOURCES | 4 | B | MUKAI | KOJI | NULL | NULL | USA | 7 | AO7 | THE X-RAY EMISSION OF THE YELLOW SYMBIOTIC STAR, HEN 3-1591 | XIS | N | | CH UMA | 151.75287 | 67.54647 | 142.89508741 | 42.65158931 | -99 | NULL | NULL | 407043010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | Y | | EK TRA | 228.50375 | -65.09306 | 317.22568595 | -6.25656218 | -99 | NULL | NULL | 407044010 | -99 | 70000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | N | | BF ERI | 69.87475 | -4.59961 | 201.03990907 | -31.30067574 | -99 | NULL | NULL | 407045010 | -99 | 30000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | N | | AT ARA | 262.64079 | -46.09947 | 343.85518736 | -6.61951744 | -99 | NULL | NULL | 407046010 | -99 | 30000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | N | | BV CEN | 202.83117 | -54.97597 | 308.68415273 | 7.44968026 | -99 | NULL | NULL | 407047010 | -99 | 30000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | N | | T PYXIDIS | 136.17292 | -32.37986 | 257.20715673 | 9.70672304 | -99 | NULL | NULL | 407048010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071213 | We propose a 100 ks observation of the classical nova remnant in the accreting binary system T Pyxidis using Suzaku. T Pyxidis is a system which causes a cycle of classical nova outbursts in a decade time scale. Shocks might occur in the ejecta, and X-rays were detected from its spatially-resolved expanding shell like a miniature supernova remnant. The immediate purposes of this program are (1) to derive the X-ray flux and luminosity after its last outburst in 2011, (2) to diagnose plasma temperature deeply, and (3) to obtain the second sample of non-thermal X-ray emission from classical nova remnants. The target is a remarkable newly discovered candidate of cosmic-ray acceleration sites, and a successful detection of non-thermal X-rays provides a new view of cosmic-ray origins. | GALACTIC POINT SOURCES | 4 | C | TAKEI | DAI | NULL | NULL | USA | 7 | AO7 | COSMIC-RAYS FROM MINIATURE SUPERNOVA REMNANTS | XIS | N | | AQL X-1 | 287.81687 | 0.58494 | 35.71842844 | -4.14317601 | -99 | NULL | NULL | 407049010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071221 | Long term optical/X-ray monitoring of X-ray binaries has revealed that the accretion flow pattern can be remarkably different during different outbursts of the same source, challenging standard disk-instability models. Of particular interest is the Low-Intensity State (LIS) in Aql X-1, where the optical-to-X-ray flux ratio is about a factor of 8 higher than that during normal outbursts explainable using the disk-instability model. Suzaku data, along with contemporaneous optical/IR and radio observations, will allow probing the nature of accretion flow in the LIS of Aql X-1. We request a 100 ksec ToO observation of Aql X-1 during a LIS to achieve our science goals. The observation will test the predictions of ADIOS models and constrain disk--jet coupling. | GALACTIC POINT SOURCES | 4 | A | MAITRA | DIPANKAR | NULL | NULL | USA | 7 | AO7-TOO | SUZAKU OBSERVATION OF AQUILA X-1 DURING ITS LOW-INTENSITY STATE | XIS | N | | SERPENS X-1 | 279.98983 | 5.036 | 36.1182193 | 4.84217349 | -99 | NULL | NULL | 407050010 | -99 | 250000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071222 | Much recent work has been focused on Fe Kalpha emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the neutron star LMXB, Serpens X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe Kalpha line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe Kalpha | GALACTIC POINT SOURCES | 4 | C | CACKETT | EDWARD | NULL | NULL | USA | 7 | AO7 | THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES | XIS | N | | HERCULES X-1 | 254.45763 | 35.34239 | 58.14908153 | 37.52297277 | -99 | NULL | NULL | 407051010 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071224 | This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. | GALACTIC POINT SOURCES | 4 | B | GREFENSTETTE | BRIAN | NULL | NULL | USA | 7 | AO7 | STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY | XIS | N | | HERCULES X-1 | 254.45763 | 35.34239 | 58.14908153 | 37.52297277 | -99 | NULL | NULL | 407051020 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071224 | This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. | GALACTIC POINT SOURCES | 4 | B | GREFENSTETTE | BRIAN | NULL | NULL | USA | 7 | AO7 | STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY | XIS | N | | HERCULES X-1 | 254.45763 | 35.34239 | 58.14908153 | 37.52297277 | -99 | NULL | NULL | 407051030 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071224 | This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. | GALACTIC POINT SOURCES | 4 | B | GREFENSTETTE | BRIAN | NULL | NULL | USA | 7 | AO7 | STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY | XIS | N | | GX 1+4 | 263.009 | -24.74561 | 1.93703286 | 4.79492907 | -99 | NULL | NULL | 407052010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071225 | We propose to observe GX 1+4 during/after a torque reversal with SUZAKU, as a Target Of Opportunity. The pulse period shows the largest known change in time, with an energy spectrum unusually hard and strong suggestions of having the highest magnetic field of any accreting pulsar. Fermi/GBM monitoring will notify of GX 1+4 changing its current spin-down state. SUZAKU will then measure, for the first time, a detailed wide-band energy spectrum of the source during spin-up. This measurement will provide a unique insight into an event in which the physical mechanism(s) is(are) still poorly understood, in part due to the lack of wide-band spectral studies with sufficient energy resolution during torque reversals. Optical/IR ToO observations from the REM telescope (Chile) will be also triggered. | GALACTIC POINT SOURCES | 4 | A | CAMERO-ARRANZ | ASCENSION | NULL | NULL | USA | 7 | AO7-TOO | TOO OBSERVATIONS OF THE NEUTRON STAR / RED GIANT BINARY SYSTEM GX 1+4 / V2116 OPHIUCHI | XIS | N | | 4U 0115+63 | 19.63292 | 63.74 | 125.92365665 | 1.02574493 | -99 | NULL | NULL | 407053010 | -99 | 50000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071231 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | 4U 0115+63 | 19.63292 | 63.74 | 125.92365665 | 1.02574493 | -99 | NULL | NULL | 407054010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071231 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | CEP X-4 | 324.878 | 56.98611 | 99.01219478 | 3.31239245 | -99 | NULL | NULL | 407055010 | -99 | 50000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071231 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | CEP X-4 | 324.878 | 56.98611 | 99.01219478 | 3.31239245 | -99 | NULL | NULL | 407056010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071231 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | XTE J1946+274 | 296.41371 | 27.36539 | 63.20701539 | 1.39576569 | -99 | NULL | NULL | 407057010 | -99 | 50000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071231 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | XTE J1946+274 | 296.41371 | 27.36539 | 63.20701539 | 1.39576569 | -99 | NULL | NULL | 407058010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071231 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | V 0332+53 | 53.7495 | 53.17319 | 146.05199466 | -2.19402959 | -99 | NULL | NULL | 407059010 | -99 | 50000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071231 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | V 0332+53 | 53.7495 | 53.17319 | 146.05199466 | -2.19402959 | -99 | NULL | NULL | 407060010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071231 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | MXB 0656-072 | 104.57 | -7.2105 | 220.12826569 | -1.76940259 | -99 | NULL | NULL | 407061010 | -99 | 50000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071231 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | MXB 0656-072 | 104.57 | -7.2105 | 220.12826569 | -1.76940259 | -99 | NULL | NULL | 407062010 | -99 | 45000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071231 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | N | | 2S 1417-62 | 215.30333 | -62.69833 | 313.02106782 | -1.59841182 | -99 | NULL | NULL | 407063010 | -99 | 65000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071232 | We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES | XIS | N | | KS 1947+300 | 297.39787 | 30.20883 | 66.09899527 | 2.08357456 | -99 | NULL | NULL | 407064010 | -99 | 65000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071232 | We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES | XIS | N | | SWIFT J1626.6-5156 | 246.651 | -51.94264 | 332.7799243 | -2.00275201 | -99 | NULL | NULL | 407065010 | -99 | 65000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071232 | We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES | XIS | N | | SAX J2103.5+4545 | 315.89879 | 45.75153 | 87.13025662 | -0.68481282 | -99 | NULL | NULL | 407066010 | -99 | 65000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071232 | We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES | XIS | N | | LSV +44 17 | 70.24717 | 44.53036 | 159.84706366 | -1.27003263 | -99 | NULL | NULL | 407067010 | -99 | 65000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071232 | We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 7 | AO7-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES | XIS | N | | 4U1538-522 | 235.59708 | -52.38611 | 327.41949089 | 2.163702 | -99 | NULL | NULL | 407068010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071233 | Observations of accreting pulsars in High Mass X-ray Binaries (HMXBs) provide us with important information about the physical processes in the stellar wind of the high mass donor star, the coupling between the accreting material and the neutron star's magnetic field, and the physics of the strongly magnetized accretion column above the neutron star. In this proposal we ask for a 40 ks observation of the accreting HMXB 4U1538-522 to conduct the most sensitive study to date of the wide range of characteristics of the broad band (0.1-100 keV) spectrum over a quarter of a binary orbit and with pulse phase. When one considers the ~50% duty cycle of Suzaku observations, the proposed observation will yield coverage of a quarter of the binary orbit. | GALACTIC POINT SOURCES | 4 | A | ROTHSCHILD | RICHARD | NULL | NULL | USA | 7 | AO7 | THE FIRST SUZAKU OBSERVATION OF 4U1538-522 | XIS | N | | 1FGL J1018.6-5856 | 154.73175 | -58.94614 | 284.35188181 | -1.6900659 | -99 | NULL | NULL | 407069010 | -99 | 70000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071234 | We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation. | GALACTIC POINT SOURCES | 4 | B | TANAKA | TAKAAKI | NULL | NULL | USA | 7 | AO7 | SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856 | XIS | N | | 1FGL J1018.6-5856 | 154.73175 | -58.94614 | 284.35188181 | -1.6900659 | -99 | NULL | NULL | 407070010 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071234 | We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation. | GALACTIC POINT SOURCES | 4 | B | TANAKA | TAKAAKI | NULL | NULL | USA | 7 | AO7 | SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856 | XIS | N | | 1FGL J1018.6-5856 | 154.73175 | -58.94614 | 284.35188181 | -1.6900659 | -99 | NULL | NULL | 407071010 | -99 | 20000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071234 | We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation. | GALACTIC POINT SOURCES | 4 | B | TANAKA | TAKAAKI | NULL | NULL | USA | 7 | AO7 | SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856 | XIS | N | | CYGNUS X-1 | 299.59042 | 35.20167 | 71.33508842 | 3.06679615 | -99 | NULL | NULL | 407072010 | -99 | 30000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071241 | We propose for a single 30 ks observation of the accreting black hole Cygnus X-1. NuSTAR is an upcoming (to be launched in Spring 2012) hard X-ray (5-80 keV) mission that will plan its schedule to obtain simultaneous coverage of Cyg X-1 with Suzaku. The observations will be used for both science and cross-calibration. The combination of Suzaku and NuSTAR will provide the best measurement of the reflection component, including a relativistically broadened iron line and a hard X-ray excess, and the information will be used to test emission models and constrain the Cyg X-1 accretion geometry. The XIS capabilities to measure the iron line are essential for the science, and the HXD coverage is essential for the cross-calibration. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 7 | AO7 | CYGNUS X-1 WITH SUZAKU AND NUSTAR | XIS | N | | XTE J1118+48 | 169.54542 | 48.03694 | 157.66026546 | 62.32060029 | -99 | NULL | NULL | 407073010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071243 | It has long been known that black hole binaries display distinct spectral states. However, the driving mechanism behind the state transition is still a matter of much debate. The importance of Suzaku in the study of black hole binaries cannot be overemphasised; with a single 40ks Suzaku observation of XTE J1752 223, we found that state transition is not a manifestation of a change in the inner extent of the accretion disk; we confirmed the black hole nature of the central source; and constrained its spin parameter. Here, we propose to build on this success through a single 40ks ToO observation of a black hole transient in outburst during a either the high/soft, intermediate or brighter phases of the low/hard state. | GALACTIC POINT SOURCES | 4 | A | REIS | RUBENS | NULL | NULL | USA | 7 | AO7-TOO | UNDERSTANDING BLACK HOLES: SPIN, DISK PHYSICS AND STATE TRANSITIONS | XIS | N | | XTE J1550-564 | 237.74458 | -56.47669 | 325.88222081 | -1.82707843 | -99 | NULL | NULL | 407074010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071243 | It has long been known that black hole binaries display distinct spectral states. However, the driving mechanism behind the state transition is still a matter of much debate. The importance of Suzaku in the study of black hole binaries cannot be overemphasised; with a single 40ks Suzaku observation of XTE J1752 223, we found that state transition is not a manifestation of a change in the inner extent of the accretion disk; we confirmed the black hole nature of the central source; and constrained its spin parameter. Here, we propose to build on this success through a single 40ks ToO observation of a black hole transient in outburst during a either the high/soft, intermediate or brighter phases of the low/hard state. | GALACTIC POINT SOURCES | 4 | A | REIS | RUBENS | NULL | NULL | USA | 7 | AO7-TOO | UNDERSTANDING BLACK HOLES: SPIN, DISK PHYSICS AND STATE TRANSITIONS | XIS | N | | XTE J1650-500 | 252.504 | -49.96211 | 336.71823399 | -3.42702607 | -99 | NULL | NULL | 407075010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071243 | It has long been known that black hole binaries display distinct spectral states. However, the driving mechanism behind the state transition is still a matter of much debate. The importance of Suzaku in the study of black hole binaries cannot be overemphasised; with a single 40ks Suzaku observation of XTE J1752 223, we found that state transition is not a manifestation of a change in the inner extent of the accretion disk; we confirmed the black hole nature of the central source; and constrained its spin parameter. Here, we propose to build on this success through a single 40ks ToO observation of a black hole transient in outburst during a either the high/soft, intermediate or brighter phases of the low/hard state. | GALACTIC POINT SOURCES | 4 | A | REIS | RUBENS | NULL | NULL | USA | 7 | AO7-TOO | UNDERSTANDING BLACK HOLES: SPIN, DISK PHYSICS AND STATE TRANSITIONS | XIS | N | | XTE J1817-330 | 274.43142 | -33.01881 | 359.81724224 | -7.99556497 | -99 | NULL | NULL | 407076010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071243 | It has long been known that black hole binaries display distinct spectral states. However, the driving mechanism behind the state transition is still a matter of much debate. The importance of Suzaku in the study of black hole binaries cannot be overemphasised; with a single 40ks Suzaku observation of XTE J1752 223, we found that state transition is not a manifestation of a change in the inner extent of the accretion disk; we confirmed the black hole nature of the central source; and constrained its spin parameter. Here, we propose to build on this success through a single 40ks ToO observation of a black hole transient in outburst during a either the high/soft, intermediate or brighter phases of the low/hard state. | GALACTIC POINT SOURCES | 4 | A | REIS | RUBENS | NULL | NULL | USA | 7 | AO7-TOO | UNDERSTANDING BLACK HOLES: SPIN, DISK PHYSICS AND STATE TRANSITIONS | XIS | N | | 4U 1755-33 | 269.666 | -33.8075 | 357.21517442 | -4.87185587 | -99 | NULL | NULL | 407077010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071243 | It has long been known that black hole binaries display distinct spectral states. However, the driving mechanism behind the state transition is still a matter of much debate. The importance of Suzaku in the study of black hole binaries cannot be overemphasised; with a single 40ks Suzaku observation of XTE J1752 223, we found that state transition is not a manifestation of a change in the inner extent of the accretion disk; we confirmed the black hole nature of the central source; and constrained its spin parameter. Here, we propose to build on this success through a single 40ks ToO observation of a black hole transient in outburst during a either the high/soft, intermediate or brighter phases of the low/hard state. | GALACTIC POINT SOURCES | 4 | A | REIS | RUBENS | NULL | NULL | USA | 7 | AO7-TOO | UNDERSTANDING BLACK HOLES: SPIN, DISK PHYSICS AND STATE TRANSITIONS | XIS | N | | GX 339-4 | 255.70625 | -48.78972 | 338.9393589 | -4.32669914 | -99 | NULL | NULL | 407078010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071244 | Due to the presence of a steady jet, constraining the properties of black hole systems in their canonical hard state is important for understanding accretion disks and jets. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? This proposal includes the use of Suzaku, the upcoming NuSTAR mission, and radio observations to answer these questions. | GALACTIC POINT SOURCES | 4 | B | TOMSICK | JOHN | NULL | NULL | USA | 7 | AO7-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | N | | 4U 1543-47 | 236.78583 | -47.66944 | 330.91865964 | 5.42579106 | -99 | NULL | NULL | 407079010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071244 | Due to the presence of a steady jet, constraining the properties of black hole systems in their canonical hard state is important for understanding accretion disks and jets. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? This proposal includes the use of Suzaku, the upcoming NuSTAR mission, and radio observations to answer these questions. | GALACTIC POINT SOURCES | 4 | B | TOMSICK | JOHN | NULL | NULL | USA | 7 | AO7-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | N | | V404 CYG | 306.01596 | 33.86728 | 73.11883543 | -2.09143677 | -99 | NULL | NULL | 407080010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071244 | Due to the presence of a steady jet, constraining the properties of black hole systems in their canonical hard state is important for understanding accretion disks and jets. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? This proposal includes the use of Suzaku, the upcoming NuSTAR mission, and radio observations to answer these questions. | GALACTIC POINT SOURCES | 4 | B | TOMSICK | JOHN | NULL | NULL | USA | 7 | AO7-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | N | | 1E 1547.0-5408 | 237.72546 | -54.30658 | 327.23698364 | -0.1315599 | -99 | NULL | NULL | 407081010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071301 | Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | USA | 7 | AO7-TOO | DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? | XIS | N | | 1E 1547.0-5408 | 237.72546 | -54.30658 | 327.23698364 | -0.1315599 | -99 | NULL | NULL | 407081020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071301 | Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | USA | 7 | AO7-TOO | DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? | XIS | N | | SGR 0501+4516 | 75.28333 | 45.27528 | 161.54955797 | 1.95129634 | -99 | NULL | NULL | 407082010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071301 | Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | USA | 7 | AO7-TOO | DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? | XIS | N | | SGR 0501+4516 | 75.28333 | 45.27528 | 161.54955797 | 1.95129634 | -99 | NULL | NULL | 407082020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071301 | Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | USA | 7 | AO7-TOO | DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? | XIS | N | | SGR 1806-20 | 272.16383 | -20.41097 | 9.99597117 | -0.24183424 | -99 | NULL | NULL | 407083010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071301 | Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | USA | 7 | AO7-TOO | DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? | XIS | N | | SGR 1806-20 | 272.16383 | -20.41097 | 9.99597117 | -0.24183424 | -99 | NULL | NULL | 407083020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071301 | Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | USA | 7 | AO7-TOO | DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? | XIS | N | | SWIFT J1822-1606 | 275.575 | -16.07411 | 15.35266129 | -1.02094777 | -99 | NULL | NULL | 407084010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071301 | Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | USA | 7 | AO7-TOO | DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? | XIS | N | | SWIFT J1822-1606 | 275.575 | -16.07411 | 15.35266129 | -1.02094777 | -99 | NULL | NULL | 407084020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071301 | Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | USA | 7 | AO7-TOO | DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? | XIS | N | | SWIFT J1834.9-0846 | 278.71717 | -8.76556 | 23.24974475 | -0.34100673 | -99 | NULL | NULL | 407085010 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071301 | Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | USA | 7 | AO7-TOO | DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? | XIS | N | | SWIFT J1834.9-0846 | 278.71717 | -8.76556 | 23.24974475 | -0.34100673 | -99 | NULL | NULL | 407085020 | -99 | 40000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 071301 | Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | USA | 7 | AO7-TOO | DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? | XIS | N | | LMC X-3 | 84.73596 | -64.08425 | 273.57643041 | -32.08143715 | -99 | NULL | NULL | 407086010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 072002 | We propose a 100 ksec triggered Suzaku observation of the low/hard state of the black hole LMC X-3. This will constrain the disc emission and Fe line profile in this state, both of which are currently very controversial. LMC X-3 has very low interstellar absorption, so gives the best view of the low temperature/low luminosity disc component in this state. Its moderate flux means it can be observed in standard imaging modes without pileup (further enhancing visibility of the disc as these modes are well calibrated down to 0.4 keV) and making the Fe line profile analysis straightforward. Historically LMC X-3 enters a low/hard state on average once a year. Suzaku will be triggered based on an alert from our Swift monitoring program that the source has entered the low/hard state. | GALACTIC POINT SOURCES | 4 | A | KOLEHMAINEN | MARI | NULL | NULL | EUR | 7 | AO7-TOO | A TOO OF LMC X-3: IS THE DISC TRUNCATED IN THE LOW/HARD STATE OF BLACK HOLE BINARIES? | XIS | N | | MWC 560 | 111.46371 | -7.73558 | 223.75985215 | 4.04625645 | -99 | NULL | NULL | 407087010 | -99 | 60000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 072003 | Although jets are ubiquitous and important components in many different astrophysical systems, their formation remains very poorly understood. The pole-on jet in the symbiotic system MWC 560 serves as a Rosetta Stone for understanding pulsed, highly collimated, jets. We propose to use Suzaku for X-ray observations of the symbiotic star MWC 560. It provides us with a unique opportunity to observe the launch site of the jet, the shock-induced propagation of the jet, and its end point, where the ejecta merge into the jet head. We detected with XMM a hard component from the accretion site and a soft component associated with the jet. Further observations are required for solving questions concerning the accretion process and for characterizing the soft component. | GALACTIC POINT SOURCES | 4 | C | STUTE | MATTHIAS | NULL | NULL | EUR | 7 | AO7 | CATCHING A SYMBIOTIC STAR'S PULSED JET IN THE ACT: X-RAY OBSERVATIONS OF MWC560 | XIS | N | | 4U 0352+30 | 58.06325 | 30.9 | 162.65863605 | -17.69224618 | -99 | NULL | NULL | 407088010 | -99 | 150000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 072011 | After 40 years of studies, surprisingly little is known about accreting pulsars at low-luminosities, yet these may be the most numerous class of neutron star binaries in the Galaxy. Upcoming large-scale surveys will likely reveal many such objects, but to identify them it is crucial to fully understand their properties. X Per, the archetypal source of this class, at 1 kpc from Earth is ideal target for detailed studies. In spite of that X Per is still puzzling. With the proposed program we aim to study X Per in detail, constrain its X-ray spectrum also as a function of the spin phase. Our study will be key to characterize the properties of low-luminosity X-ray pulsars population and will help to identify it in upcoming surveys. | GALACTIC POINT SOURCES | 4 | B | DOROSHENKO | VICTOR | NULL | NULL | EUR | 7 | AO7 | CRACKING THE X PER | XIS | N | | EXO 2030+375 | 308.06367 | 37.63747 | 77.15188826 | -1.24180491 | -99 | NULL | NULL | 407089010 | -99 | 75000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 072013 | We propose to observe the Be/X-ray binary system EXO 2030+375 in the ascending part of one of its normal periastron flares for 75ks to study the onset of the pulsar activity. Quasi-periodic hour-long flux oscillations were recently observed during INTEGRAL serendipitous observations and by EXOSAT in 1985. They appear to happen at the viscous time-scale of a disk, evidencing some kind of instability in the transition zone between the magnetosphere and the accretion disk. The broad-band coverage and sensitivity of Suzaku will allow us to investigate in detail the opening of the magnetic gate for this high-magnetic field neutron star by studying the high time resolution light curve, the shape of its pulsed signal and the spectral properties. | GALACTIC POINT SOURCES | 4 | A | FERRIGNO | CARLO | NULL | NULL | EUR | 7 | AO7 | UNVEIL ACCRETION ONSET DURING A NORMAL OUTBURST OF EXO 2030+375 | XIS | Y | | 4U 1705-44 | 257.22696 | 17.14847 | 37.83631459 | 30.1547389 | -99 | NULL | NULL | 407090010 | -99 | 100000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 072015 | We propose a ToO Suzaku 100-ks observation of the neutron star X-ray binary 4U 1705-44, to perform a detailed study of its broad-band (0.4-200 keV) X-ray spectrum during a hard state. XIS data will provide important information on the iron K-shell features, and the broad-band spectral capabilities of the HXD will allow to study the hard X-ray spectrum and in particular the Compton reflection bump at 20-50 keV. We plan to fit both the iron features and the reflection bump with a self-consistent model, which will allow to prove (or disprove) a disk origin of the iron line. Moreover the proposed observation will allow to study the correlation between the spectral index of the primary spectrum and the reflection amplitude, which gives important constraints on the geometry of the system. | GALACTIC POINT SOURCES | 4 | A | DI SALVO | TIZIANA | NULL | NULL | EUR | 7 | AO7-TOO | SUZAKU BROAD-BAND OBSERVATION OF 4U 1705-44: PROBING THE DISK ORIGIN OF THE IRON LINE IN THE HARD STATE | XIS | N | | J1620-4927 | 245.17275 | -49.46006 | 333.8881362 | 0.4079132 | -99 | NULL | NULL | 407091010 | -99 | 25000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 072019 | The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. | GALACTIC POINT SOURCES | 4 | A | MARELLI | MARTINO | NULL | NULL | EUR | 7 | AO7 | SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS | XIS | N | | J1803-2149 | 270.78992 | -21.81519 | 8.14453694 | 0.19016071 | -99 | NULL | NULL | 407092010 | -99 | 25000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 072019 | The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. | GALACTIC POINT SOURCES | 4 | A | MARELLI | MARTINO | NULL | NULL | EUR | 7 | AO7 | SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS | XIS | N | | J1746-3239 | 266.72867 | -32.66517 | 356.95743439 | -2.1748349 | -99 | NULL | NULL | 407093010 | -99 | 25000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 072019 | The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. | GALACTIC POINT SOURCES | 4 | A | MARELLI | MARTINO | NULL | NULL | EUR | 7 | AO7 | SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS | XIS | N | | J1522-5734 | 230.52229 | -57.58311 | 322.05253936 | -0.41511189 | -99 | NULL | NULL | 407094010 | -99 | 25000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 072019 | The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. | GALACTIC POINT SOURCES | 4 | A | MARELLI | MARTINO | NULL | NULL | EUR | 7 | AO7 | SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS | XIS | N | | 4U 1735-44 | 264.74292 | -44.45 | 346.05430491 | -6.99387213 | -99 | NULL | NULL | 407095010 | -99 | 60000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 072024 | We propose to observe the bursting low-mass X-ray binary 4U~1735-44 with Suzaku for a total exposure time of 60 ks. We plan to investigate the broad-band X-ray spectrum, performing a detailed spectroscopic and timing analysis in the energy range 0.4-100 keV. The main scientific aims of this observation are to study the iron line at 6.4-7 keV simultaneously with the expected iron edge, to detect other emission lines at lower energy, and either a Compton reflection hump at 20-40 keV or a hard tail at energy above 25 keV (depending of the state of the source) thanks to the broad-band capabilities of Suzaku. This will allow us to increase the sample of broad iron lines in neutron star X-ray binaries, and above all, to infer and probe the origin of these components, which is still debated. | GALACTIC POINT SOURCES | 4 | C | EGRON | ELISE | NULL | NULL | EUR | 7 | AO7 | BROAD BAND SPECTRAL ANALYSIS AND STUDY OF THE DISK REFLECTION COMPONENT IN 4U 1735-44 WITH SUZAKU | XIS | N | | 1FGL J1018.6-5856 | 154.73208 | -58.94356 | 284.35060516 | -1.68781714 | -99 | NULL | NULL | 407096010 | -99 | 60000 | -99 | -99 | -99 | -99 | NULL | NULL | NULL | NULL | NULL | -99 | -99 | -99 | -99 | -99 | NULL | NOTPROCESSED | NULL | 88068 | NULL | NULL | NULL | NULL | 073113 | Recently, a modulated signal has been detected with the Fermi from the source 1FGL J1018.6-5856. The presence of a O-type star in this source, and the variable character of the signal suggested that the source is a new gamma-ray binary system. Since it is expected that X-rays in these sources has the synchrotron origin, detailed X-ray observations are very important for understanding of the processes occurring in the system. However, sensitive observations of source in the X-ray energy bands are still missing. Therefore, we propose to observe the source with Suzaku. Since a long observational campaign is planned for 2012 by the HESS collaboration, the obtained X-ray, together with TeV, data will allow a proper modeling of the physical processes behind the non-thermal emission in system. | GALACTIC POINT SOURCES | 4 | B | ODAKA | HIROKAZU | TANAKA | TAKAAKI | JUS | 7 | AO7 | X-RAY OBSERVATION OF GAMMA-RAY BINARY 1FGL J1018.6-5856 | XIS | N | | BULGE 3 | 274.7046 | -31.4846 | 1.3002625 | -7.49777303 | 80.4025 | 53800.3437962963 | 53801.7474421296 | 500001010 | 51846.8 | 50000 | 51854.8 | 51854.8 | 51854.8 | 51846.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45078.3 | 45078.3 | 121245.9 | 0 | PROCESSED | 54325.1603935185 | 54247 | 54041.7128703704 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001014 | Leading . | GALACTIC DIFFUSE EMISSION | 5 | A | MCCAMMON | DAN | NULL | NULL | JAP | 0 | SWG | THE SOFT GALACTIC BULGE | XIS | N | | BULGE 2 | 270.6176 | -29.5847 | 1.30042786 | -3.49803376 | 83.2679 | 53801.7493981482 | 53802.0689699074 | 500002010 | 13028 | 10000 | 13052 | 13044 | 13036 | 13028 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 10674.1 | 10674.1 | 27599.9 | 1 | PROCESSED | 54320.5751273148 | 54247 | 54041.664525463 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001014 | Leading . | GALACTIC DIFFUSE EMISSION | 5 | A | MCCAMMON | DAN | NULL | NULL | JAP | 0 | SWG | THE SOFT GALACTIC BULGE | XIS | N | | BULGE 6 | 282.6839 | -33.8925 | 1.99857856 | -14.59644221 | 88.3467 | 53802.7373032407 | 53803.0466087963 | 500003010 | 14261.7 | 10000 | 14261.7 | 14261.7 | 14261.7 | 14261.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 11414 | 11414 | 26715.9 | 1 | PROCESSED | 54320.5876041667 | 54247 | 54041.7424305556 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001014 | Leading . | GALACTIC DIFFUSE EMISSION | 5 | A | MCCAMMON | DAN | NULL | NULL | JAP | 0 | SWG | THE SOFT GALACTIC BULGE | XIS | N | | RCW86 SW | 220.2761 | -62.6782 | 315.14426109 | -2.43598628 | 109.6929 | 53778.0961689815 | 53780.2814699074 | 500004010 | 100765.9 | 100000 | 100781.9 | 100765.9 | 100781.9 | 100781.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 90681.9 | 90681.9 | 188791.8 | 2 | PROCESSED | 54330.3924537037 | 54247 | 54041.2835648148 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001019 | The supernova remnants (SNRs) are most convincing candidates for the acceleration of cosmic-rays. Together with the TeV gamma-ray detection by CANGAROO and HESS, it is now confirmed that at least some of the SNRs can actually accelerate electrons up to > 10 TeV. However, such studies have not provided direct information on ``protons'', which is the major component of cosmic-rays. Here we propose to measure spatial distribution of accelerated protons in the shell of RCW 86, and its association with the high energy (>10 TeV) electrons which emit synchrotron X-rays up to 50 keV. Large effective area and the good detection capability of Suzaku will be ideal tools for our scientific goal. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 0 | SWG | THE FIRST DIRECT MAPPING OF ACCELERATED PROTONS IN THE SW SHELL OF RCW 86 | XIS | N | | GC CENTER #2 | 266.7693 | -28.6295 | 0.42794484 | -0.11339991 | 74.7707 | 53821.958587963 | 53823.7585069444 | 500005010 | 88424.7 | 100000 | 88432.7 | 88424.7 | 88432.7 | 88432.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 64591.1 | 64591.1 | 155501.9 | 2 | PROCESSED | 54328.6633796296 | 54247 | 54133.0079861111 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001020 | We propose to obtain high quality spectrum near the GC. The objective is to resolve 6.4, 6.7, and 6.9 keV line and determine the high energy tail and sub-structures, which may be X-ray reflection from Sgr A* (6.4 keV line + 7.1 keV edge + high energy tail), thermal plasma (6.7 + 6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 0 | SWG | SUZAKU GALACTIC CENTER OBSERVATION PROJECT: #2 SGR B1 | NULL | N | | SN 1987A | 83.8361 | -69.2786 | 279.71542477 | -31.94667609 | 132.5904 | 53677.835775463 | 53678.3475 | 500006010 | 36786.3 | 40000 | 36786.3 | 36786.3 | 36786.3 | 36786.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32919.8 | 32919.8 | 44166.1 | 1 | PROCESSED | 54326.9673726852 | 54247 | 54037.1281481482 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001028 | SN1987A is providing us with a unique opportunity to study the supernova explosion itself and the very early phase of the supernova-remnants evolution. The supernova blast wave has started to strike the inner circumstellar ring. The neutrino flash observed at the time of explosion implies the formation of a neutron star, but no evidence of this has been detected yet. We propose to observe SN1987A for 40 ksec with Suzaku HXD and XIS. Our first goal is the search for a periodic hard signal from the putative pulsar. We also want to study the collision of the supernova blast wave with the inner ring. In order to follow the temporal evolution of the shock, we propose to observe the source with Suzaku in the early phase of the SWG PV-phase as a reference for further studies. | GALACTIC DIFFUSE EMISSION | 5 | A | HASINGER | GUENTHER | NULL | NULL | JAP | 0 | SWG | SUZAKU OBSERVATION OF SN1987A : SEARCH FOR PULSAR EMISSION AND STUDY OF A NEWBORN SNR | NULL | N | | HESS J1804-216 | 271.1693 | -21.6722 | 8.44223916 | -0.04647489 | 89.0483 | 53831.6120138889 | 53832.4919328704 | 500007010 | 37522.2 | 50000 | 37522.2 | 37522.2 | 37522.2 | 37522.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28933.6 | 28933.6 | 75990.1 | 0 | PROCESSED | 54322.9283217593 | 54247 | 54042.288900463 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001029 | HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 0 | SWG | SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS'' | XIS | N | | HESS J1804-216 BGD | 270.9564 | -22.0176 | 8.04431311 | -0.04388906 | 89.2004 | 53832.4925462963 | 53833.454375 | 500008010 | 40717.1 | 50000 | 40717.1 | 40717.1 | 40717.1 | 40717.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30642.9 | 30642.9 | 83087.9 | 1 | PROCESSED | 54327.1449652778 | 54247 | 54056.4266666667 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001029 | HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 0 | SWG | SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS'' | XIS | N | | GALACTIC RIDGE | 281.0049 | -4.0776 | 28.45801897 | -0.21166151 | 265.5297 | 53671.1112037037 | 53673.8960069445 | 500009010 | 93327.6 | 100000 | 93343.6 | 93359.6 | 93343.6 | 93327.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 77536.4 | 77536.4 | 240575.9 | 0 | PROCESSED | 54331.0101967593 | 54247 | 54037.6929513889 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001042 | We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field. | GALACTIC DIFFUSE EMISSION | 5 | A | EBISAWA | KEN | NULL | NULL | JAP | 0 | SWG | ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION | NULL | N | | GALACTIC RIDGE | 281.0036 | -4.078 | 28.45707071 | -0.21069081 | 265.5303 | 54023.0938888889 | 54025.8141087963 | 500009020 | 98858.3 | 100000 | 98874.3 | 98866.3 | 98858.3 | 98874.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 81951.9 | 81951.9 | 235013.9 | 1 | PROCESSED | 54330.1000115741 | 54697 | 54055.6082407407 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001042 | We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field. | GALACTIC DIFFUSE EMISSION | 5 | A | EBISAWA | KEN | NULL | NULL | JAP | 0 | SWG | ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION | XIS | Y | | RXJ_0852-4622_NW | 132.2926 | -45.6157 | 265.39238743 | -1.14402175 | 137.763 | 53723.4478240741 | 53727.3016666667 | 500010010 | 175453 | 150000 | 175453 | 175525 | 175460.8 | 175461 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 230002.5 | 230002.5 | 332943.7 | 7 | PROCESSED | 54331.9048263889 | 54247 | 54059.902662037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001048 | We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | JAP | 0 | SWG | HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622 | HXD | N | | RXJ_0852-4622_NW_offset | 135.1284 | -47.9102 | 268.39892579 | -1.13950817 | 140.267 | 53727.3040393518 | 53728.368912037 | 500010020 | 59178.4 | 50000 | 59178.4 | 59192.5 | 59202.6 | 59192.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 63482.1 | 63482.1 | 91995.9 | 0 | PROCESSED | 54327.312962963 | 54247 | 54039.2486226852 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001048 | We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | JAP | 0 | SWG | HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622 | HXD | N | | SMC DIFFUSE 1 | 13.0188 | -72.8206 | 302.86615918 | -44.30756989 | 221.6864 | 53687.4452893518 | 53688.2231944445 | 500011010 | 46778.9 | 50000 | 46778.9 | 46786.9 | 46786.9 | 46786.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 47868.4 | 47868.4 | 67199.9 | 0 | PROCESSED | 54322.7758449074 | 54247 | 54038.3531712963 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001049 | We propose to use Suzaku XIS to observe regions of diffuse emission in the Magellanic Clouds. The diffuse component was identified by ROSAT PSPC observations, but has never been studied with a true spectroscopic instrument. Suzaku is well-matched to the angular size and expected temperature of the regions of diffuse emission in the LMC. Not only will such observations give a clear view of the temperature structure of this gas, they will provide a direct measurement of ambient abundances in the Clouds. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | JAP | 0 | SWG | DIFFUSE EMISSION IN THE MAGELLANIC CLOUDS | XIS | N | | 73P/SW3 | 279.2884 | 33.5067 | 62.26395264 | 17.33399104 | 47.3721 | 53862.3946875 | 53862.4794444444 | 500012010 | 3250 | 5000 | 3250 | 3250 | 3250 | 3250 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2313.9 | 2313.9 | 7304 | 0 | PROCESSED | 54320.6031944444 | 54256 | 54042.1755671296 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 279.6627 | 33.4734 | 62.35168426 | 17.03145652 | 46.5564 | 53862.4804282407 | 53862.5419444444 | 500012020 | 3248 | 5000 | 3248 | 3248 | 3248 | 3248 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2111.9 | 2111.9 | 5279.9 | 0 | PROCESSED | 54320.4688078704 | 54256 | 54042.2282175926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 316.717 | 24.6807 | 71.53645371 | -15.07849931 | 72.7087 | 53868.1752314815 | 53868.2085532407 | 500013010 | 2353 | 20000 | 2353 | 2353 | 2353 | 2353 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2595 | 2595 | 2871.9 | 0 | PROCESSED | 54320.6021064815 | 54256 | 54042.2312268518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 317.1042 | 24.5187 | 71.64340536 | -15.45205291 | 72.7099 | 53868.2091666667 | 53868.2752199074 | 500013020 | 3225 | 20000 | 3225 | 3225 | 3225 | 3225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3467 | 3467 | 5703.9 | 0 | PROCESSED | 54320.4892361111 | 54256 | 54042.2634027778 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 317.5094 | 24.3437 | 71.75290875 | -15.84652301 | 72.7094 | 53868.2758333333 | 53868.3418865741 | 500013030 | 3225 | 20000 | 3225 | 3225 | 3225 | 3225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2915 | 2915 | 5703.9 | 0 | PROCESSED | 54320.6158796296 | 54256 | 54042.2712731482 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 317.9167 | 24.1666 | 71.86402338 | -16.24383714 | 72.7109 | 53868.3425 | 53868.4085532407 | 500013040 | 3225 | 20000 | 3225 | 3225 | 3225 | 3225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2677 | 2677 | 5703.9 | 0 | PROCESSED | 54320.4917708333 | 54256 | 54042.2977430556 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 318.3252 | 23.9905 | 71.97868305 | -16.64134569 | 72.7093 | 53868.4091666667 | 53868.4752199074 | 500013050 | 3225 | 20000 | 3225 | 3225 | 3225 | 3225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2584 | 2584 | 5703.9 | 0 | PROCESSED | 54320.6176851852 | 54256 | 54089.4348611111 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 318.7382 | 23.8104 | 72.09504522 | -17.04458663 | 72.7096 | 53868.4758333333 | 53868.5418865741 | 500013060 | 3218 | 20000 | 3218 | 3218 | 3218 | 3218 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2539 | 2539 | 5695.9 | 0 | PROCESSED | 54320.492349537 | 54256 | 54042.3000462963 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 319.1503 | 23.6322 | 72.21442919 | -17.44595626 | 72.7095 | 53868.5425 | 53868.6085532407 | 500013070 | 3062.4 | 20000 | 3062.4 | 3062.4 | 3062.4 | 3062.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2088 | 2088 | 5688 | 1 | PROCESSED | 54320.614375 | 54256 | 54042.3037268518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 319.575 | 23.4516 | 72.3420597 | -17.8575616 | 72.7092 | 53868.609212963 | 53868.6738310185 | 500013080 | 3164.4 | 20000 | 3164.4 | 3164.4 | 3164.4 | 3164.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2986 | 2986 | 5551.9 | 0 | PROCESSED | 54320.4853472222 | 54256 | 54042.3213657407 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 18.4857 | -9.3839 | 140.65827116 | -71.47693301 | 59.4008 | 53893.6903703704 | 53893.7356365741 | 500014010 | 3228 | 35000 | 3228 | 3228 | 3228 | 3228 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3312 | 3312 | 3903.9 | 0 | PROCESSED | 54320.6211689815 | 54267 | 54052.5070949074 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 17.8447 | -9.1515 | 138.54867442 | -71.41609802 | 59.3994 | 53893.7363888889 | 53893.8023032407 | 500014020 | 3236.9 | 35000 | 3236.9 | 3236.9 | 3236.9 | 3236.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2478 | 2478 | 5687.9 | 0 | PROCESSED | 54320.6365740741 | 54267 | 54052.5079861111 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 17.8996 | -9.1693 | 138.7272506 | -71.42013328 | 59.3998 | 53893.8025 | 53893.8689699074 | 500014030 | 3236.1 | 35000 | 3236.1 | 3236.1 | 3236.1 | 3236.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2433.1 | 2433.1 | 5735.9 | 0 | PROCESSED | 54320.6368634259 | 54267 | 54052.5088310185 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 17.9545 | -9.1915 | 138.90931762 | -71.42827213 | 59.4015 | 53893.8691666667 | 53893.9356365741 | 500014040 | 3236 | 35000 | 3236 | 3236 | 3236 | 3236 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2490.9 | 2490.9 | 5735.9 | 0 | PROCESSED | 54320.5128356482 | 54267 | 54052.5308912037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 18.0085 | -9.2093 | 139.0853548 | -71.43220951 | 59.4015 | 53893.9358333333 | 53894.0023032407 | 500014050 | 3235 | 35000 | 3235 | 3235 | 3235 | 3235 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2504.1 | 2504.1 | 5735.9 | 0 | PROCESSED | 54320.5147106482 | 54267 | 54052.5317361111 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 18.0599 | -9.2267 | 139.25333623 | -71.43625621 | 59.4006 | 53894.0025 | 53894.0689699074 | 500014060 | 3235 | 35000 | 3235 | 3235 | 3235 | 3235 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2490 | 2490 | 5735.9 | 0 | PROCESSED | 54320.6379398148 | 54267 | 54052.5346759259 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 18.1094 | -9.2436 | 139.41528011 | -71.44015907 | 59.3996 | 53894.0691666667 | 53894.1356365741 | 500014070 | 2220.9 | 35000 | 2220.9 | 2220.9 | 2220.9 | 2220.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1939 | 1939 | 5735.9 | 1 | PROCESSED | 54320.6268634259 | 54267 | 54052.5472800926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 18.1606 | -9.2654 | 139.58635244 | -71.44823165 | 59.3999 | 53894.1358333333 | 53894.2085416667 | 500014080 | 1863.7 | 35000 | 1863.7 | 1863.7 | 1863.7 | 1863.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 1921.2 | 1921.2 | 6277.9 | 0 | PROCESSED | 54320.6348263889 | 54267 | 54052.5243171296 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 18.2084 | -9.2837 | 139.744498 | -71.45365551 | 59.3985 | 53894.2087384259 | 53894.2689467593 | 500014090 | 1508.9 | 35000 | 1508.9 | 1508.9 | 1508.9 | 1508.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1655.2 | 1655.2 | 5202 | 0 | PROCESSED | 54320.4982523148 | 54267 | 54052.5382986111 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 18.2503 | -9.299 | 139.88257526 | -71.45759255 | 59.3985 | 53894.2691435185 | 53894.3356134259 | 500014100 | 1312.1 | 35000 | 1312.1 | 1312.1 | 1312.1 | 1312.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1322 | 1322 | 5742 | 0 | PROCESSED | 54320.6302893518 | 54267 | 54052.5405324074 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 18.2949 | -9.3163 | 140.03044964 | -71.46265703 | 59.3979 | 53894.3358101852 | 53894.4022800926 | 500014110 | 1424.9 | 35000 | 1424.9 | 1424.9 | 1424.9 | 1424.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1433 | 1433 | 5742 | 0 | PROCESSED | 54320.5114236111 | 54267 | 54052.5225694444 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 18.338 | -9.3332 | 140.17356876 | -71.46762322 | 59.3974 | 53894.4024768518 | 53894.4682986111 | 500014120 | 1555.1 | 35000 | 1555.1 | 1555.1 | 1555.1 | 1555.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1566 | 1566 | 5682 | 0 | PROCESSED | 54320.5052199074 | 54267 | 54052.5441782407 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 18.3869 | -9.3535 | 140.33698221 | -71.47421859 | 59.3991 | 53894.4684490741 | 53894.5356365741 | 500014130 | 1693.9 | 35000 | 1693.9 | 1693.9 | 1693.9 | 1693.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1694 | 1694 | 5804 | 0 | PROCESSED | 54320.6286689815 | 54267 | 54052.5234722222 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 18.435 | -9.3697 | 140.49459076 | -71.47695116 | 59.4003 | 53894.5358333333 | 53894.6016087963 | 500014140 | 1977 | 35000 | 1977 | 1977 | 1977 | 1977 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1951 | 1951 | 5671.9 | 0 | PROCESSED | 54320.4993171296 | 54267 | 54052.5450231482 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | 73P/SW3 | 18.4874 | -9.3902 | 140.66879726 | -71.4825298 | 59.4036 | 53894.6018055556 | 53894.680775463 | 500014150 | 3232 | 35000 | 3232 | 3232 | 3232 | 3232 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3293 | 3293 | 6815.9 | 0 | PROCESSED | 54320.6442361111 | 54267 | 54052.5265509259 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | | MBM12 | 44.0042 | 19.487 | 159.18888296 | -34.46916863 | 253.4644 | 53769.9600578704 | 53772.6460416667 | 500015010 | 102937.1 | 100000 | 102937.1 | 102937.1 | 102937.1 | 102937.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93670.9 | 93670.9 | 232049.9 | 1 | PROCESSED | 54330.2671412037 | 54247 | 54041.1327662037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001059 | Suzaku can potentially determine the time since the nearby supernova that created (or reheated) the Local Hot Bubble (LHB) by measuring the ratio of the O VII/O VIII lines emitted by the LHB. The LHB temperature is ~10^6 K, and in equilibrium we would expect no O VIII emission. However, the LHB is almost certainly not in equilibrium, and it is quite possible that significant O^{+7} is still recombining (and emitting O VIII) following its creation in the most recent local supernova 2-4 Myr ago. We propose to measure these lines from the LHB using the nearby molecular cloud MBM12 as a curtain to shadow more distant emission. Even if O VIII is not detected, the O VII measurement will be the first unambiguous measurement of a line from the LHB. | GALACTIC DIFFUSE EMISSION | 5 | A | SMITH | RANDALL | NULL | NULL | JAP | 0 | SWG | DATING THE LOCAL HOT BUBBLE WITH SUZAKU | XIS | N | | SN1006 SE | 225.8656 | -42.0517 | 327.61589547 | 14.40537 | 115.0022 | 53765.3759259259 | 53766.487662037 | 500016010 | 51607.6 | 50000 | 51613.2 | 51621.2 | 51621.2 | 51607.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 55670.4 | 55670.4 | 96039.9 | 2 | PROCESSED | 54324.9845138889 | 54247 | 54040.6484259259 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001062 | We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | A | HUGHES | JOHN | NULL | NULL | JAP | 0 | SWG | THE EJECTA IN SN1006 | XIS | N | | SN1006 NW | 225.6364 | -41.8003 | 327.59294648 | 14.70833496 | 115.0008 | 53766.4881365741 | 53767.55375 | 500017010 | 53019.4 | 50000 | 53019.4 | 53027.7 | 53027.3 | 53027.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60412.3 | 60412.3 | 92067.9 | 0 | PROCESSED | 54324.6815625 | 54247 | 54040.7669675926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001062 | We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | A | HUGHES | JOHN | NULL | NULL | JAP | 0 | SWG | THE EJECTA IN SN1006 | XIS | N | | SGR C | 266.1523 | -29.4673 | 359.43182832 | -0.08906822 | 82.0001 | 53786.5315393518 | 53789.4515509259 | 500018010 | 106921.9 | 100000 | 106921.9 | 106921.9 | 106921.9 | 106921.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 46606.9 | 46606.9 | 252277.8 | 2 | PROCESSED | 54328.8217013889 | 54247 | 54041.6109375 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001079 | We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD. | GALACTIC DIFFUSE EMISSION | 5 | A | MURAKAMI | HIROSHI | NULL | NULL | JAP | 0 | SWG | FOSSILS OF THE GALACTIC CENTER ACTIVITY | XIS | N | | SGR C BGD | 265.7856 | -29.8854 | 358.90876565 | -0.03691694 | 81.9998 | 53789.4522106482 | 53789.8349421296 | 500019010 | 13307.3 | 10000 | 13315.3 | 13315.3 | 13315.3 | 13307.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 12240.4 | 12240.4 | 33063.9 | 0 | PROCESSED | 54320.7962847222 | 54247 | 54041.3629166667 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001079 | We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD. | GALACTIC DIFFUSE EMISSION | 5 | A | MURAKAMI | HIROSHI | NULL | NULL | JAP | 0 | SWG | FOSSILS OF THE GALACTIC CENTER ACTIVITY | XIS | N | | CYGNUS LOOP NE1 | 314.1885 | 31.738 | 75.60815027 | -8.84073861 | 223.0005 | 53697.7354282407 | 53698.2051388889 | 500020010 | 20343.7 | 20000 | 20351.7 | 20351.7 | 20351.7 | 20343.7 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17992 | 17992 | 40575.9 | 0 | PROCESSED | 54324.2030092593 | 54247 | 54037.9167476852 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | NULL | N | | CYGNUS LOOP NE2 | 313.9681 | 31.9542 | 75.65570239 | -8.55863001 | 223.0005 | 53698.2056134259 | 53698.6766666667 | 500021010 | 21413.5 | 20000 | 21445.5 | 21437.5 | 21429.5 | 21413.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21654.1 | 21654.1 | 40693.9 | 0 | PROCESSED | 54324.5717013889 | 54247 | 54038.4014351852 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | NULL | N | | CYGNUS LOOP NE3 | 313.7583 | 32.1826 | 75.71932756 | -8.27611719 | 222.9011 | 53703.7415162037 | 53704.2355208333 | 500022010 | 21133.8 | 20000 | 21191.6 | 21719.9 | 21133.8 | 21359.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20244.5 | 20244.5 | 42679.9 | 1 | PROCESSED | 54324.6667013889 | 54247 | 54038.7522106482 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | N | | CYGNUS LOOP NE4 | 313.5005 | 32.369 | 75.72495347 | -7.98937114 | 221.2023 | 53704.2368287037 | 53704.7661342593 | 500023010 | 25004.9 | 20000 | 25004.9 | 25268.9 | 25006.7 | 25068.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25124.9 | 25124.9 | 45726 | 1 | PROCESSED | 54324.6202430556 | 54247 | 54038.67625 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | N | | TYCHO SNR | 6.3244 | 64.1507 | 120.08671326 | 1.42345384 | 81.1044 | 53913.439224537 | 53915.6530555556 | 500024010 | 101127.4 | 100000 | 101143.4 | 101127.4 | 101143.4 | 101143.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 94512.3 | 94512.3 | 191206.8 | 3 | PROCESSED | 54332.1766203704 | 54289 | 54052.7199884259 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001099 | We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HUGHES | JOHN | NULL | NULL | JAP | 0 | SWG | SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT | XIS | N | | TYCHO SNR HXD BKGD | 9.2173 | 64.3076 | 121.35322514 | 1.48051733 | 84.2005 | 53915.6541782407 | 53916.7606944444 | 500025010 | 51008.8 | 50000 | 51008.8 | 51008.8 | 51008.8 | 51008.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 48722.4 | 48722.4 | 95593.9 | 2 | PROCESSED | 54324.0584375 | 54302 | 54052.5940509259 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 001099 | We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HUGHES | JOHN | NULL | NULL | JAP | 0 | SWG | SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT | HXD | N | | NEP | 272.8227 | 66.0165 | 95.79277142 | 28.663354 | 126.3033 | 53776.2556944445 | 53778.0836111111 | 500026010 | 88508.2 | 80000 | 88532.2 | 88508.2 | 88524.2 | 88532.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 83672.8 | 83672.8 | 157902 | 0 | PROCESSED | 54327.7111342593 | 54247 | 54041.1403703704 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000042 | We propose a second Suzaku observation of the NEP region in order to constrain the long-term and short-term valiability of OVII and OIVVV emission line intensities.Short-term variability detected in the first Suzaku observation implies existence of a charge-exchange component in oVIII linem suggesting solar wind and geo corona interaction. First purpose is to confirm this with the second observtaion.Secondly, to search a long-term variability. If it is observed, it will place a further constraints on the solar wind and interplanetary medium near the Earth. | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | NEP | XIS | N | | HIGH LAT. DIFFUSE A | 246.1745 | 43.4846 | 68.4171583 | 44.39202319 | 129.9994 | 53780.2926388889 | 53781.9640509259 | 500027010 | 73578.7 | 70000 | 73586.7 | 73586.7 | 73578.7 | 73586.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 67399.3 | 67399.3 | 144397.9 | 3 | PROCESSED | 54328.5553472222 | 54247 | 54041.3110416667 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000044 | We propose observing the diffse background at two locations where the low temperature component is particularly string. One of the these enhancement is ostensibly an extension of the local bubble, while the other it is probably due to a region of very bright emission in the halo (z> 400 pc). We can verify the thermal nature of these sources, and look for CNO abyndance ratio differences between local disk and halo gas. It is critical to make these abundance determinations before the low energy response deteriorates any further. Note that this observation should also allow a calibration of the XIS response below the carbon edge to ~20%. | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HIGH LATTITUDE DIFFUSE A & B | XIS | N | | HIGH LAT. DIFFUSE B | 38.7468 | -52.2774 | 272.40280946 | -58.27300774 | 280.6379 | 53783.933900463 | 53786.5211111111 | 500027020 | 103553 | 100000 | 103553 | 103561 | 103561 | 103561 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 68609.4 | 68609.4 | 223523.8 | 3 | PROCESSED | 54329.4329513889 | 54247 | 54041.5670717593 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000044 | We propose observing the diffse background at two locations where the low temperature component is particularly string. One of the these enhancement is ostensibly an extension of the local bubble, while the other it is probably due to a region of very bright emission in the halo (z> 400 pc). We can verify the thermal nature of these sources, and look for CNO abyndance ratio differences between local disk and halo gas. It is critical to make these abundance determinations before the low energy response deteriorates any further. Note that this observation should also allow a calibration of the XIS response below the carbon edge to ~20%. | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HIGH LATTITUDE DIFFUSE A & B | XIS | N | | VICINITY OF LMC X-3 | 83.4844 | -63.8863 | 273.3865557 | -32.64248934 | 284.6189 | 53811.6008333333 | 53813.9168055556 | 500031010 | 82018.5 | 80000 | 82026.5 | 82018.5 | 82026.5 | 82026.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 74614.8 | 74614.8 | 200063.9 | 2 | PROCESSED | 54329.0668402778 | 54247 | 54056.4806828704 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 000043 | We propose to observe the vicnity of LMC X-3 for 80 ks. We expectt to determine the OVII and OVIII emission line intensities within 20% errors. Combining these results with the OVII and OVIII absorption lines observed in the energy spectra of LMC X-3 with Chandra LETG-HRC, we can determine the geometrocal extent od the hot gas along the line-of-sight direction. This will answer the long-unanswered question; from where the high lattitude OVII/OVIII emissions come ? | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | VICINITY OF LMC X-3 | XIS | N | | SKY_50.0_-62.4 | 50.0507 | -62.4328 | 278.67600391 | -47.08169247 | 281.591 | 53795.7055671296 | 53796.9369675926 | 501001010 | 80145 | 80000 | 80153 | 80145 | 80153 | 80145 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 74012.2 | 74012.2 | 106376 | 0 | PROCESSED | 54324.2393518518 | 54401 | 53905.6164930556 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011252 | We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble. | GALACTIC DIFFUSE EMISSION | 5 | A | SHELTON | ROBIN | NULL | NULL | USA | 1 | AO1 | SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE | XIS | N | | SKY_53.3_-63.4 | 53.24 | -63.4549 | 278.62179386 | -45.30780651 | 286.1724 | 53797.8694444444 | 53800.3342476852 | 501002010 | 101475.2 | 100000 | 101475.2 | 101475.2 | 101475.2 | 101475.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 145431.8 | 145431.8 | 212853.9 | 4 | PROCESSED | 54329.5976736111 | 54401 | 53906.7729282407 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011252 | We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble. | GALACTIC DIFFUSE EMISSION | 5 | A | SHELTON | ROBIN | NULL | NULL | USA | 1 | AO1 | SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE | XIS | N | | M17 | 275.2076 | -16.1829 | 15.0906551 | -0.7606192 | 110.1996 | 53805.8263425926 | 53808.5349421296 | 501003010 | 102702.1 | 100000 | 102710.1 | 102710.1 | 102702.1 | 102710.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 92566.1 | 92566.1 | 233967.8 | 4 | PROCESSED | 54330.0440625 | 54394 | 53905.822662037 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010066 | Recent Chandra observations discovered that HII regions possess a few MK extended plasma, but the origin of the emission is still unknown. We propose to observe M17, which has the most spectacular sample of such emission. A superb soft-band response of XIS will enable us to measure the strengths of O and N emission lines, giving us strong arguments to elucidate the cause of the emission. A 300 ks Chandra observation is planned this year in addition to the existing 40 ks data, which will help us to discriminate the point source contribution. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 1 | AO1 | XIS INVESTIGATION FOR THE ORIGIN OF DIFFUSE X-RAY EMISSION IN GALACTIC H II REGIONS | XIS | N | | DRACO HVC REGION A | 243.9602 | 60.0594 | 91.20688798 | 42.38144862 | 79.8192 | 53814.6161111111 | 53816.0050578704 | 501004010 | 61179.8 | 60000 | 61179.8 | 61179.8 | 61179.8 | 61179.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 61230.1 | 61230.1 | 119987.9 | 2 | PROCESSED | 54405.7030902778 | 54394 | 53906.0459722222 | 2.1.6.15 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010069 | High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE - | XIS | N | | DRACO HVC REGION B | 243.9603 | 59.1738 | 90.07720195 | 42.68363475 | 80.282 | 53816.0059953704 | 53817.4148611111 | 501005010 | 61632 | 60000 | 61644.7 | 61644 | 61632 | 61636 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60686.5 | 60686.5 | 121709.9 | 2 | PROCESSED | 54405.7328819444 | 54400 | 53906.4964583333 | 2.1.6.15 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010069 | High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE - | XIS | N | | IC 443 | 94.2975 | 22.7757 | 188.8694635 | 3.11574616 | 274.0004 | 54165.4446643518 | 54166.5154398148 | 501006010 | 42011.3 | 40000 | 42011.3 | 42012.9 | 0 | 42020.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34693.4 | 34693.4 | 92509.9 | 2 | PROCESSED | 54324.7636574074 | 54736 | 54174.6613541667 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010040 | IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution. | GALACTIC DIFFUSE EMISSION | 5 | B | OZAKI | MASANOBU | NULL | NULL | JAP | 1 | AO1 | UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION | XIS | Y | | IC 443 | 94.2972 | 22.4797 | 189.13057055 | 2.97563306 | 274.0001 | 54166.5158680556 | 54167.612025463 | 501006020 | 44013.5 | 40000 | 44013.5 | 44037.5 | 0 | 44021.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36320.9 | 36320.9 | 94699.9 | 1 | PROCESSED | 54324.2986805556 | 54736 | 54172.2247800926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010040 | IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution. | GALACTIC DIFFUSE EMISSION | 5 | B | OZAKI | MASANOBU | NULL | NULL | JAP | 1 | AO1 | UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION | XIS | Y | | CTB 37B | 258.4918 | -38.2006 | 348.64561092 | 0.37683278 | 270.1267 | 53974.0604976852 | 53976.2398032407 | 501007010 | 82815.1 | 80000 | 82871.1 | 82815.1 | 82879.1 | 82863.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 68860.3 | 68860.3 | 188277.9 | 2 | PROCESSED | 54328.2313541667 | 54526 | 54053.4840162037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010042 | The Galactic Plane Survey with HESS found several new TeV sources, called as "dark particle accelerators". They must be powerful cosmic-ray accelerators, although their origin is still unknown due to the lack of information in other wavelengths. We investigate one of the extended sample with radio SNR counterpart, CTB 37B, which is marginally detected on the edge of ASCA GIS. ASCA spectrum shows rather soft power-law feature, indicating that there are both thermal and non-thermal X-ray emission. With the low background of XISs and HXD, parameters of both components are determined with 80 ks exposure. The non-thermal component suggests the new sample of accelerators, and the thermal compopent reveals the condition of the proton acceleration site, for the first time. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 1 | AO1 | UNCOVERING THE NATURE OF DARK PARTICLE ACCELERATORS | XIS | N | | GC SOUTH | 266.5016 | -29.1694 | 359.84485124 | -0.1935349 | 265.0006 | 54004.5960185185 | 54007.8925231482 | 501008010 | 129577.3 | 130000 | 129577.3 | 129577.3 | 129577.3 | 129577.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 111259.1 | 111259.1 | 284803.8 | 5 | PROCESSED | 54331.2681018518 | 54744 | 54021.0929050926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010044 | Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER | XIS | Y | | GC SOUTH BGD | 266.1893 | -28.9082 | 359.92534776 | 0.17564926 | 265.0003 | 54007.8931365741 | 54009.2884143518 | 501009010 | 51190 | 50000 | 51198 | 51206 | 51190 | 51198 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 47715.7 | 47715.7 | 120547.9 | 0 | PROCESSED | 54324.1121643518 | 54735 | 54020.9371064815 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010044 | Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER | XIS | Y | | HESS J1745-303 | 266.2629 | -30.3722 | 358.71029443 | -0.64354718 | 263.6011 | 54015.0950462963 | 54016.4300810185 | 501010010 | 50670.7 | 50000 | 50670.7 | 50670.7 | 50670.7 | 50670.7 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 45689.7 | 45689.7 | 115311.9 | 1 | PROCESSED | 54327.2596643518 | 54526 | 54021.698587963 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010046 | So far, the evidence for hadron acceleration up to near the knee energy has not yet obtained. Recent galactic plane survey in the TeV gamma-ray band reveals several new unidentified sources like HESS J1745-303. It is extended, hence likely a supernova remnant. Also it coincides with an EGRET unidentified source (3EG J1744-3011), which may suggest that it is a source of accelerated protons. However, HESS J1745-303 shows rather hard spectrum that cannot be explained by the simplest version of the diffusive shock acceleration model. X-ray study on HESS J1745-303 is necessary for further discussions. We might find that observed data requires modification of the common picture that young supernova remnants are the dominant source of high-energy protons. | GALACTIC DIFFUSE EMISSION | 5 | A | YAMAZAKI | RYO | NULL | NULL | JAP | 1 | AO1 | X-RAY STUDY ON THE TEV UNIDENTIFIED SOURCE HESS J1745-303 | XIS | N | | G344.7-0.1 | 255.9588 | -41.7032 | 344.67682908 | -0.15577285 | 89.2821 | 54152.1890393518 | 54153.2919097222 | 501011010 | 42133.6 | 40000 | 42133.6 | 42133.6 | 0 | 42133.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34201.6 | 34201.6 | 95280 | 1 | PROCESSED | 54405.8961342593 | 54777 | 54158.2352662037 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010050 | We propose an observation of a supernova remnant (SNR) G344.7-0.1 with Suzaku. In addition to emission lines from highly ionized ions (Si, S, and so on), we found a strong emission line at 6.4 keV in the spectra obtained with ASCA and XMM-Newton. This line is thought to be a K-line from the low-ionized Fe, but the origin is still unknown. Precise measurements of the line energy and the spectral parameters with the XIS will provide us with understanding the origin of the Fe-K line and the physical process in the SNR. | GALACTIC DIFFUSE EMISSION | 5 | C | YAMAUCHI | SHIGEO | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATION OF G344.7-0.1 | XIS | Y | | CYGNUS_LOOP_P1 | 313.519 | 31.9657 | 75.41990185 | -8.25713566 | 240 | 54417.6059259259 | 54418.0904976852 | 501012010 | 16738.5 | 10000 | 16738.5 | 16748.9 | 0 | 16742.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15775.8 | 15775.8 | 41860 | 1 | PROCESSED | 54430.2016087963 | 54798 | 54430.2159375 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | | CYGNUS_LOOP_P2 | 313.2729 | 31.7708 | 75.13379207 | -8.21853117 | 240.0005 | 54418.0909722222 | 54418.4168865741 | 501013010 | 16379.9 | 10000 | 16387.9 | 16387.9 | 0 | 16379.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10978.6 | 10978.6 | 28151.9 | 0 | PROCESSED | 54430.180150463 | 54798 | 54430.1915972222 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | | CYGNUS_LOOP_P3 | 313.0409 | 31.565 | 74.84662265 | -8.19493741 | 240.0003 | 54418.4174074074 | 54418.9377083333 | 501014010 | 16764.8 | 12000 | 16781.2 | 16780.8 | 0 | 16764.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14696.2 | 14696.2 | 44943.9 | 0 | PROCESSED | 54430.2504861111 | 54798 | 54430.2624884259 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | | CYGNUS_LOOP_P4 | 312.8083 | 31.361 | 74.56035476 | -8.16867105 | 239.9997 | 54418.9382291667 | 54419.3196643518 | 501015010 | 18279 | 15000 | 18287 | 18279 | 0 | 18287 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14286 | 14286 | 32943.9 | 0 | PROCESSED | 54430.2299074074 | 54798 | 54430.2398726852 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | | CYGNUS_LOOP_P5 | 312.5567 | 31.1701 | 74.2739834 | -8.12038976 | 239.9995 | 54419.3201388889 | 54420.0627777778 | 501016010 | 28406.2 | 22000 | 28406.2 | 28406.2 | 0 | 28406.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25370 | 25370 | 64155.9 | 1 | PROCESSED | 54430.3177893518 | 54798 | 54430.4318865741 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | | CYGNUS_LOOP_P6 | 312.3057 | 30.9823 | 73.99029438 | -8.06939848 | 240.0003 | 54415.3923032407 | 54416.1668287037 | 501017010 | 28704.9 | 22000 | 28704.9 | 28704.9 | 0 | 28704.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26887.8 | 26887.8 | 66911.9 | 0 | PROCESSED | 54430.1751041667 | 54798 | 54430.18875 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | | CYGNUS_LOOP_P7 | 312.0838 | 30.7678 | 73.70103145 | -8.0534172 | 239.9966 | 54416.1673032407 | 54416.7223263889 | 501018010 | 24154.5 | 22000 | 24154.5 | 24154.5 | 0 | 24154.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18861 | 18861 | 47920 | 0 | PROCESSED | 54430.1240972222 | 54798 | 54430.1343287037 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | | CYGNUS_LOOP_P9 | 311.8173 | 30.594 | 73.41991066 | -7.98099126 | 239.9998 | 54416.7228935185 | 54417.2502199074 | 501019010 | 19565.6 | 15000 | 19565.6 | 19565.6 | 0 | 19565.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17344.6 | 17344.6 | 45537.9 | 0 | PROCESSED | 54430.2193865741 | 54798 | 54430.2327546296 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | | CYGNUS_LOOP_P10 | 311.5744 | 30.3992 | 73.13474548 | -7.93635975 | 240.0007 | 54417.2506944444 | 54417.6043402778 | 501020010 | 16795.8 | 10000 | 16795.8 | 16819.8 | 0 | 16803.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12672.9 | 12672.9 | 30549.9 | 0 | PROCESSED | 54430.1487731482 | 54798 | 54430.1578472222 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | | CYGNUS_LOOP_P8 | 313.9965 | 31.4722 | 75.29540263 | -8.88432445 | 62.5181 | 53868.0059837963 | 53868.1717476852 | 501028010 | 4870.6 | 6000 | 4870.6 | 4870.6 | 4870.6 | 4870.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2328 | 2328 | 14316 | 0 | PROCESSED | 54320.6489236111 | 54394 | 53914.3326157407 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | | CYGNUS_LOOP_P12 | 313.7421 | 31.2725 | 74.99964096 | -8.84356964 | 62.1405 | 53864.7943055556 | 53865.1391087963 | 501029010 | 13542.6 | 10000 | 13542.6 | 13542.6 | 13542.6 | 13542.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2156.7 | 2156.7 | 29780 | 1 | PROCESSED | 54320.8458333333 | 54394 | 53914.0447916667 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | | CYGNUS_LOOP_P13 | 313.4901 | 31.0708 | 74.70349314 | -8.80441033 | 68.2467 | 53865.1416666667 | 53865.5321643518 | 501030010 | 17073 | 17000 | 17073 | 17081 | 17089 | 17089 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 14269 | 14269 | 33727.9 | 0 | PROCESSED | 54320.8883333333 | 54394 | 53914.0847569444 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | | CYGNUS_LOOP_P14 | 313.2365 | 30.8681 | 74.40554659 | -8.76356285 | 62.362 | 53867.6311111111 | 53868.0050462963 | 501031010 | 18580.9 | 18000 | 18580.9 | 18580.9 | 18580.9 | 18580.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 12737.8 | 12737.8 | 32297.9 | 0 | PROCESSED | 54323.0484837963 | 54394 | 53914.3142476852 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | | CYGNUS_LOOP_P15 | 312.9857 | 30.6621 | 74.106397 | -8.72540127 | 61.9987 | 53880.177974537 | 53880.6716898148 | 501032010 | 20728.9 | 21000 | 20728.9 | 20728.9 | 20728.9 | 20728.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17476 | 17476 | 42634.9 | 0 | PROCESSED | 54323.2058796296 | 54394 | 53926.2440046296 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | | CYGNUS_LOOP_P16 | 312.737 | 30.4592 | 73.81069789 | -8.68546284 | 61.9998 | 53877.1905439815 | 53877.7605671296 | 501033010 | 23337.5 | 22000 | 23369.5 | 23337.5 | 23369.5 | 23369.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20118.4 | 20118.4 | 49243.9 | 2 | PROCESSED | 54326.8950462963 | 54398 | 53926.8416319445 | 2.0.6.13 | 5 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | | CYGNUS_LOOP_P17 | 312.199 | 30.014 | 73.16561663 | -8.59879153 | 61.9999 | 53877.7613657407 | 53878.0446064815 | 501034010 | 14195.3 | 14000 | 14199.3 | 14203.3 | 14199.3 | 14195.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14823.1 | 14823.1 | 24464 | 0 | PROCESSED | 54320.6985069444 | 54394 | 53926.1395833333 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | | CYGNUS_LOOP_P18 | 312.0547 | 29.7111 | 72.84665082 | -8.68804998 | 237.4994 | 54087.0528819444 | 54087.3405208333 | 501035010 | 12011 | 13000 | 12915 | 12011 | 0 | 12907 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11439.4 | 11439.4 | 24835.9 | 3 | PROCESSED | 54320.5629513889 | 54750 | 54096.4390972222 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | | CYGNUS_LOOP_P19 | 311.8094 | 30.0818 | 73.00862935 | -8.2918477 | 237.4997 | 54087.3411805556 | 54087.8245833333 | 501036010 | 18595 | 17000 | 18595 | 18595 | 0 | 18595 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18355 | 18355 | 41755.9 | 0 | PROCESSED | 54322.5466782407 | 54744 | 54096.1443171296 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | | RCW 86 | 221.2555 | -62.3618 | 315.68741681 | -2.33681001 | 278.3377 | 53959.4574652778 | 53961.1294907407 | 501037010 | 59805.4 | 60000 | 59829.4 | 59805.4 | 59829.4 | 59821.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54405 | 54405 | 144420 | 1 | PROCESSED | 54324.8825810185 | 54394 | 54021.0740972222 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010054 | We propose an observation of the Northwest region of RCW 86, one of Galactic supernova remnants (SNRs). Hard X-ray continuum of RCW 86 is accompanied by Fe K line emission at 6.4keV. There is strong possibility that the origin of this line is electrons and protons accelerated in the shell of the SNR. In PV phase, the Southeast region of RCW 86 will be observed, and the density of this region is much larger than that of the Northwest region. Therefore we must compare the fluxes of Fe line and hard continuum of both regions, and discuss the correlation between the flux and the density of emitting region. Such comparative study is very useful for understanding the particle acceleration in the shell-like SNRs. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 1 | AO1 | RCW 86:PECULIAR SNR WITH NEUTRAL FE K LINE | XIS | N | | GC_SGR_B_EAST | 267.0203 | -28.3518 | 0.77973231 | -0.1584432 | 71.8708 | 54162.5141203704 | 54164.5273726852 | 501039010 | 96401.8 | 100000 | 96401.8 | 96401.8 | 0 | 96401.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91082.9 | 91082.9 | 173931.8 | 3 | PROCESSED | 54327.8467592593 | 54736 | 54171.4429050926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010060 | We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 1 | AO1 | OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION | XIS | Y | | GC_SGR_B_NORTH | 266.6958 | -28.383 | 0.60519276 | 0.06967717 | 271.4415 | 53999.7284837963 | 54001.2863425926 | 501040010 | 61375.3 | 62000 | 61391.3 | 61375.3 | 61383.3 | 61391.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53867 | 53867 | 134581.8 | 2 | PROCESSED | 54327.8705324074 | 54735 | 54021.2828472222 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010060 | We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 1 | AO1 | OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION | XIS | Y | | GC_SGR_B_NORTH | 266.6955 | -28.3829 | 0.60514127 | 0.06995468 | 271.4417 | 54002.2105555556 | 54003.2919444444 | 501040020 | 44829.5 | 38000 | 44845.5 | 44829.5 | 44837.5 | 44853.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39970.5 | 39970.5 | 93431.9 | 1 | PROCESSED | 54327.2088194445 | 54744 | 54021.2868055556 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010060 | We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 1 | AO1 | OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION | XIS | Y | | SNR 0509-67.5 | 77.3855 | -67.5341 | 278.15788525 | -34.58671131 | 68.6442 | 53965.2623032407 | 53966.1640509259 | 501041010 | 51276.2 | 50000 | 51276.2 | 51276.2 | 51276.2 | 51276.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 50829.4 | 50829.4 | 77890 | 1 | PROCESSED | 54322.9097222222 | 54526 | 54020.7617592593 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010072 | Hot plasma in young supernova remnants (SNRs) are generally in the state of non-equilibrium ionization (NEI), hence strong L-shell lines of Si, Fe and other elements appear in soft energy band (<1keV). With the observations with Chandra and XMM, quite large ambiguity of ionization age for each element remains because of the limited energy resolution in the soft energy band. Utilizing the supreme energy resolution and background property of Suzaku/XIS, we propose the observation of the youngest type Ia SNR in the LMC, 0509-67.5. We correctly diagnose the NEI plasma of this SNR by determining the ionization age and electron temperature for each element component and constrain the ejecta structure of Type Ia SNR. | GALACTIC DIFFUSE EMISSION | 5 | C | NAKAJIMA | HIROSHI | NULL | NULL | JAP | 1 | AO1 | NEI PLASMA DIAGNOSTICS OF A YOUNG TYPE IA SNR:0509-67.5 | XIS | N | | HESS J1614-518 | 243.5851 | -51.743 | 331.574855 | -0.5276897 | 283.402 | 53993.6672222222 | 53994.4571064815 | 501042010 | 40177.7 | 50000 | 40185.7 | 40177.7 | 40185.7 | 40185.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43560.7 | 43560.7 | 68227.9 | 0 | PROCESSED | 54323.3265509259 | 54526 | 54020.8545833333 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010073 | We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N | | HESS J1614-518 BG | 242.0174 | -52.4329 | 330.3996927 | -0.37656553 | 291.2192 | 53994.4597569444 | 53995.3015509259 | 501043010 | 43555.4 | 50000 | 43563.4 | 43563.4 | 43555.4 | 43563.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 50592.2 | 50592.2 | 72703.9 | 1 | PROCESSED | 54323.3811458333 | 54526 | 54020.8662268518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010073 | We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N | | HESS J1825-137 | 276.5031 | -13.6997 | 17.87105596 | -0.70261201 | 269.3213 | 54025.8175462963 | 54027.1682291667 | 501044010 | 50293 | 50000 | 50293 | 50293 | 50293 | 50293 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42955.7 | 42955.7 | 116694 | 1 | PROCESSED | 54325.0219328704 | 54526 | 54055.4418634259 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010073 | We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N | | HESS J1825-137 BG | 276.9022 | -13.2649 | 18.4366217 | -0.84356166 | 269.33 | 54027.1689351852 | 54028.5072337963 | 501045010 | 52144.4 | 50000 | 52152.4 | 52144.4 | 52152.4 | 52144.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42197.4 | 42197.4 | 115607.9 | 2 | PROCESSED | 54325.0172453704 | 54526 | 54055.6591550926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010073 | We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N | | GALACTIC CENTER | 265.9791 | -28.902 | 359.8343278 | 0.33569605 | 108.8002 | 54169.6271990741 | 54170.1633564815 | 501046010 | 25211 | 25000 | 25227 | 25211 | 0 | 25243 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25008.7 | 25008.7 | 46291.9 | 0 | PROCESSED | 54322.4241319444 | 54736 | 54179.4773842593 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GALACTIC CENTER GC2 | 265.779 | -29.1853 | 359.50136289 | 0.33591697 | 108.7998 | 54170.1638773148 | 54170.7946064815 | 501047010 | 25599 | 25000 | 25607 | 25599 | 0 | 25623 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19088.6 | 19088.6 | 54479.9 | 0 | PROCESSED | 54323.1010069444 | 54736 | 54182.2693865741 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GALACTIC CENTER GC3 | 265.5781 | -29.4684 | 359.1684549 | 0.33584661 | 108.8001 | 54170.7951273148 | 54171.3397453704 | 501048010 | 27454.6 | 25000 | 27478.6 | 27454.6 | 0 | 27478.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24054.8 | 24054.8 | 47047.9 | 1 | PROCESSED | 54320.8735069444 | 54736 | 54182.2788425926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GALACTIC CENTER | 265.3803 | -29.7558 | 358.83357751 | 0.33021849 | 269 | 54016.4324074074 | 54017.0968055556 | 501049010 | 19562.7 | 20000 | 19562.7 | 19562.7 | 19562.7 | 19562.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17633.6 | 17633.6 | 57395.9 | 1 | PROCESSED | 54323.3270833333 | 54735 | 54053.4403356482 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GALACTIC CENTER | 265.9089 | -29.649 | 359.16615355 | -0.00387238 | 269 | 54017.0975115741 | 54017.5690277778 | 501050010 | 22047.7 | 20000 | 22047.7 | 22047.7 | 22047.7 | 22047.7 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18625.6 | 18625.6 | 40735.9 | 0 | PROCESSED | 54323.2511805556 | 54735 | 54053.4127777778 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GALACTIC CENTER | 265.7083 | -29.9322 | 358.83372455 | -0.00453222 | 269.0002 | 54017.5695486111 | 54018.2808333333 | 501051010 | 21869 | 20000 | 21877 | 21877 | 21869 | 21877 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21132.2 | 21132.2 | 61445.9 | 0 | PROCESSED | 54326.9430439815 | 54735 | 54053.5109953704 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GALACTIC CENTER | 265.5037 | -30.2156 | 358.49956421 | -0.00336241 | 269.0005 | 54018.2813541667 | 54018.887662037 | 501052010 | 19245.1 | 20000 | 19261.1 | 19261.1 | 19253.1 | 19245.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16046.2 | 16046.2 | 52379.9 | 1 | PROCESSED | 54322.6539583333 | 54735 | 54053.5074537037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GALACTIC CENTER | 265.2994 | -30.4982 | 358.16648703 | -0.00302139 | 269.0003 | 54018.8881828704 | 54019.4209953704 | 501053010 | 21908.6 | 20000 | 21908.6 | 21932.1 | 21916.6 | 21916.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19948 | 19948 | 46031.9 | 0 | PROCESSED | 54322.5734143518 | 54735 | 54053.5019675926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GALACTIC CENTER GC9 | 266.6299 | -29.2499 | 359.83430056 | -0.33104727 | 109.8001 | 54171.3410532407 | 54171.9988888889 | 501054010 | 26104.4 | 25000 | 26104.4 | 26104.4 | 0 | 26104.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23542.4 | 23542.4 | 56829.9 | 0 | PROCESSED | 54322.5788310185 | 54736 | 54182.2954166667 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GALACTIC CENTER GC10 | 266.4308 | -29.5343 | 359.50116476 | -0.33080245 | 109.7996 | 54171.9994097222 | 54172.6529976852 | 501055010 | 27225.7 | 25000 | 27225.7 | 27249.7 | 0 | 27233.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21181.9 | 21181.9 | 56453.9 | 0 | PROCESSED | 54326.9427777778 | 54736 | 54182.3161342593 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GALACTIC CENTER GC11 | 266.231 | -29.8182 | 359.16839231 | -0.33075371 | 109.7993 | 54172.6536111111 | 54173.2086111111 | 501056010 | 26537.4 | 25000 | 26545.4 | 26545.4 | 0 | 26537.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25278.9 | 25278.9 | 47946 | 0 | PROCESSED | 54323.2388310185 | 54736 | 54182.3328125 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GALACTIC CENTER | 266.0341 | -30.1068 | 358.83318764 | -0.33628911 | 269.0002 | 54019.4218402778 | 54020.1446064815 | 501057010 | 20488.4 | 20000 | 20488.4 | 20496.4 | 20496.4 | 20496.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19086 | 19086 | 62437.9 | 0 | PROCESSED | 54326.9540972222 | 54735 | 54053.6059837963 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GC SGR D NORTH | 266.9758 | -27.7178 | 1.30220378 | 0.20283685 | 108.7992 | 54173.2100578704 | 54174.7883564815 | 501058010 | 63242.2 | 63000 | 63250.2 | 63242.2 | 0 | 63258.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51147.9 | 51147.9 | 136351.9 | 0 | PROCESSED | 54327.5074189815 | 54735 | 54182.440462963 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GC SGR D | 267.0913 | -27.9356 | 1.16847417 | 0.00287016 | 108.7996 | 54174.7887847222 | 54176.2127199074 | 501059010 | 62237.2 | 63000 | 62237.2 | 62245.2 | 0 | 62245.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54369.7 | 54369.7 | 123028 | 0 | PROCESSED | 54326.7557523148 | 54736 | 54185.4865740741 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GC SGR D EAST | 267.2856 | -27.6502 | 1.50163715 | 0.00269695 | 108.7997 | 54176.2132407407 | 54177.8737731482 | 501060010 | 64795.3 | 63000 | 64795.3 | 64826.7 | 0 | 64811.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54629.7 | 54629.7 | 143465.9 | 1 | PROCESSED | 54324.9423263889 | 54736 | 54185.4429050926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | RXJ1713-3946 | 257.9704 | -39.5791 | 347.29183097 | -0.10508063 | 267.9995 | 53989.172025463 | 53989.5306365741 | 501063010 | 18422 | 20000 | 18422 | 18422 | 18422 | 18422 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17759.7 | 17759.7 | 30971.9 | 1 | PROCESSED | 54320.5825462963 | 54526 | 54021.1086458333 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | | RXJ1713-3946 | 258.1633 | -39.7281 | 347.25895477 | -0.31287235 | 268.0002 | 53989.5311574074 | 53989.9216898148 | 501064010 | 21322 | 20000 | 21322 | 21322 | 21322 | 21322 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 23030.6 | 23030.6 | 33727.9 | 0 | PROCESSED | 54320.8300115741 | 54526 | 54020.8109027778 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | | RXJ1713-3946 | 258.1672 | -39.4231 | 347.50735004 | -0.13585591 | 267.9988 | 53989.9221643518 | 53990.3106712963 | 501065010 | 22011 | 20000 | 22011 | 22011 | 22011 | 22011 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20797.3 | 20797.3 | 33557.9 | 0 | PROCESSED | 54323.0392361111 | 54526 | 54020.8390162037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | | RXJ1713-3946 | 257.7744 | -39.7271 | 347.08325974 | -0.07081205 | 268.0001 | 53990.3113310185 | 53990.7106944444 | 501066010 | 20920.7 | 20000 | 20940.7 | 20920.7 | 20926 | 20944.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20699 | 20699 | 34504 | 1 | PROCESSED | 54320.8296643518 | 54526 | 54020.8077546296 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | | RXJ1713-3946 | 257.7765 | -39.428 | 347.32530765 | 0.10490445 | 268.0003 | 53990.7111689815 | 53991.0488888889 | 501067010 | 21179.6 | 20000 | 21187.6 | 21179.6 | 21193.1 | 21195.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 21986.1 | 21986.1 | 29167.9 | 0 | PROCESSED | 54320.7777662037 | 54526 | 54020.8250925926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | | RXJ1713-3946 | 258.5534 | -39.7289 | 347.43430559 | -0.55631777 | 267.9997 | 53991.0497337963 | 53991.4460300926 | 501068010 | 21001.5 | 20000 | 21017.5 | 21009.5 | 21001.5 | 21025.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21209.3 | 21209.3 | 34233.9 | 1 | PROCESSED | 54323.0678356482 | 54526 | 54021.2424537037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | | RXJ1713-3946 | 258.5524 | -39.4291 | 347.6770378 | -0.38034705 | 267.9999 | 53997.5713773148 | 53997.9140509259 | 501069010 | 18375 | 20000 | 18375 | 18375 | 18375 | 18375 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 14276.7 | 14276.7 | 29599.9 | 0 | PROCESSED | 54323.0316550926 | 54526 | 54021.1502546296 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | | RXJ1713-3946 | 258.5527 | -40.0289 | 347.19063141 | -0.73133412 | 268.0015 | 53997.9147569444 | 53998.4425925926 | 501070010 | 20744.2 | 20000 | 20744.2 | 20752.2 | 20752.2 | 20752.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 22026.6 | 22026.6 | 45595.9 | 1 | PROCESSED | 54322.5989467593 | 54526 | 54021.1763541667 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | | RXJ1713-3946 | 258.942 | -39.4278 | 347.8535904 | -0.62405701 | 268.0013 | 53998.4433912037 | 53998.8467476852 | 501071010 | 21174.1 | 20000 | 21174.1 | 21198.1 | 21190.1 | 21182.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18338.7 | 18338.7 | 34839.9 | 0 | PROCESSED | 54323.1323148148 | 54526 | 54020.8878009259 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | | RXJ1713-3946 | 258.9408 | -39.7267 | 347.60984156 | -0.7970823 | 268.0009 | 54013.3138541667 | 54013.877974537 | 501072010 | 19981.7 | 20000 | 19981.7 | 19981.7 | 19981.7 | 19981.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16299.7 | 16299.7 | 48718 | 1 | PROCESSED | 54322.580474537 | 54526 | 54021.6599652778 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | | G156.2+5.7E | 75.8128 | 51.6405 | 156.70319129 | 6.10796494 | 274.6638 | 54149.9177893518 | 54151.1750231482 | 501074010 | 53333.1 | 50000 | 53349.4 | 53349.1 | 0 | 53333.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50821.8 | 50821.8 | 108619.9 | 2 | PROCESSED | 54405.89 | 54773 | 54158.2839583333 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011235 | G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target. | GALACTIC DIFFUSE EMISSION | 5 | C | PETRE | ROBERT | NULL | NULL | USA | 1 | AO1 | A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7 | XIS | Y | | G156.2+5.7NW | 74.223 | 52.4174 | 155.48379099 | 5.80912082 | 273.883 | 54147.6530902778 | 54148.7558333333 | 501075010 | 50546.8 | 50000 | 50546.8 | 50546.8 | 0 | 50546.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46195.8 | 46195.8 | 95259.9 | 0 | PROCESSED | 54323.998275463 | 54695 | 54153.2775 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011235 | G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target. | GALACTIC DIFFUSE EMISSION | 5 | C | PETRE | ROBERT | NULL | NULL | USA | 1 | AO1 | A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7 | XIS | Y | | SNR 0103-72.6 | 16.2944 | -72.389 | 301.47055063 | -44.70024477 | 13.8765 | 53848.0156018518 | 53849.3773032407 | 501077010 | 49271.5 | 50000 | 49279.5 | 49287.5 | 49287.5 | 49271.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37190.5 | 37190.5 | 117629.9 | 3 | PROCESSED | 54323.9669212963 | 54401 | 53907.4220023148 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011241 | We propose Suzaku observations of O-rich supernova remnants (SNRs) 0103-72.6 and 0049-73.6 in the Small Magellanic Cloud (SMC). These SMC SNRs are oldest members (18000 and 14000 yr old) of O-rich SNRs and share X-ray spectral characteristics with a young (1000 yr old) O-rich SNR 0102-7219 which is also in the SMC. While sharing similar spectral features with 0102-7219, the morphologies of 0103-72.6 and 0049-73.6 indicate more evolved phases of the SNR in a similar interstellar environment as 0102-7219. Cross-comparison studies with the high spectral resolution Suzaku/XIS observations among 0103-72.6/0049-73.6 (this proposal) and 0102-7219 (scheduled/observed for the instrument calibrations) will provide a unique opportunity for the study of a long-term evolution of an O-rich SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 1 | AO1 | BACK TO THE FUTURE: LONG-TERM EVOLUTION OF OXYGET-RICH SUPERNOVA REMNANTS IN THE SMALL MAGELLANIC CLOUD | XIS | N | | SNR G93.3+6.9 CENTER | 312.9805 | 55.373 | 93.25121789 | 6.97467523 | 40.9208 | 53905.2215509259 | 53905.6480787037 | 501079010 | 20537.2 | 20000 | 20545.2 | 20545.2 | 20545.2 | 20537.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20008 | 20008 | 36815.9 | 0 | PROCESSED | 54320.8424537037 | 54401 | 53926.792962963 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | | SNR G93.3+6.9 S1 | 313.1088 | 55.5284 | 93.41888838 | 7.01647125 | 40.6424 | 53905.6486458333 | 53905.9696064815 | 501080010 | 15875 | 15000 | 15875 | 15890.2 | 15891 | 15883 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 12758.8 | 12758.8 | 27727.9 | 1 | PROCESSED | 54389.5268287037 | 54401 | 53926.199212963 | 2.1.6.14 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | | SNR G93.3+6.9 S2 | 312.6887 | 55.4958 | 93.24230604 | 7.18061007 | 40.0056 | 53905.9701736111 | 53906.4293865741 | 501081010 | 16009.2 | 15000 | 16035.2 | 16027.2 | 16009.2 | 16035.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 18375.7 | 18375.7 | 39667.9 | 1 | PROCESSED | 54389.5320601852 | 54401 | 53927.314537037 | 2.1.6.14 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | | SNR G93.3+6.9 S3 | 313.171 | 55.2801 | 93.24775568 | 6.83197363 | 40.0152 | 53906.4300462963 | 53906.7266087963 | 501082010 | 16334.7 | 15000 | 16334.7 | 16358.7 | 16350.7 | 16342.7 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13918.6 | 13918.6 | 25615.9 | 0 | PROCESSED | 54320.7147800926 | 54401 | 53926.2481365741 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | | SNR G93.3+6.9 S4 | 312.7524 | 55.2472 | 93.07038921 | 6.99620044 | 39.4008 | 53906.7271296296 | 53907.0550347222 | 501083010 | 15366.2 | 15000 | 15366.2 | 15366.2 | 15366.2 | 15366.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14469.4 | 14469.4 | 28327.9 | 1 | PROCESSED | 54320.7038773148 | 54401 | 53926.117662037 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | | MONOGEM RING WEST | 118.3557 | 8.2507 | 212.50229712 | 17.5030797 | 287.8334 | 53865.545462963 | 53867.1127199074 | 501084010 | 54268.5 | 50000 | 54268.5 | 54268.5 | 54268.5 | 54268.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43231.2 | 43231.2 | 135389.9 | 2 | PROCESSED | 54327.5581365741 | 54401 | 53914.2479282407 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011243 | We propose to acquire the first high-quality, CCD resolution spectrum of the Monogem Ring SNR. The Monogem Ring is a large (D~25 degrees), old (t~10^5 yr) SNR with a soft X-ray spectrum. A 50 ks observation with Suzaku will detect and measure the OVII Triplet and OVIII Lyman-alpha line fluxes. We will use the ratio of these two line complexes to constrain the temperature and ionization timescale of the plasma in this region of the Monogem Ring. Determing the plasma conditions in such evolved SNRs is important for understanding how these remnants merge with and affect the interstellar medium. | GALACTIC DIFFUSE EMISSION | 5 | B | PLUCINSKY | PAUL | NULL | NULL | USA | 1 | AO1 | THE MONOGEM RING: MEASURING THE O LINE EMISSION WITH SUZAKU | XIS | N | | VELA FRAGMENT B | 135.5139 | -43.4767 | 265.2464603 | 1.98991007 | 89.0012 | 54044.6051388889 | 54046.4341898148 | 501085010 | 57880.4 | 60000 | 57896.4 | 57880.4 | 57896.4 | 57896.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 56965.2 | 56965.2 | 158021.9 | 2 | PROCESSED | 54327.9224652778 | 54695 | 54091.4107175926 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011245 | Ejecta fragments from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM-Newton, show strongly enhanced but very different abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe another fragment, "B". The abundances and distribution will provide further evidence about the origin and evolution of these ejecta clumps, In combination with the existing observations of fragments A and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interaction with the remnant shell and the surrounding ISM. | GALACTIC DIFFUSE EMISSION | 5 | C | GAETZ | TERRANCE | NULL | NULL | USA | 1 | AO1 | SEARCHING FOR EJECTA IN VELA SNR FRAGMENT B | XIS | Y | | PUP A : BEK | 125.942 | -42.9405 | 260.51799115 | -3.16426215 | 276.3687 | 53842.2933449074 | 53842.5807407407 | 501086010 | 16091.3 | 15000 | 16091.3 | 16099.3 | 16091.3 | 16091.3 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9698.5 | 9698.5 | 24797 | 0 | PROCESSED | 54327.0470138889 | 54401 | 53906.8467708333 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | | PUP A : NE | 125.7583 | -42.7117 | 260.25284038 | -3.14403225 | 277.1213 | 53842.913287037 | 53843.3091319445 | 501087010 | 20710.9 | 20000 | 20733.6 | 20734.9 | 20718.9 | 20710.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19744.3 | 19744.3 | 34189.9 | 1 | PROCESSED | 54327.2677662037 | 54401 | 53906.9450231482 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | | PUP A : INTERIOR | 125.5916 | -42.8951 | 260.333956 | -3.34905821 | 276.8883 | 53842.5813541667 | 53842.9127199074 | 501088010 | 20270.9 | 20000 | 20292.4 | 20294.9 | 20278.9 | 20270.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19951.9 | 19951.9 | 28623.9 | 0 | PROCESSED | 54326.9224652778 | 54401 | 53906.8948611111 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | | PUP A : SE | 126.0128 | -43.1802 | 260.74447692 | -3.25911558 | 277.1832 | 53843.3098842593 | 53843.8328009259 | 501089010 | 29749.3 | 30000 | 29749.3 | 29817.2 | 29765.2 | 29761.2 | 4 | 2 | 4 | 4 | 1 | 0 | 0 | 22886.7 | 22886.7 | 45174 | 0 | PROCESSED | 54405.7210532407 | 54401 | 53907.001412037 | 2.1.6.15 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | | PUP A : S | 125.6829 | -43.1445 | 260.57740663 | -3.43620983 | 277.8865 | 53843.8334606482 | 53844.4397569444 | 501090010 | 31144.5 | 30000 | 31160.5 | 31152.5 | 31144.5 | 31168.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 26585.6 | 26585.6 | 52371.9 | 1 | PROCESSED | 54405.7329166667 | 54401 | 53907.0902199074 | 2.1.6.15 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | | N11 SB | 74.1823 | -66.412 | 277.1886014 | -36.07081942 | 146.432 | 54046.4407291667 | 54047.232037037 | 501091010 | 30452 | 30000 | 30452 | 30452 | 30452 | 30452 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 26405 | 26405 | 68365.9 | 0 | PROCESSED | 54322.8478935185 | 54455 | 54088.5643287037 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011251 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 2 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 4 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | GALACTIC DIFFUSE EMISSION | 5 | C | WILLIAMS | ROSA | NULL | NULL | USA | 1 | AO1 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | N | | LMC X-3 OFF FIELD 1 | 85.5783 | -64.5441 | 274.09377866 | -31.6918405 | 324.0002 | 53847.1442361111 | 53848.0099421296 | 501097010 | 43606.7 | 50000 | 43606.7 | 43606.7 | 43606.7 | 43606.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42026.1 | 42026.1 | 74745.9 | 0 | PROCESSED | 54327.0138888889 | 54526 | 53907.3335763889 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011256 | The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona. | GALACTIC DIFFUSE EMISSION | 5 | A | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA | XIS | N | | LMC X-3 OFF FIELD 1 | 85.5246 | -64.555 | 274.10794908 | -31.71433471 | 145.4977 | 54039.3159722222 | 54039.7509722222 | 501097020 | 15374.9 | 10000 | 15374.9 | 15382.9 | 15382.9 | 15382.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14926.3 | 14926.3 | 37580 | 0 | PROCESSED | 54320.8499537037 | 54526 | 54088.8072222222 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011256 | The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona. | GALACTIC DIFFUSE EMISSION | 5 | A | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA | XIS | N | | CAR-D1 | 162.0244 | -59.5887 | 287.89332648 | -0.36746291 | 282.973 | 53891.5567361111 | 53892.6343055556 | 501099010 | 76907.4 | 75000 | 76924 | 76932 | 76931.4 | 76907.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 64257.6 | 64257.6 | 93089.9 | 0 | PROCESSED | 54323.974224537 | 54401 | 53926.947974537 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011257 | Soft X-ray emission nebulae with kT =0.1-0.8 keV, log Lx =33-35 ergs/s, and the size of 1-1000 pc accompany a number of giant HII region, but the origin is not understood yet. The Carinae Nebula is 10-100 times more luminous than any other giant HII region in our Galaxy in soft X-rays. From an XMM-Newton observation of the eastern tip of the nebula called Car-D1, we found marginal CVI, CV and OVII lines. If it is real, the carbon abundance should be more than >6 solar, and the OVII line requires more than 2-temperature components. To detect those emission lines clearly and address the origin and environment of the diffuse plasma, we propose a Suzaku observation of the Car-D1 region, optimized for the XIS BI chip. | GALACTIC DIFFUSE EMISSION | 5 | B | HAMAGUCHI | KENJI | NULL | NULL | USA | 1 | AO1 | ORIGIN OF THE DIFFUSE X-RAY EMISSION AROUND THE CARINA NEBULA, A MASSIVE STAR FORMING REGION | XIS | N | | GALACTIC PLANE 111 | 347.9369 | 61.9538 | 111.50111702 | 1.31488521 | 81.8498 | 53892.6499652778 | 53893.680775463 | 501100010 | 72140.9 | 75000 | 72164.9 | 72164.9 | 72164.9 | 72140.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 61025 | 61025 | 89034.9 | 1 | PROCESSED | 54327.2307407407 | 54401 | 53927.3325115741 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011258 | We propose to observe the line of sight towards (l,b)=(111.5,1.3). This line of sight was observed by XMM because the line of sight is particularly simple, allowing the isolation of the spectrum of the Local Hot Bubble (LHB). The XMM observation did not isolate the LHB, but did reveal the existance of a cool (kT~0.18 keV) X-ray emitting component between 200 and 2000 pcs away that was morphologically unidentifiable in the ROSAT All-Sky Survey. This component may represent the gas responsible for the 3/4 keV "infill problem", and may represent a previously overlooked high filling factor component of the hot ISM. Suzaku observations along this line of sight, coupled with the Suzaku observation towards MBM12, will allow the isolation of this component. | GALACTIC DIFFUSE EMISSION | 5 | B | KUNTZ | K. | NULL | NULL | USA | 1 | AO1 | BEYOND THE LOCAL HOT BUBBLE TOWARDS L=111 | XIS | N | | DRACO ENHANCEMENT | 239.3128 | 61.2868 | 93.98685674 | 43.98646489 | 194.9053 | 54048.1213888889 | 54049.8515509259 | 501101010 | 43862.8 | 75000 | 79427.4 | 79427.4 | 43862.8 | 79419.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 75874.1 | 75874.1 | 149474 | 1 | PROCESSED | 54328.9772106482 | 54455 | 54088.7470486111 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011259 | We propose to observe the Draco Enhancement, a region of very bright 1/4 keV emission in the northern Galactic halo that is only 15 degrees from the Suzaku observation of the North Ecliptic Pole. A decomposition of the spectrum of the Galactic halo by Kuntz & Snowden showed that, to within the uncertainties of the ROSAT All-Sky Survey, the halo emission was composed of two thermal components; a uniform hot component with kT~0.25 keV, and a very patchy soft component with kT~0.1 keV. The soft component is found in only a few isolated regions of the sky, of which the Draco Enhancement is the brightest. This emission is too soft to be studied with XMM. Suzaku will allow us to determine the temperature of the soft component or place very strict upper limits on its temperature. | GALACTIC DIFFUSE EMISSION | 5 | C | KUNTZ | K. | NULL | NULL | USA | 1 | AO1 | THE SOFT COMPONENT OF THE GALACTIC HALO | XIS | N | | MBM12 OFF-CLOUD | 41.3205 | 18.3346 | 157.33933963 | -36.81758445 | 247.4802 | 53772.648599537 | 53774.618275463 | 501104010 | 75329.2 | 70000 | 75337.2 | 75329.2 | 75337.2 | 75337.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 67769 | 67769 | 170115.9 | 1 | PROCESSED | 54329.8071296296 | 54401 | 53905.9757523148 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 011262 | Suzaku will observe MBM 12, a nearby molecular cloud which shadows all but the most local soft X-ray emission. The goal of that observation is to measure the O VII and O VIII emission from the Local Hot Bubble, taking advantage of Suzaku's low energy sensitivity and low background. In light of this, we propose to observe the diffuse background near the MBM 12 position. This will: (1) Measure the O VII and O VIII emission from the Galactic disk and halo, after subtracting the local emission, and (2) confirm that this background emission does not contaminate the initial observation. The absolute measure of the strength of the O VII line, as well as the O VIII/O VII ratio, is essential to understanding the origin of the Galactic component to the 3/4 keV diffuse emission. | GALACTIC DIFFUSE EMISSION | 5 | B | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | THE ORIGIN OF THE GALACTIC DIFFUSE 3/4 KEV X-RAY BACKGROUND | XIS | N | | HESS J1718-385 | 259.5512 | -38.6075 | 348.79652534 | -0.53531102 | 91.2393 | 54154.3587731482 | 54154.7773611111 | 501105010 | 20744 | 19000 | 20744 | 20744 | 0 | 20744 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15836.5 | 15836.5 | 36151.9 | 0 | PROCESSED | 54323.1104976852 | 54527 | 54158.2865740741 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 012044 | HESS J1718-385 is a newly discovered TeV gamma-ray source, with an unusually hard energy spectrum, which lies in close proximity to an energetic pulsar. It is likely that this object belongs to the class of offset pulsar wind nebula (PWN), accelerating electrons and positrons up to ~100 TeV. So far no sensitive X-ray observations of this region have taken place. The synchrotron spectrum of the nebula is predicted to peak in the energy range of the Suzaku HXD. The unprecedented high energy sensitivity of this instrument is required to study the highest energy particles accelerated in this object. Spectral measurements by Suzaku would confirm the inverse-Compton origin of the VHE gamma-rays and place tight constraints on the maximum energy of accelerated electrons. | GALACTIC DIFFUSE EMISSION | 5 | A | HINTON | JAMES | NULL | NULL | EUR | 1 | AO1 | PROBING THE LIMITS OF PARTICLE ACCELERATION IN A NEW HARD SPECTRUM TEV GAMMA-RAY SOURCE | XIS | N | | G156.2+5.7 CENTER | 74.723 | 51.7342 | 156.21466687 | 5.62934315 | 273.4473 | 54148.7568171296 | 54149.9169444444 | 501106010 | 51214.2 | 50000 | 51222.2 | 51230.2 | 0 | 51214.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 46482 | 46482 | 100199.9 | 0 | PROCESSED | 54322.8893634259 | 54695 | 54158.4264351852 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 013079 | Recent observations revealed that about 10 shell-like supernova remnants (SNRs) exhibit power-law X-ray spectra with no emission line which are considered to be synchrotron radiation from high-energy electrons (larger than 1 TeV). However, all those samples are young SNRs (ages about 300-2000 yr). G156.2+5.7 is an old SNR (age about 10^4 year), but emits hard X-rays in addition to usual thin thermal emission (about 0.5 keV temperature). We propose a Suzaku observation on a center region of this SNR, where diffuse hard X-rays were detected with ASCA and XMM. Our primary objective is to determine whether or not the hard tail is synchrotron X-rays, and study cosmic-ray acceleration in this old SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | UENO | MASARU | PETRE | ROBERT | JUS | 1 | AO1 | REVEALING THE ORIGIN OF HARD X-RAY EMISSION FROM AN OLD SNR, G156.2+5.7 | XIS | Y | | VELA X (REGION A) | 128.7666 | -45.458 | 263.74862198 | -2.99483781 | 337.7597 | 53927.7846990741 | 53929.4703819444 | 501107010 | 60773.5 | 60000 | 60773.5 | 60773.5 | 60773.5 | 60773.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54161.1 | 54161.1 | 145605.8 | 3 | PROCESSED | 54329.2805671296 | 54401 | 53942.4562037037 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 014211 | The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. | GALACTIC DIFFUSE EMISSION | 5 | B | KARGALTSEV | OLEG | MORI | KOJI | USJ | 1 | AO1 | THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR | XIS | N | | VELA X (REGION C) | 127.7806 | -46.2716 | 263.99736145 | -4.03006469 | 349.189 | 53933.9133796296 | 53934.7730787037 | 501108010 | 29202.8 | 30000 | 29202.8 | 29202.8 | 29202.8 | 29202.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25592.9 | 25592.9 | 74248 | 1 | PROCESSED | 54327.0649652778 | 54404 | 53943.4988773148 | 2.0.6.13 | 6 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 014211 | The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. | GALACTIC DIFFUSE EMISSION | 5 | B | KARGALTSEV | OLEG | MORI | KOJI | USJ | 1 | AO1 | THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR | XIS | N | | VELA PULSAR/PWN 1 | 128.7701 | -45.1981 | 263.5414959 | -2.83747227 | 337.9628 | 53926.0492592593 | 53927.7841782407 | 501109010 | 60291.3 | 60000 | 60344.6 | 60291.3 | 60331.3 | 60323.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 52689.9 | 52689.9 | 149865.9 | 1 | PROCESSED | 54327.9542824074 | 54401 | 53942.4588078704 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 014211 | The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. | GALACTIC DIFFUSE EMISSION | 5 | B | KARGALTSEV | OLEG | MORI | KOJI | USJ | 1 | AO1 | THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR | HXD | N | | VELA PULSAR/PWN 3 | 128.6368 | -45.8007 | 263.96966687 | -3.27226783 | 344.1164 | 53925.347974537 | 53926.0467476852 | 501110010 | 17588.6 | 20000 | 17604.6 | 17588.6 | 17588.6 | 17604.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17225.2 | 17225.2 | 60351.9 | 0 | PROCESSED | 54323.0630902778 | 54401 | 53930.634224537 | 2.0.6.13 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 014211 | The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. | GALACTIC DIFFUSE EMISSION | 5 | B | KARGALTSEV | OLEG | MORI | KOJI | USJ | 1 | AO1 | THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR | XIS | N | | G12.0-0.1 | 273.0232 | -18.6277 | 11.94868379 | -0.09019508 | 259.2908 | 54375.5953819444 | 54376.9863310185 | 502001010 | 53752.1 | 53000 | 53752.1 | 53752.1 | 0 | 53752.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47183 | 47183 | 120172 | 1 | PROCESSED | 54403.1000694444 | 54751 | 54403.1207986111 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020010 | We propose an observation of a supernova remnant (SNR) G12.0-0.1 with Suzaku. ASCA discovered X-ray emission from this SNR. The X-ray spectrum exhibit a power-law shape, and the radius and X-ray luminosity estimated from the ASCA results are similar to those of SN 1006, which suggests that it is a SN 1006-like SNR. However, due to the poor statistics, we could not conclude that G12.0-0.1 is SN 1006-like SNR. Precise measurements of the X-ray spectrum with the XIS will provide us with understanding the physical process in the SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAUCHI | SHIGEO | NULL | NULL | JAP | 2 | AO2 | SUZAKU OBSERVATION OF G12.0-0.1 | XIS | Y | | GC14 | 267.1584 | -29.141 | 0.16624555 | -0.66947426 | 260.5381 | 54382.6950694444 | 54383.1530555556 | 502002010 | 23190.3 | 20000 | 23206.3 | 23190.3 | 0 | 23206.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20932.9 | 20932.9 | 39559.9 | 0 | PROCESSED | 54402.7161111111 | 54771 | 54402.7240740741 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GC15 | 266.9617 | -29.4257 | 359.83382525 | -0.66952641 | 260.7835 | 54383.1536226852 | 54383.6391666667 | 502003010 | 21467.1 | 20000 | 21475.1 | 21467.1 | 0 | 21475.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18922.5 | 18922.5 | 41943.9 | 0 | PROCESSED | 54402.7409490741 | 54771 | 54402.7485532407 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GC16 | 267.4868 | -29.3131 | 0.16607902 | -1.00376926 | 260.5335 | 54383.6397800926 | 54384.0419444444 | 502004010 | 19873 | 20000 | 19873 | 19890.3 | 0 | 19874.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18832.1 | 18832.1 | 34736 | 0 | PROCESSED | 54402.537337963 | 54771 | 54402.5680208333 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GC17 | 267.2896 | -29.5968 | 359.83441438 | -1.00224826 | 260.2809 | 54384.0425578704 | 54384.480787037 | 502005010 | 20603.5 | 20000 | 20603.5 | 20603.5 | 0 | 20603.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18174.3 | 18174.3 | 37854 | 1 | PROCESSED | 54402.5452430556 | 54777 | 54402.5689583333 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GC18 | 266.183 | -28.6222 | 0.16630142 | 0.32982124 | 260.5302 | 54384.4819560185 | 54384.9633564815 | 502006010 | 22631.1 | 20000 | 22631.1 | 22641.3 | 0 | 22635.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21670.2 | 21670.2 | 41584.1 | 1 | PROCESSED | 54402.6549537037 | 54771 | 54402.6632291667 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GC19 | 265.8593 | -28.4466 | 0.1669402 | 0.66404713 | 262.6738 | 54384.9647569444 | 54385.4112731482 | 502007010 | 22017.4 | 20000 | 22017.4 | 22041.4 | 0 | 22025.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19524.8 | 19524.8 | 38572 | 0 | PROCESSED | 54402.4310763889 | 54771 | 54402.4381365741 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GC20 | 265.6604 | -28.73 | 359.83402449 | 0.66365416 | 262.9349 | 54385.4117939815 | 54385.9099421296 | 502008010 | 23778.6 | 20000 | 23790.6 | 23786.6 | 0 | 23778.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22923.4 | 22923.4 | 43032 | 0 | PROCESSED | 54403.0139699074 | 54771 | 54403.0227314815 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GC21 | 267.484 | -27.3686 | 1.83363899 | -0.00346152 | 261.5433 | 54385.9113888889 | 54386.3127199074 | 502009010 | 20861.5 | 20000 | 20861.5 | 20861.5 | 0 | 20861.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19648.3 | 19648.3 | 34663.9 | 1 | PROCESSED | 54402.5691319444 | 54771 | 54402.5769444444 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GC22 | 266.3806 | -28.337 | 0.50023196 | 0.3305092 | 262.5049 | 54386.3138888889 | 54386.785 | 502010010 | 21621.4 | 20000 | 21621.4 | 21621.4 | 0 | 21621.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21194.4 | 21194.4 | 40662 | 1 | PROCESSED | 54402.6825347222 | 54771 | 54402.6900231482 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | GC23 | 266.578 | -28.0524 | 0.83380185 | 0.3300796 | 262.2345 | 54386.7855208333 | 54387.2294444444 | 502011010 | 23013 | 20000 | 23013 | 23021 | 0 | 23029 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22071.2 | 22071.2 | 38319.9 | 2 | PROCESSED | 54402.5213657407 | 54777 | 54402.5316898148 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | | HESS J1745-303 1 | 266.2249 | -30.1096 | 358.91712668 | -0.478438 | 70.5005 | 54527.7555555556 | 54529.7363310185 | 502016010 | 70529.1 | 67000 | 70537.1 | 70529.1 | 0 | 70545.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61793.2 | 61793.2 | 171095.9 | 3 | PROCESSED | 54539.3010532407 | 54908 | 54539.3190509259 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 020023 | A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAZAKI | RYO | NULL | NULL | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y | | HESS J1745-303 2 | 266.4705 | -30.0867 | 359.0474588 | -0.64781783 | 70.5003 | 54531.5601388889 | 54533.6669444444 | 502017010 | 72544.3 | 67000 | 72552.3 | 72552.3 | 0 | 72544.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63972.3 | 63972.3 | 182014.9 | 2 | PROCESSED | 54550.3784027778 | 54919 | 54550.4057986111 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 020023 | A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAZAKI | RYO | NULL | NULL | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y | | HESS J1745-303 3 | 266.0567 | -30.2413 | 358.72882707 | -0.42335991 | 69.0003 | 54533.6682523148 | 54535.8752199074 | 502018010 | 79016.2 | 67000 | 79016.2 | 79040.2 | 0 | 79024.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70201 | 70201 | 190658 | 2 | PROCESSED | 54550.3213773148 | 54919 | 54550.3420601852 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 020023 | A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAZAKI | RYO | NULL | NULL | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y | | SGR D SNR | 267.1922 | -28.1274 | 1.05009547 | -0.17236121 | 267.8977 | 54349.018599537 | 54352.6738310185 | 502020010 | 139080.8 | 133000 | 139080.8 | 139080.8 | 0 | 139080.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 124502.5 | 124502.5 | 315779.8 | 1 | PROCESSED | 54404.7849074074 | 54776 | 54371.5203472222 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020031 | We propose a 100 ksec observation of the Sgr D region. This region contains a supernova remnant (SNR), a massive molecular cloud, an HII region and diffuse TeV gamma-ray emission. The objectives are to detect Sgr D SNR and diffuse X-rays from the TeV source, to discover new SNRs and X-ray Reflection Nebulae (XRNe), and to investigate the spatial distribution of high temperature plasma connecting the Galactic center and the Galactic ridge regions. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 2 | AO2 | OBSERVATIONS OF SGR D SNR, A TEV SOURCE AND DIFFUSE X-RAYS | XIS | Y | | ANTICENTER | 113.3357 | -19.5305 | 234.9976882 | 0.00424804 | 280.7829 | 54212.8606481482 | 54215.4197222222 | 502021010 | 89542.9 | 80000 | 89550.9 | 89558.9 | 0 | 89542.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78988.7 | 78988.7 | 221050.8 | 3 | PROCESSED | 54330.0300578704 | 54744 | 54223.2040046296 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020032 | We propose to observe diffuse radiation from the Galactic plane in the general direction of the anticenter. Absolute measurement of the O VII and O VIII line fluxes will help establish the origin of this mysterious component of the diffuse background. This will allow a search for spectral signatures of non-thermal emission, i.e. charge- exchange emission, in the 3/4 keV band and the determination of abundances in hot gas thermal emission without risk of confusion by emission from hot gas in the Galactic Bulge. | GALACTIC DIFFUSE EMISSION | 5 | B | MASUI | KENSUKE | NULL | NULL | JAP | 2 | AO2 | SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK | XIS | Y | | (L,B)=(0.25,-0.27) | 266.8068 | -28.8823 | 0.22878525 | -0.27253682 | 265.3343 | 54343.5232986111 | 54346.7919560185 | 502022010 | 134790.4 | 133000 | 134798.4 | 134806.4 | 0 | 134790.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 116842.5 | 116842.5 | 282375.9 | 1 | PROCESSED | 54404.7619212963 | 54724 | 54356.5238657407 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020044 | The Suzaku PV observations found that the diffuse X-rays (6.7 and 6.9 keV-lines) from the GC region can well be explained by a thermal emission from hot plasma with kT=6-7keV (GCDX). The comparison of Suzaku and VLA 90cm images show a hit for special correlation, suggest a magnetic confinement of GCDX. Thus, in order to search for new SNRs and investigate the galactic latitude dependency of the GCDX, we make a GC observation with the aiming point of (l,b)=(0.25, -0.27). We also see the correlation of GCDX with the radio. | GALACTIC DIFFUSE EMISSION | 5 | B | TSURU | TAKESHI | NULL | NULL | JAP | 2 | AO2 | GLOBAL STRUCTURES OF THE GALACTIC CENTER DIFFUSE X-RAY PLASMA (GCDX) | XIS | Y | | VELA JR P1 | 131.9787 | -45.8064 | 265.40235777 | -1.43438498 | 347.0031 | 54285.3151273148 | 54285.6904398148 | 502023010 | 10649.6 | 10000 | 10649.6 | 10657.6 | 0 | 10657.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9044.6 | 9044.6 | 32419.9 | 0 | PROCESSED | 54328.4144675926 | 54696 | 54328.4268402778 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P2 | 132.1691 | -45.7748 | 265.4613949 | -1.31133586 | 347.0033 | 54285.6908217593 | 54285.9036342593 | 502024010 | 10850.2 | 10000 | 10874.2 | 10866.2 | 0 | 10850.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9603.7 | 9603.7 | 18375.9 | 0 | PROCESSED | 54328.4112037037 | 54696 | 54328.4167361111 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P3 | 132.1192 | -45.6039 | 265.30669647 | -1.23070071 | 347.0044 | 54285.9040162037 | 54286.1057175926 | 502025010 | 10298 | 10000 | 10298 | 10298 | 0 | 10298 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6726 | 6726 | 17423.9 | 0 | PROCESSED | 54328.4405208333 | 54696 | 54328.4516782407 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P4 | 132.5157 | -45.5453 | 265.43667302 | -0.97855833 | 347.0031 | 54286.1062847222 | 54286.4480787037 | 502026010 | 10972.4 | 10000 | 10972.4 | 10972.4 | 0 | 10972.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11295.9 | 11295.9 | 29511.9 | 1 | PROCESSED | 54328.4266435185 | 54759 | 54328.4405787037 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P5 | 132.9105 | -45.488 | 265.56829981 | -0.72857938 | 347.002 | 54286.4486458333 | 54286.7502777778 | 502027010 | 10977 | 10000 | 10977 | 10977 | 0 | 10977 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10785.8 | 10785.8 | 26053.9 | 0 | PROCESSED | 54328.4557986111 | 54696 | 54328.4697800926 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P6 | 133.325 | -45.4847 | 265.75161327 | -0.50306307 | 347.0024 | 54286.7508449074 | 54286.9863888889 | 502028010 | 11507.2 | 10000 | 11531.2 | 11523.2 | 0 | 11507.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8257.9 | 8257.9 | 20343.9 | 0 | PROCESSED | 54328.3799537037 | 54696 | 54328.3854166667 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P7 | 133.7759 | -45.5828 | 266.02998701 | -0.32446592 | 347.0033 | 54286.9870023148 | 54287.3023032407 | 502029010 | 14583.8 | 10000 | 14583.8 | 14583.8 | 0 | 14583.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12605 | 12605 | 27239.9 | 0 | PROCESSED | 54328.4528125 | 54696 | 54328.4686111111 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P8 | 133.862 | -45.8612 | 266.28131071 | -0.45847751 | 347.0005 | 54287.3028240741 | 54287.7009722222 | 502030010 | 13219.6 | 10000 | 13219.6 | 13219.6 | 0 | 13219.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14441 | 14441 | 34391.9 | 0 | PROCESSED | 54333.4437384259 | 54703 | 54333.4507175926 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P9 | 133.4161 | -45.7633 | 266.00615013 | -0.63304204 | 347.0009 | 54287.7015856482 | 54287.9516666667 | 502031010 | 13252.4 | 10000 | 13268.4 | 13252.4 | 0 | 13268.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9887.7 | 9887.7 | 21599.9 | 0 | PROCESSED | 54333.4355671296 | 54703 | 54333.4413657407 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P10 | 132.9993 | -45.7656 | 265.8217159 | -0.85784968 | 347.0018 | 54287.9522337963 | 54288.2308564815 | 502032010 | 13040 | 10000 | 13048 | 13040 | 0 | 13056 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10698.8 | 10698.8 | 24067.9 | 0 | PROCESSED | 54333.4252083333 | 54703 | 54333.4328240741 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P11 | 132.5986 | -45.8258 | 265.69032827 | -1.11165473 | 347.0024 | 54288.2314236111 | 54288.6112731482 | 502033010 | 11283.3 | 10000 | 11283.3 | 11283.3 | 0 | 11283.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12207.9 | 12207.9 | 32790.1 | 1 | PROCESSED | 54328.396712963 | 54696 | 54328.4031944445 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P12 | 132.2515 | -46.051 | 265.71195175 | -1.4410688 | 347.0011 | 54289.0722106482 | 54289.4078009259 | 502034010 | 9947.9 | 10000 | 9947.9 | 9947.9 | 0 | 9947.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10494 | 10494 | 28983.9 | 0 | PROCESSED | 54328.4737384259 | 54696 | 54328.4792939815 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P13 | 131.851 | -46.106 | 265.57984888 | -1.69160478 | 347.0011 | 54290.1290162037 | 54290.4411342593 | 502035010 | 9408.9 | 10000 | 9408.9 | 9408.9 | 0 | 9408.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8953.1 | 8953.1 | 26963.9 | 0 | PROCESSED | 54328.4845949074 | 54696 | 54328.4906134259 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P14 | 131.9312 | -46.3861 | 265.83284327 | -1.824218 | 347.0017 | 54290.4416087963 | 54290.675150463 | 502036010 | 11034 | 10000 | 11034 | 11042 | 0 | 11042 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11139.1 | 11139.1 | 20167.9 | 0 | PROCESSED | 54328.4693055556 | 54696 | 54328.4740277778 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P15 | 132.3334 | -46.3288 | 265.96324441 | -1.57253381 | 347.0016 | 54291.1946064815 | 54291.46 | 502037010 | 8876 | 10000 | 8876 | 8876 | 0 | 8876 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7341.1 | 7341.1 | 22912.1 | 1 | PROCESSED | 54328.4606134259 | 54696 | 54328.472962963 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P16 | 132.6844 | -46.1051 | 265.94403391 | -1.24290223 | 347.0001 | 54291.4605671296 | 54291.7363773148 | 502038010 | 16442 | 10000 | 16450 | 16450 | 0 | 16442 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16277 | 16277 | 23823.9 | 1 | PROCESSED | 54328.4918518518 | 54696 | 54328.4979398148 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P17 | 133.087 | -46.0455 | 266.0760896 | -0.98967894 | 347.0002 | 54291.7369444444 | 54291.9238773148 | 502039010 | 13032.6 | 10000 | 13064.5 | 13064.6 | 0 | 13032.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8827.2 | 8827.2 | 16143.9 | 0 | PROCESSED | 54333.3993518518 | 54707 | 54333.4040277778 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | VELA JR P18 | 133.5064 | -46.0415 | 266.25968404 | -0.76370949 | 347.0006 | 54291.9244444444 | 54292.1668634259 | 502040010 | 15012.3 | 10000 | 15012.3 | 15036.2 | 0 | 15020.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12895.2 | 12895.2 | 20943.9 | 1 | PROCESSED | 54328.4602199074 | 54696 | 54328.4716666667 | 2.0.6.13 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | | SN1006 | 225.7268 | -41.9424 | 327.58003425 | 14.55159393 | 117.0193 | 54521.6264351852 | 54526.8613310185 | 502046010 | 211737.3 | 200000 | 211745.3 | 211737.3 | 0 | 211745.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 184362.2 | 184362.2 | 417275.9 | 6 | PROCESSED | 54535.6674884259 | 54904 | 54535.729375 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 020052 | Thermal plasma incident SN1006 has very interesting characteristic. Suzaku PV spectrum revealed ionization parameter of the plasma is significantly low. We investigated the spatial variation of the ionization parameter, and found the outer region of SN1006 has lower ionization parameter than the inner region. However, since the center region of SN1006 is placed on the edge of FOV in the PV observation, the spectra have poor statistics, and the ionization state and the metal abundance cannot be decided with good precision. We propose to observe the center region of SN1006 deeply to decide the physical condition of the plasma of young SNR. Necessary exposure time is 150ksec. | GALACTIC DIFFUSE EMISSION | 5 | A | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 2 | AO2 | THE CENTER REGION OF SN1006 | XIS | Y | | LOW_LATITUDE_86-21 | 332.3169 | 30.2173 | 86.0039952 | -20.78963339 | 82.7457 | 54229.0809259259 | 54230.9966898148 | 502047010 | 81548.6 | 80000 | 81548.6 | 81548.6 | 0 | 81548.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72293.1 | 72293.1 | 165509.9 | 2 | PROCESSED | 54328.7660069444 | 54744 | 54244.7948032407 | 2.0.6.13 | 4 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020061 | High galactic-latitude Suzaku observations of soft X-ray diffuse emission so far made show general tendency that the OVII emission line becomes stronger with decreasing abs(b). This suggests that the major part of the emission is originating from the halo of our galaxy. However, we cannot rule out the possibility that the data is contaminated by solar wind charge exchange emission from the entire heliosphere. In oder to confirm the abs(b) dependency and to constrain the spatial distribution of the halo emission, we propose to observe diffuse radiation at a low galactic latitude of abs(b) ~ 20 deg, where the galactic absorption still does not affect the line intensity significantly. | GALACTIC DIFFUSE EMISSION | 5 | B | YOSHINO | TOMOTAKA | NULL | NULL | JAP | 2 | AO2 | SOFT X-RAY DIFFUSE EMISSION AT A LOW GALACTIC LATITUDE | XIS | Y | | 47 TUCANAE | 6.2112 | -71.9961 | 305.8317488 | -44.9821189 | 65.5967 | 54261.1765162037 | 54263.5404976852 | 502048010 | 132105.2 | 133000 | 132145.2 | 132105.2 | 0 | 132137.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132904.2 | 132904.2 | 204231.9 | 1 | PROCESSED | 54329.1934375 | 54745 | 54271.5258796296 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020066 | We propose a 100 ks observation of the globular cluster 47 Tuc. An extended (~2') hard x-ray emission, presumably of non-thermal origin, was detected with Chandra from a position ~6' toward north east of its center. However, the Chandra ACIS spectrum does not allow us to determine with confidence whether it is a non-thermal emission or a high temperature thermal source. Utilizing the high sensitivity of the XIS, we try to distinguish between these two cases. If confirmed, the result may provide valuable information on particle acceleration in non-relativistic shocks, with potential relations the galactic-ridge x-ray emission. We perform a single pointing observation placing the center of the diffuse emission onto XIS nominal position. | GALACTIC DIFFUSE EMISSION | 5 | B | YUASA | TAKAYUKI | NULL | NULL | JAP | 2 | AO2 | OBSERVATIONAL INVESTIGATION OF PARTICLE ACCELERATION IN A GLOBULAR CLUSTER SHOCK | XIS | Y | | HESS J1702-420 | 255.6874 | -42.0709 | 344.26217794 | -0.21974248 | 106.4451 | 54550.458599537 | 54555.625162037 | 502049010 | 215693.2 | 200000 | 215705.3 | 215693.2 | 0 | 215705.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 140637.5 | 140637.5 | 395721.5 | 6 | PROCESSED | 54566.8834490741 | 54933 | 54566.9486458333 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 020067 | The Galactic Plane Survey with HESS found several new TeV sources, called as "dark particle accelerators". They must be powerful cosmic-ray accelerators, although their origin is still unknown due to the lack of information in other wavelengths. We investigate one of the most mysterious sample, HESS J1702-420, which has the brightest HESS compact source without clear counterparts. ASCA Galactic plane survey shows no evidence of X-ray emission although the exposure was too short. With the large effective area and the low background of XISs, we will be able to detect quite dim counterpart or make strong upper-limit in the hard X-ray band. This result will lead us to distinguish that HESS J1702-420 is the true "dark" protonic accelerator, or a hypothetical PWN powered by PSR J1702-4128. | GALACTIC DIFFUSE EMISSION | 5 | B | BAMBA | AYA | NULL | NULL | JAP | 2 | AO2 | RESOLVING THE DARKEST DARK PARTICLE ACCELERATOR | XIS | Y | | GC_G0.9+0.1 | 266.9332 | -28.1474 | 0.91503767 | 0.01290063 | 105.8953 | 54536.2637152778 | 54540.229375 | 502051010 | 138761.4 | 133000 | 138761.4 | 138761.4 | 0 | 138761.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 122221.4 | 122221.4 | 342576.8 | 1 | PROCESSED | 54550.651087963 | 54919 | 54550.6988078704 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 020071 | The Suzaku PV observations found that the diffuse X-rays (6.7 and 6.9 keV-lines) from the GC region can well be explained by a thermal emission from hot plasma (6-7 keV). The most plausible energy injection source is multiple SNe. The huge thermal energy (10^54 ergs) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm this scenario, we propose to observe the shell of G0.9+0.1 and the connecting region of Sgr B and D. The first objective is to detect a thermal emission from the shell of G0.9+0.1 and the second is to discover new SNRs. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 2 | AO2 | SNR G0.9+0.1 AND THE CONNECTING REGION OF SGR B AND D | XIS | Y | | M17 EAST | 275.3895 | -16.2062 | 15.15230897 | -0.92571433 | 271.9996 | 54377.3569907407 | 54380.0940277778 | 502052010 | 114569.5 | 107000 | 114577.5 | 114569.5 | 0 | 114577.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 100887.3 | 100887.3 | 236449.8 | 3 | PROCESSED | 54403.5124884259 | 54771 | 54403.5436111111 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020085 | We continue our XIS study of the soft extended X-ray emission in M17. The first study conducted in a region close to the OB association brought a detailed surface brightness distribution and the highest S/N ratio spectrum of the diffuse emission. In this proposed study, we move our eyes to the west to observe another bright emission outside of the previously studied regions. DSS and ROSAT all-sky survey images suggest that this is a shocked region, in which OB stellar winds impinge upon ISM. We aim to obtain the surface brightness map of this region and measure the plasma temperature difference in and out of the possible shocked region. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 2 | AO2 | FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS - | XIS | Y | | M17 EAST BKG | 275.6441 | -15.5803 | 15.81995827 | -0.84785909 | 271.9998 | 54380.0947800926 | 54381.7571064815 | 502053010 | 71494 | 67000 | 71494 | 71508.5 | 0 | 71502 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 62554.9 | 62554.9 | 143610 | 1 | PROCESSED | 54403.219212963 | 54771 | 54403.2344791667 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020085 | We continue our XIS study of the soft extended X-ray emission in M17. The first study conducted in a region close to the OB association brought a detailed surface brightness distribution and the highest S/N ratio spectrum of the diffuse emission. In this proposed study, we move our eyes to the west to observe another bright emission outside of the previously studied regions. DSS and ROSAT all-sky survey images suggest that this is a shocked region, in which OB stellar winds impinge upon ISM. We aim to obtain the surface brightness map of this region and measure the plasma temperature difference in and out of the possible shocked region. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 2 | AO2 | FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS - | XIS | Y | | GALACTIC BULGE | 268.3774 | -29.9651 | 359.99980668 | -2.0020922 | 279.4328 | 54372.0700347222 | 54375.590462963 | 502059010 | 136824 | 133000 | 136824 | 136824 | 0 | 136824 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110515.6 | 110515.6 | 304130.6 | 2 | PROCESSED | 54402.6143981482 | 54770 | 54402.653275463 | 2.1.6.15 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 020118 | We propose a 100 ks observation on the Galactic Bulge (b=-2.0) with Suzaku. The origin of thermal diffuse X-ray emission will be for the first time clarified with a fine spectroscopy with Suzaku XIS, especially from the Fe-K line analysis. The non-thermal emission from the Galactic Bulge will be also investigated with HXD-PIN. | GALACTIC DIFFUSE EMISSION | 5 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | INVESTIGATION ON THE GALACTIC BULGE DIFFUSE X-RAY EMISSION WITH SUZAKU | XIS | Y | | COMET_8P_TUTTLE-P1_BGD-1 | 28.5142 | 5.254 | 150.31676982 | -54.25438929 | 248.4996 | 54471.3338888889 | 54471.5001273148 | 502061010 | 8390 | 6000 | 8390 | 8390 | 0 | 8390 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7441.9 | 7441.9 | 14343.9 | 0 | PROCESSED | 54542.2523263889 | 54908 | 54542.2616319444 | 2.2.7.18 | 3 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1_BGD-2 | 28.5654 | 5.0072 | 150.57128999 | -54.45813442 | 248.5002 | 54471.5006018518 | 54471.6876273148 | 502061020 | 5682.1 | 4000 | 5690.1 | 5682.1 | 0 | 5696.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5598 | 5598 | 16151.9 | 0 | PROCESSED | 54542.2566666667 | 54908 | 54542.2619097222 | 2.2.7.18 | 3 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-1 | 27.7163 | 7.989 | 147.31647839 | -52.04673223 | 248.4436 | 54470.5233333333 | 54470.5821759259 | 502062010 | 680.3 | 2000 | 680.3 | 680.3 | 0 | 680.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 632 | 632 | 5080 | 0 | PROCESSED | 54542.1940625 | 54908 | 54542.4502083333 | 2.2.7.18 | 4 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-2 | 27.9946 | 7.7582 | 147.87340904 | -52.1573456 | 248.4994 | 54470.5826041667 | 54470.6488310185 | 502062020 | 2219.3 | 2000 | 2219.3 | 2219.3 | 0 | 2219.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2164 | 2164 | 5718 | 0 | PROCESSED | 54542.2083912037 | 54908 | 54542.2129166667 | 2.2.7.18 | 4 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-3 | 28.0473 | 7.5049 | 148.10975305 | -52.37174422 | 248.4997 | 54470.6493055556 | 54470.7154861111 | 502062030 | 1963.3 | 2000 | 1963.3 | 1963.3 | 0 | 1963.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1905 | 1905 | 5718 | 0 | PROCESSED | 54542.2244212963 | 54908 | 54542.2294791667 | 2.2.7.18 | 4 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-4 | 28.0997 | 7.2516 | 148.34803657 | -52.5857522 | 248.4989 | 54470.7159143518 | 54470.7821527778 | 502062040 | 1723.3 | 2000 | 1723.3 | 1723.3 | 0 | 1723.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1456.7 | 1456.7 | 5722 | 0 | PROCESSED | 54542.2130787037 | 54908 | 54542.2187847222 | 2.2.7.18 | 3 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-5 | 28.1493 | 7.0036 | 148.58110255 | -52.79544349 | 248.5006 | 54470.7825810185 | 54470.8487384259 | 502062050 | 1674.6 | 2000 | 1674.6 | 1674.6 | 0 | 1674.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1703 | 1703 | 5686.1 | 0 | PROCESSED | 54542.198587963 | 54908 | 54542.2043055556 | 2.2.7.18 | 3 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-6 | 28.2017 | 6.7525 | 148.82276905 | -53.00641332 | 248.5018 | 54470.8491666667 | 54470.9154050926 | 502062060 | 2026.6 | 2000 | 2026.6 | 2026.6 | 0 | 2026.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2044 | 2044 | 5664 | 0 | PROCESSED | 54542.2264699074 | 54908 | 54542.2318634259 | 2.2.7.18 | 3 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-7 | 28.2572 | 6.4878 | 149.08057764 | -53.2281425 | 248.4991 | 54470.9158333333 | 54470.9820717593 | 502062070 | 3219 | 2000 | 3219 | 3219 | 0 | 3219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3459 | 3459 | 5664 | 0 | PROCESSED | 54542.2344444444 | 54908 | 54542.2385532407 | 2.2.7.18 | 3 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-8 | 28.3076 | 6.2429 | 149.32011202 | -53.43313536 | 248.4984 | 54470.9825 | 54471.0487384259 | 502062080 | 3219 | 3200 | 3219 | 3219 | 0 | 3219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3374 | 3374 | 5664 | 0 | PROCESSED | 54542.2187268518 | 54908 | 54542.2264583333 | 2.2.7.18 | 3 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-9 | 28.3593 | 5.9969 | 149.56477648 | -53.63811023 | 248.4989 | 54471.0491666667 | 54471.1154050926 | 502062090 | 3218.6 | 3200 | 3218.6 | 3218.6 | 0 | 3218.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2439 | 2439 | 5664 | 0 | PROCESSED | 54542.2309606482 | 54908 | 54542.2348611111 | 2.2.7.18 | 3 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-10 | 28.408 | 5.7525 | 149.8061723 | -53.84230192 | 248.5015 | 54471.1158333333 | 54471.1820717593 | 502062100 | 3219.6 | 3200 | 3219.6 | 3219.6 | 0 | 3219.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2166 | 2166 | 5679.9 | 0 | PROCESSED | 54542.2383912037 | 54908 | 54542.2429513889 | 2.2.7.18 | 3 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-11 | 28.4619 | 5.5053 | 150.05998726 | -54.04643055 | 248.5015 | 54471.1825 | 54471.2487384259 | 502062110 | 3219 | 3200 | 3219 | 3219 | 0 | 3219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2035.6 | 2035.6 | 5688 | 0 | PROCESSED | 54542.2827314815 | 54908 | 54542.2871990741 | 2.2.7.18 | 3 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-12 | 28.5143 | 5.2526 | 150.31791041 | -54.25562458 | 248.4993 | 54471.2491666667 | 54471.3154050926 | 502062120 | 3219.6 | 3200 | 3219.6 | 3219.6 | 0 | 3219.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2162 | 2162 | 5696 | 0 | PROCESSED | 54542.2453703704 | 54908 | 54542.261400463 | 2.2.7.18 | 3 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P1-13 | 28.5683 | 5.0085 | 150.57488577 | -54.45575395 | 248.5007 | 54471.3158333333 | 54471.3334606482 | 502062130 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1503.9 | 0 | PROCESSED | 54542.2384490741 | 54910 | 54544.4202893518 | 2.2.7.18 | 3 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_01 | 39.6412 | -35.6843 | 240.18300744 | -65.68930545 | 257.5577 | 54490.0082291667 | 54490.1627083333 | 502063010 | 4346.8 | 5000 | 4346.8 | 4346.8 | 0 | 4346.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4402.9 | 4402.9 | 13327.9 | 1 | PROCESSED | 54546.0913194445 | 54912 | 54546.0974189815 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_02 | 39.704 | -35.8295 | 240.49763907 | -65.60654763 | 257.6692 | 54490.1630902778 | 54490.2960069444 | 502063020 | 5204.9 | 5000 | 5204.9 | 5204.9 | 0 | 5204.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5591.9 | 5591.9 | 11449.9 | 0 | PROCESSED | 54546.1033101852 | 54912 | 54546.1091666667 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_03 | 39.7649 | -35.9737 | 240.80897167 | -65.5250468 | 257.7596 | 54490.2964351852 | 54490.4293287037 | 502063030 | 6038.9 | 6000 | 6054.9 | 6038.9 | 0 | 6054.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6601.1 | 6601.1 | 11463.9 | 0 | PROCESSED | 54546.0981597222 | 54912 | 54546.1040046296 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_04 | 39.8249 | -36.1145 | 241.11100541 | -65.44459708 | 257.8515 | 54490.4297106482 | 54490.562662037 | 502063040 | 6687.6 | 6700 | 6687.6 | 6719.1 | 0 | 6687.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7388.7 | 7388.7 | 11479.9 | 0 | PROCESSED | 54546.1084606482 | 54912 | 54546.1129513889 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_05 | 39.8852 | -36.2545 | 241.40935004 | -65.36366996 | 257.9439 | 54490.5630439815 | 54490.6959953704 | 502063050 | 6697.4 | 6700 | 6697.6 | 6697.6 | 0 | 6697.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6161.9 | 6161.9 | 11479.9 | 0 | PROCESSED | 54546.1210648148 | 54912 | 54546.126712963 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_06 | 39.9457 | -36.3936 | 241.70384829 | -65.28238509 | 258.0349 | 54490.6963773148 | 54490.8293287037 | 502063060 | 6690.4 | 6700 | 6690.6 | 6690.6 | 0 | 6690.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4338 | 4338 | 11479.9 | 0 | PROCESSED | 54546.1146527778 | 54912 | 54546.1201736111 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_07 | 40.0041 | -36.5319 | 241.99586619 | -65.20252382 | 258.1285 | 54490.8297106482 | 54490.962662037 | 502063070 | 5267.6 | 5000 | 5291.6 | 5267.6 | 0 | 5299.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2753 | 2753 | 11479.9 | 0 | PROCESSED | 54546.1262268518 | 54912 | 54546.130462963 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_08 | 40.0642 | -36.6693 | 242.2833952 | -65.12116443 | 253.2206 | 54490.9649421296 | 54491.0959953704 | 502063080 | 3541.6 | 4000 | 3549.6 | 3541.6 | 0 | 3557.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 3564 | 3564 | 11311.9 | 0 | PROCESSED | 54546.1353472222 | 54912 | 54546.1411689815 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_09 | 40.126 | -36.804 | 242.56232387 | -65.03879756 | 253.3121 | 54491.0963773148 | 54491.2292824074 | 502063090 | 4397.9 | 4000 | 4397.9 | 4397.9 | 0 | 4397.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4752 | 4752 | 11443.9 | 0 | PROCESSED | 54546.208912037 | 54912 | 54546.2142592593 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_10 | 40.1849 | -36.9375 | 242.83840601 | -64.95862507 | 253.4045 | 54491.2297106482 | 54491.362662037 | 502063100 | 5730.4 | 5000 | 5738.4 | 5738.4 | 0 | 5730.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6209.1 | 6209.1 | 11473.9 | 0 | PROCESSED | 54546.1898148148 | 54912 | 54546.1949884259 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_11 | 40.2448 | -37.071 | 243.11250517 | -64.87732742 | 253.5002 | 54491.3630439815 | 54491.4959953704 | 502063110 | 6382.2 | 6700 | 6390.2 | 6382.2 | 0 | 6390.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6838.5 | 6838.5 | 11479.9 | 0 | PROCESSED | 54546.1949884259 | 54912 | 54546.1994097222 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_12 | 40.3045 | -37.2045 | 243.38522043 | -64.79583615 | 253.5926 | 54491.4963773148 | 54491.6293287037 | 502063120 | 6608.2 | 6700 | 6608.2 | 6608.2 | 0 | 6624.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6469.8 | 6469.8 | 11479.9 | 0 | PROCESSED | 54546.2570949074 | 54912 | 54546.2619675926 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_13 | 40.3641 | -37.3366 | 243.65335896 | -64.71445889 | 253.6857 | 54491.6297106482 | 54491.762662037 | 502063130 | 6590.7 | 6700 | 6614.7 | 6598.7 | 0 | 6590.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5022.1 | 5022.1 | 11479.9 | 0 | PROCESSED | 54546.2157291667 | 54912 | 54546.2204861111 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_14 | 40.423 | -37.4668 | 243.91615364 | -64.63380941 | 253.7796 | 54491.7630439815 | 54491.8959953704 | 502063140 | 6562.7 | 6700 | 6562.7 | 6586.7 | 0 | 6562.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3833 | 3833 | 11479.9 | 0 | PROCESSED | 54546.2526736111 | 54912 | 54546.2568518518 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_15 | 40.4836 | -37.5961 | 244.17467378 | -64.55180166 | 253.8725 | 54491.8963773148 | 54492.0293287037 | 502063150 | 3471.7 | 4000 | 3479.7 | 3471.7 | 0 | 3487.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2346.1 | 2346.1 | 11479.9 | 1 | PROCESSED | 54546.2096527778 | 54912 | 54546.2153587963 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_16 | 40.5411 | -37.7213 | 244.42429467 | -64.47300408 | 253.9693 | 54492.0297106482 | 54492.162662037 | 502063160 | 3770.5 | 4000 | 3770.5 | 3770.5 | 0 | 3770.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3988.1 | 3988.1 | 11479.9 | 0 | PROCESSED | 54546.2263541667 | 54912 | 54546.2311574074 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_17 | 40.6015 | -37.8518 | 244.68288405 | -64.39021906 | 254.0645 | 54492.1630439815 | 54492.2959953704 | 502063170 | 5149.5 | 5000 | 5149.5 | 5149.5 | 0 | 5149.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5414.2 | 5414.2 | 11432 | 0 | PROCESSED | 54546.2419560185 | 54912 | 54546.2465509259 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_18 | 40.6547 | -37.9803 | 244.9394556 | -64.31314542 | 254.1595 | 54492.2963773148 | 54492.4293287037 | 502063180 | 6150.5 | 6000 | 6150.5 | 6150.5 | 0 | 6150.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6613.3 | 6613.3 | 11479.9 | 0 | PROCESSED | 54546.232037037 | 54912 | 54546.2369675926 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_BGD-1 | 40.599 | -37.8517 | 244.68396515 | -64.39213957 | 254.2787 | 54492.4296643518 | 54492.562662037 | 502064010 | 6570.7 | 5000 | 6570.7 | 6602.4 | 0 | 6586.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6629.3 | 6629.3 | 11487.9 | 0 | PROCESSED | 54546.2370717593 | 54912 | 54546.2413888889 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | COMET_8P_TUTTLE-P2_BGD-2 | 40.4817 | -37.5941 | 244.17118034 | -64.55380496 | 254.4101 | 54492.5631365741 | 54492.7293287037 | 502064020 | 6979.7 | 5000 | 6979.7 | 7003.7 | 0 | 6987.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5547.1 | 5547.1 | 14351.9 | 0 | PROCESSED | 54546.2484722222 | 54912 | 54546.2537847222 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | | G21.5-0.9 | 278.4035 | -10.5067 | 21.56184596 | -0.8687642 | 103.5554 | 54188.7945023148 | 54189.6252199074 | 502065010 | 25141.6 | 100000 | 25156 | 25141.6 | 0 | 25156 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 22889 | 22889 | 71769.9 | 1 | PROCESSED | 54324.3367592593 | 54695 | 54209.5181018518 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021211 | We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray. | GALACTIC DIFFUSE EMISSION | 5 | B | HARRUS | ILANA | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9 | HXD | Y | | G21.5-0.9 | 278.4038 | -10.5066 | 21.56207071 | -0.86897985 | 103.5553 | 54190.0674074074 | 54191.7405671296 | 502065020 | 53526.1 | 100000 | 53526.1 | 53551 | 0 | 53566.1 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 48618 | 48618 | 144541.8 | 0 | PROCESSED | 54328.3614930556 | 54695 | 54200.5054861111 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021211 | We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray. | GALACTIC DIFFUSE EMISSION | 5 | B | HARRUS | ILANA | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9 | HXD | Y | | G332.5-5.6 CENTER | 250.7335 | -54.5135 | 332.53119736 | -5.54004522 | 262.5079 | 54330.694224537 | 54331.8731944444 | 502066010 | 70148.8 | 80000 | 70148.8 | 70148.8 | 0 | 70156.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 71490.7 | 71490.7 | 101839.9 | 0 | PROCESSED | 54404.7105324074 | 54721 | 54354.4910300926 | 2.1.6.15 | 3 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021216 | We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova. | GALACTIC DIFFUSE EMISSION | 5 | B | REYNOLDS | STEPHEN | NULL | NULL | USA | 2 | AO2 | G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION | XIS | Y | | G332.5-5.6 NE | 251.0925 | -54.3783 | 332.77088512 | -5.61037777 | 77.916 | 54504.4521296296 | 54505.6669444444 | 502067010 | 71192.6 | 80000 | 71200.6 | 71208.6 | 0 | 71192.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65250.8 | 65250.8 | 104941.8 | 0 | PROCESSED | 54515.6833912037 | 54883 | 54515.6965509259 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021216 | We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova. | GALACTIC DIFFUSE EMISSION | 5 | B | REYNOLDS | STEPHEN | NULL | NULL | USA | 2 | AO2 | G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION | XIS | Y | | G296.1-0.5N | 177.8287 | -62.3875 | 296.02814016 | -0.3243747 | 322.3815 | 54321.2538541667 | 54323.4522453704 | 502068010 | 77175.9 | 67000 | 77175.9 | 77175.9 | 0 | 77175.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68484.6 | 68484.6 | 189923.7 | 1 | PROCESSED | 54404.8102777778 | 54716 | 54347.5137268518 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021218 | Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles. | GALACTIC DIFFUSE EMISSION | 5 | B | BORKOWSKI | KAZIMIERZ | NULL | NULL | USA | 2 | AO2 | G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE | XIS | Y | | G296.1-0.5S | 177.6962 | -62.7172 | 296.04515802 | -0.65925146 | 111.5869 | 54482.7727662037 | 54484.6668402778 | 502069010 | 69213 | 67000 | 69213 | 69213 | 0 | 69213 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61009.6 | 61009.6 | 163623.7 | 2 | PROCESSED | 54515.097962963 | 54929 | 54563.4417824074 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021218 | Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles. | GALACTIC DIFFUSE EMISSION | 5 | C | BORKOWSKI | KAZIMIERZ | NULL | NULL | USA | 2 | AO2 | G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE | XIS | Y | | ARC1 | 40.8605 | -42.0069 | 253.28744097 | -62.75503946 | 235.1247 | 54480.7980787037 | 54482.7640509259 | 502070010 | 104369.4 | 100000 | 104377.4 | 104385.4 | 0 | 104369.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 115420.2 | 115420.2 | 169837.7 | 3 | PROCESSED | 54490.6791550926 | 54860 | 54490.7270717593 | 2.1.6.16 | 1 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021222 | Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. | GALACTIC DIFFUSE EMISSION | 5 | C | SHELTON | ROBIN | NULL | NULL | USA | 2 | AO2 | A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC | XIS | Y | | ARC2 | 39.9365 | -39.101 | 247.81076012 | -64.49485898 | 35.5401 | 54256.3120486111 | 54258.149525463 | 502071010 | 105727.1 | 100000 | 105735.1 | 105735.1 | 0 | 105727.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82923.6 | 82923.6 | 158741.8 | 1 | PROCESSED | 54328.645775463 | 54702 | 54264.533275463 | 2.0.6.13 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021222 | Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. | GALACTIC DIFFUSE EMISSION | 5 | B | SHELTON | ROBIN | NULL | NULL | USA | 2 | AO2 | A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC | XIS | Y | | ARC_BACKGROUND | 39.8321 | -35.8483 | 240.48423372 | -65.50115915 | 257.6627 | 54496.6274537037 | 54499.812662037 | 502072010 | 0 | 100000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 105161 | 105161 | 275153.7 | 4 | PROCESSED | 54515.3963888889 | 54883 | 54515.6371875 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021222 | Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. | GALACTIC DIFFUSE EMISSION | 5 | C | SHELTON | ROBIN | NULL | NULL | USA | 2 | AO2 | A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC | XIS | Y | | MBM20 | 68.9409 | -14.6227 | 211.39642208 | -36.55928879 | 252.4258 | 54507.612025463 | 54510.6980439815 | 502075010 | 107066.8 | 100000 | 107066.8 | 107066.8 | 0 | 107066.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92803.6 | 92803.6 | 266603.6 | 2 | PROCESSED | 54522.4101851852 | 54889 | 54522.4496527778 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 021224 | We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source. | GALACTIC DIFFUSE EMISSION | 5 | B | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 2 | AO2 | STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20 | XIS | Y | | ERIDANUS HOLE | 67.1401 | -17.0746 | 213.43674881 | -39.09232011 | 64.2755 | 54311.0359606482 | 54313.2161921296 | 502076010 | 103752.3 | 100000 | 103752.3 | 103752.3 | 0 | 103752.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92209.1 | 92209.1 | 188351.8 | 2 | PROCESSED | 54404.8421412037 | 54710 | 54340.7341898148 | 2.1.6.15 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 021224 | We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source. | GALACTIC DIFFUSE EMISSION | 5 | B | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 2 | AO2 | STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20 | XIS | Y | | G54.1+0.3 | 292.6593 | 18.8091 | 54.05763723 | 0.20765467 | 245.096 | 54403.6644560185 | 54406.3335532407 | 502077010 | 101641.1 | 100000 | 101641.1 | 101649.1 | 0 | 101649.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92923.5 | 92923.5 | 230585.7 | 3 | PROCESSED | 54417.7049074074 | 54786 | 54417.8870833333 | 2.1.6.16 | 2 | Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 | 022032 | A proprietary XMM-Newton observation reveals that the pulsar wind nebula G54.1+0.3 has a very hard spectrum (gamma ~ 1.5) and possibly a break between 5 and 10 keV. We propose a 100 ks SUZAKU observation to confirm unambiguously the presence of the break. If confirmed, the break would pose stringent constraints on models of electron emission and propagation in pulsar wind nebulae. | GALACTIC DIFFUSE EMISSION | 5 | C | BOCCHINO | FABRIZIO | NULL | NULL | EUR | 2 | AO2 | THE BREAK IN THE HARD X-RAY ENERGY OF THE PULSAR WIND NEBULA G54.1+0.3 | HXD | Y | | KEPLER | 262.6698 | -21.4886 | 4.51918955 | 6.82146946 | 98.2145 | 54514.1665393518 | 54516.9793287037 | 502078010 | 116963.6 | 100000 | 116963.6 | 116963.6 | 0 | 116963.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98955.1 | 98955.1 | 242995.6 | 3 | PROCESSED | 54525.581412037 | 54894 | 54525.6176851852 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 023074 | We propose to observe the Kepler's SNR in which evidence of particle acceleration will be found. Aim of the observation is to determine power-law contribution in the hard-tail spectrum above 10 keV with HXD-PIN. If we also find the Fe-Kb and Ni-K emission lines with XIS which have not observed in any previous missions, temperature and nt parameter of a NEI model will be fixed. The determination will help to distinguish the power-law component from the thermal one. We also memtioned that the amount of Fe and Ni will be a good estimator to determine the type of Kepler's SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | TAMAGAWA | TORU | Park | Sangwook | JUS | 2 | AO2 | SEARCH FOR EVIDENCE OF COSMIC-RAY ACCELERATION IN THE KEPLER'S SNR | XIS | Y | | RCW86_WEST | 220.2753 | -62.427 | 315.24703456 | -2.20673417 | 96.1553 | 54864.7563194444 | 54866.0134259259 | 503001010 | 53551.9 | 50000 | 53551.9 | 53551.9 | 0 | 53551.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48908.1 | 48908.1 | 108602 | 1 | PROCESSED | 54962.1812268518 | 55329 | 54880.570462963 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030011 | Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y | | RCW86_NORTH | 220.4956 | -62.2074 | 315.43082177 | -2.04872285 | 96.1584 | 54860.901099537 | 54862.1175231482 | 503002010 | 55376 | 50000 | 55384 | 55384 | 0 | 55376 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50273.1 | 50273.1 | 105081.8 | 2 | PROCESSED | 54962.1317361111 | 55329 | 54880.5551041667 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030011 | Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y | | RCW86_SOUTH | 220.8315 | -62.6734 | 315.37853465 | -2.53716675 | 96.1597 | 54862.1182291667 | 54863.3647569445 | 503003010 | 54818.1 | 50000 | 54818.1 | 54818.1 | 0 | 54834.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47348.3 | 47348.3 | 107684.8 | 1 | PROCESSED | 54962.3811805556 | 55329 | 54880.5892361111 | 2.3.12.25 | 3 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030011 | Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y | | RCW86_SE | 221.3859 | -62.671 | 315.61056381 | -2.64231092 | 96.79 | 54863.365787037 | 54864.7550115741 | 503004010 | 53327.4 | 50000 | 53359.4 | 53327.4 | 0 | 53359.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47813.6 | 47813.6 | 119987.9 | 0 | PROCESSED | 54962.145 | 55329 | 54880.5420138889 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030011 | Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y | | ANTICENTER2 | 12.9862 | 62.9112 | 122.98962226 | 0.03950805 | 69.9598 | 54679.0120717593 | 54680.8411921296 | 503006010 | 86110.1 | 80000 | 86123 | 86123 | 0 | 86110.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106785 | 106785 | 158019.8 | 1 | PROCESSED | 54693.3033796296 | 55070 | 54693.3237847222 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030020 | We propose to observe diffuse radiation from the Galactic plane in the general direction of the anticenter. The ROSAT 3/4 keV band all sky map does not show significant dip in intensity at galactic plane, where the CXB component is totally absorbed by galactic absorption. Thus unknown emission must be compensating the CXB component in this energy band. Our AO-2 observation of a general direction of the anticenter direction gives a clear clue to understand the origin of the mysterious emission. We propose to make additional observation in order to confirm the emission component detected in the AO-2 observation generally exist in the galactic plane. | GALACTIC DIFFUSE EMISSION | 5 | B | MASUI | KENSUKE | NULL | NULL | JAP | 3 | AO3 | SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK | XIS | Y | | GC_LARGEPROJECT1 | 266.4387 | -28.5683 | 0.32941305 | 0.16640393 | 260.8767 | 54711.4273958333 | 54712.9530555556 | 503007010 | 52152.3 | 50000 | 52152.3 | 52152.3 | 0 | 52152.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44183.8 | 44183.8 | 131793.8 | 2 | PROCESSED | 54777.8369444444 | 54557 | 54780.6858796296 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT2 | 266.7785 | -29.1292 | 0.00479668 | -0.37932142 | 260.8763 | 54712.9538078704 | 54714.2891087963 | 503008010 | 53638.8 | 50000 | 53654.8 | 53638.8 | 0 | 53654.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42811.1 | 42811.1 | 115333.8 | 0 | PROCESSED | 54777.7471759259 | 54557 | 54780.4880092593 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT3 | 266.4525 | -29.3384 | 359.67825031 | -0.24492188 | 260.8779 | 54714.2896759259 | 54715.6634722222 | 503009010 | 52397.5 | 50000 | 52405.5 | 52397.5 | 0 | 52411.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40269.1 | 40269.1 | 118677.8 | 2 | PROCESSED | 54777.8299421296 | 54557 | 54780.6767476852 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT4 | 266.0398 | -29.5556 | 359.30535174 | -0.05184233 | 261.05 | 54715.6640393518 | 54717.0690277778 | 503010010 | 53105.6 | 50000 | 53121.6 | 53105.6 | 0 | 53113.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37064.6 | 37064.6 | 121366 | 1 | PROCESSED | 54777.5397337963 | 54557 | 54780.6585648148 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT5 | 265.9469 | -29.8331 | 359.02671432 | -0.12852462 | 265.43 | 54717.3806597222 | 54718.8981365741 | 503011010 | 57633.4 | 50000 | 57633.4 | 57633.4 | 0 | 57633.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40155.5 | 40155.5 | 131099.8 | 1 | PROCESSED | 54777.6566203704 | 54557 | 54780.6683912037 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT6 | 266.2992 | -29.9408 | 359.09468885 | -0.44519015 | 265.9621 | 54723.8160532407 | 54725.0348842593 | 503012010 | 57685.5 | 50000 | 57693.5 | 57685.5 | 0 | 57698.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51903.2 | 51903.2 | 105287.8 | 1 | PROCESSED | 54777.4563657407 | 54557 | 54780.6521643518 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT7 | 265.6744 | -30.0704 | 358.7007591 | -0.05229538 | 265.9998 | 54725.0356365741 | 54727.1975 | 503013010 | 104769 | 100000 | 104777 | 104777 | 0 | 104769 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93901.3 | 93901.3 | 186709.8 | 3 | PROCESSED | 54777.6505787037 | 54557 | 54780.5885532407 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT8 | 265.1842 | -30.7499 | 357.90048261 | -0.05223369 | 268.8911 | 54727.1991782407 | 54728.3141203704 | 503014010 | 55365.1 | 50000 | 55365.1 | 55389.1 | 0 | 55365.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51206.9 | 51206.9 | 96311.8 | 1 | PROCESSED | 54777.8241550926 | 54557 | 54783.7018055556 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT9 | 265.0297 | -30.9626 | 357.64981902 | -0.05267713 | 269.1132 | 54728.3146412037 | 54729.4140393518 | 503015010 | 56771.6 | 50000 | 56779.6 | 56771.6 | 0 | 56787.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52845.4 | 52845.4 | 94975.9 | 0 | PROCESSED | 54777.8057523148 | 54557 | 54780.4933564815 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT10 | 264.8736 | -31.1751 | 357.39875369 | -0.05245192 | 268.5898 | 54731.2832060185 | 54732.3383912037 | 503016010 | 52171.2 | 50000 | 52171.2 | 52179.2 | 0 | 52179.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49291.3 | 49291.3 | 91163.9 | 1 | PROCESSED | 54777.7188888889 | 54557 | 54780.6078935185 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT11 | 264.7183 | -31.3859 | 357.14965021 | -0.05250387 | 268.3335 | 54732.3390046296 | 54733.3897337963 | 503017010 | 51286.5 | 50000 | 51294.5 | 51286.5 | 0 | 51302.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48583.4 | 48583.4 | 90775.9 | 2 | PROCESSED | 54777.870625 | 54557 | 54780.6941550926 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT12 | 264.5602 | -31.5978 | 356.8985011 | -0.05173107 | 288.0843 | 54733.394375 | 54733.9377777778 | 503018010 | 29401.2 | 50000 | 29412.5 | 29412.5 | 0 | 29401.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26671.6 | 26671.6 | 46942 | 0 | PROCESSED | 54777.7444444444 | 54557 | 54780.4814583333 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT12 | 264.5606 | -31.5967 | 356.89961278 | -0.05143068 | 268.4538 | 54742.7536226852 | 54743.154375 | 503018020 | 12246.6 | 10000 | 12246.6 | 12246.6 | 0 | 12246.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10232 | 10232 | 34617.9 | 1 | PROCESSED | 54777.5525578704 | 54557 | 54780.5624652778 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT12 | 264.5561 | -31.5945 | 356.89942182 | -0.04701536 | 96.416 | 54881.313900463 | 54881.6919444445 | 503018030 | 11914 | 10000 | 11922 | 11922 | 0 | 11914 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10090.9 | 10090.9 | 32657.9 | 1 | PROCESSED | 54962.381412037 | 54557 | 54895.5872106482 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT13 | 264.4001 | -31.8052 | 356.65040302 | -0.04773216 | 95.4712 | 54881.6929282407 | 54883.0522453704 | 503019010 | 52776.4 | 50000 | 52776.4 | 52797.2 | 0 | 52784.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42439.5 | 42439.5 | 117433.8 | 0 | PROCESSED | 54963.067974537 | 54557 | 54902.1118171296 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT14 | 264.2413 | -32.0163 | 356.39993487 | -0.04727305 | 95.7088 | 54883.0527199074 | 54884.7911342593 | 503020010 | 61044.1 | 50000 | 61068.1 | 61044.1 | 0 | 61060.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51718.5 | 51718.5 | 150131.9 | 1 | PROCESSED | 54962.4140972222 | 54557 | 54895.6029166667 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | GC_LARGEPROJECT15 | 265.2338 | -30.2129 | 358.37855715 | 0.19604348 | 267.777 | 54743.1555902778 | 54744.4565277778 | 503021010 | 53826 | 50000 | 53834 | 53834 | 0 | 53826 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49640.5 | 49640.5 | 112378.1 | 0 | PROCESSED | 54777.4686921296 | 54557 | 54780.430150463 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | | LOOP 1 L=356.00 | 263.2426 | -31.9466 | 356.00010804 | 0.70279756 | 93.3363 | 54908.96625 | 54909.8933333333 | 503022010 | 41319.3 | 40000 | 41319.3 | 41319.3 | 0 | 41319.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34318.7 | 34318.7 | 80069.9 | 0 | PROCESSED | 54963.3456365741 | 55330 | 54923.2640162037 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030023 | NANTEN telescope discovered huge molecular loops in the galactic center region. The model that the huge loops is due to magnetic buoyancy caused by the Parkey instability is proposed. The loops size is 12 order of magnitude larger than the solar loops, but the physics would be common. X-ray emission from shock heated and/or accelerated particles would be expected at the foot point of the loops. We propose an X-ray observation at the foot point of the molecular loop with Suzaku and investigate the magnetic activity in the galactic scale. | GALACTIC DIFFUSE EMISSION | 5 | C | YAMAUCHI | SHIGEO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF MOLECULAR LOOPS IN THE GALACTIC CENTER | XIS | Y | | LOOP 2 L=356.33 | 263.4562 | -31.667 | 356.33349006 | 0.70266893 | 94.2779 | 54916.2757060185 | 54917.0786921296 | 503023010 | 31152.7 | 40000 | 31152.7 | 31152.7 | 0 | 31152.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28234.6 | 28234.6 | 69369.9 | 0 | PROCESSED | 54963.1729513889 | 55330 | 54930.234849537 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030023 | NANTEN telescope discovered huge molecular loops in the galactic center region. The model that the huge loops is due to magnetic buoyancy caused by the Parkey instability is proposed. The loops size is 12 order of magnitude larger than the solar loops, but the physics would be common. X-ray emission from shock heated and/or accelerated particles would be expected at the foot point of the loops. We propose an X-ray observation at the foot point of the molecular loop with Suzaku and investigate the magnetic activity in the galactic scale. | GALACTIC DIFFUSE EMISSION | 5 | C | YAMAUCHI | SHIGEO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF MOLECULAR LOOPS IN THE GALACTIC CENTER | XIS | Y | | HESS J1800-240A | 270.4845 | -23.9659 | 6.13495239 | -0.62617494 | 86.9255 | 54558.6209606482 | 54559.3266087963 | 503025010 | 34782.2 | 30000 | 34782.2 | 34790.2 | 0 | 34790.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25703.3 | 25703.3 | 60967.9 | 0 | PROCESSED | 54574.0403587963 | 54953 | 54574.0504861111 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030043 | H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region. | GALACTIC DIFFUSE EMISSION | 5 | A | TANAKA | TAKAAKI | NULL | NULL | JAP | 3 | AO3 | OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION | XIS | Y | | HESS J1800-240B | 270.1124 | -24.0578 | 5.8867537 | -0.376417 | 87.1402 | 54562.3157523148 | 54563.0141666667 | 503026010 | 31672.8 | 30000 | 31672.8 | 31672.8 | 0 | 31672.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26769.8 | 26769.8 | 60320 | 1 | PROCESSED | 54580.1709490741 | 54953 | 54580.1793402778 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030043 | H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region. | GALACTIC DIFFUSE EMISSION | 5 | A | TANAKA | TAKAAKI | NULL | NULL | JAP | 3 | AO3 | OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION | XIS | Y | | HESS J1800-240C | 269.7173 | -24.0469 | 5.71665641 | -0.05804766 | 87.3071 | 54563.0147337963 | 54563.6877662037 | 503027010 | 30975.5 | 30000 | 30975.5 | 30975.5 | 0 | 30975.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27815.5 | 27815.5 | 58123.9 | 1 | PROCESSED | 54580.1815277778 | 54953 | 54580.1897453704 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030043 | H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region. | GALACTIC DIFFUSE EMISSION | 5 | A | TANAKA | TAKAAKI | NULL | NULL | JAP | 3 | AO3 | OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION | XIS | Y | | HESS J1825-137 | 276.5024 | -13.9965 | 17.60816681 | -0.84042551 | 271.0002 | 54754.9096064815 | 54756.458599537 | 503028010 | 57210.4 | 50000 | 57210.4 | 57210.4 | 0 | 57210.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51548.5 | 51548.5 | 133793.8 | 1 | PROCESSED | 54777.9353125 | 55148 | 54780.7053703704 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030044 | The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons. | GALACTIC DIFFUSE EMISSION | 5 | B | TANAKA | TAKAAKI | NULL | NULL | JAP | 3 | AO3 | MAPPING OBSERVATIONS OF HESS J1825-137 | XIS | Y | | HESS_J1825-137_2 | 276.1969 | -13.7002 | 17.73170044 | -0.43977824 | 271.0001 | 54756.4591666667 | 54758.1953009259 | 503029010 | 57199.3 | 50000 | 57199.3 | 57199.3 | 0 | 57199.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51185 | 51185 | 149985.8 | 0 | PROCESSED | 54777.9703819444 | 55148 | 54780.5081365741 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030044 | The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons. | GALACTIC DIFFUSE EMISSION | 5 | B | TANAKA | TAKAAKI | NULL | NULL | JAP | 3 | AO3 | MAPPING OBSERVATIONS OF HESS J1825-137 | XIS | Y | | HESS_J1825-137_3 | 276.1966 | -13.9971 | 17.46909054 | -0.57831059 | 271.0001 | 54758.195775463 | 54759.7917476852 | 503030010 | 55499.6 | 50000 | 55499.6 | 55499.6 | 0 | 55499.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47325.2 | 47325.2 | 137837.9 | 1 | PROCESSED | 54778.0046064815 | 55148 | 54780.7804050926 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030044 | The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons. | GALACTIC DIFFUSE EMISSION | 5 | B | TANAKA | TAKAAKI | NULL | NULL | JAP | 3 | AO3 | MAPPING OBSERVATIONS OF HESS J1825-137 | XIS | Y | | VELA JR P19 | 133.9797 | -46.1476 | 266.55257885 | -0.58147519 | 346.9993 | 54650.629849537 | 54651.2362731482 | 503031010 | 19817.4 | 10000 | 19817.4 | 19817.4 | 0 | 19817.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17156.4 | 17156.4 | 52383.9 | 1 | PROCESSED | 54665.2314699074 | 55036 | 54665.3240393518 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P20 | 133.6175 | -46.3272 | 266.52787238 | -0.88873335 | 346.9997 | 54651.2368402778 | 54651.5828009259 | 503032010 | 16823.7 | 10000 | 16823.7 | 16831.7 | 0 | 16831.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14798.2 | 14798.2 | 29887.9 | 0 | PROCESSED | 54665.19875 | 55036 | 54665.3228125 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P21 | 133.1972 | -46.3295 | 266.34323773 | -1.11269222 | 347.0005 | 54651.5833680556 | 54652.0557175926 | 503033010 | 14287.2 | 10000 | 14295.2 | 14287.2 | 0 | 14303.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12066.5 | 12066.5 | 40801.9 | 1 | PROCESSED | 54665.2108796296 | 55036 | 54665.3234375 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P22 | 132.4428 | -46.6127 | 266.23093455 | -1.69368029 | 346.9992 | 54652.0565625 | 54652.3891087963 | 503034010 | 15264.3 | 10000 | 15264.3 | 15270.9 | 0 | 15270.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14971.7 | 14971.7 | 28728 | 0 | PROCESSED | 54670.1272685185 | 55036 | 54670.1353125 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P23 | 132.7881 | -46.3947 | 266.21323714 | -1.3716571 | 347.0013 | 54652.3896759259 | 54652.7710416667 | 503035010 | 15690.1 | 10000 | 15698.1 | 15690.1 | 0 | 15706.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11039 | 11039 | 32943.9 | 1 | PROCESSED | 54664.2194907407 | 55031 | 54664.7904513889 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P24 | 132.0303 | -46.6729 | 266.0989339 | -1.95139979 | 347.001 | 54652.7719328704 | 54653.1668865741 | 503036010 | 12373.5 | 10000 | 12373.5 | 12373.5 | 0 | 12373.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12254.8 | 12254.8 | 34120 | 1 | PROCESSED | 54679.3105671296 | 55048 | 54679.3185763889 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P25 | 132.5224 | -46.8921 | 266.48184745 | -1.82836861 | 347.0024 | 54653.1675462963 | 54653.4335532407 | 503037010 | 13160 | 10000 | 13160 | 13160 | 0 | 13160 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12432.5 | 12432.5 | 22975.9 | 0 | PROCESSED | 54679.3099884259 | 55048 | 54679.3166203704 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P26 | 132.8787 | -46.6693 | 266.46476457 | -1.49839932 | 347.0019 | 54653.4341203704 | 54653.837025463 | 503038010 | 14553 | 10000 | 14553 | 14553 | 0 | 14553 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10953.6 | 10953.6 | 34783.9 | 0 | PROCESSED | 54679.3635300926 | 55048 | 54679.3709606482 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P27 | 133.2844 | -46.6061 | 266.59417196 | -1.24373956 | 347.0008 | 54653.8375925926 | 54654.1668865741 | 503039010 | 11033.7 | 10000 | 11041.7 | 11041.7 | 0 | 11033.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11337.2 | 11337.2 | 28447.9 | 0 | PROCESSED | 54679.3267824074 | 55048 | 54679.3497222222 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P28 | 133.7109 | -46.6037 | 266.78076878 | -1.01777641 | 347.0004 | 54654.1674537037 | 54654.4259143518 | 503040010 | 13093 | 10000 | 13101 | 13093 | 0 | 13101 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12054 | 12054 | 22296 | 0 | PROCESSED | 54679.3607291667 | 55048 | 54679.3674421296 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P29 | 134.0711 | -46.43 | 266.80859879 | -0.71638658 | 347 | 54654.4264814815 | 54654.7203703704 | 503041010 | 11368.5 | 10000 | 11380.2 | 11368.5 | 0 | 11380.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8222.5 | 8222.5 | 25367.9 | 0 | PROCESSED | 54679.388599537 | 55048 | 54679.3958217593 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P30 | 134.1665 | -46.7036 | 267.059354 | -0.84402772 | 347.0006 | 54654.7208449074 | 54655.0844328704 | 503042010 | 10115.9 | 10000 | 10115.9 | 10115.9 | 0 | 10115.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10053.6 | 10053.6 | 31383.9 | 0 | PROCESSED | 54679.3883912037 | 55048 | 54679.397962963 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P31 | 133.8003 | -46.8845 | 267.03483855 | -1.15221367 | 347.0003 | 54655.085 | 54655.3273032407 | 503043010 | 11209.5 | 10000 | 11217.5 | 11225.5 | 0 | 11209.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11542 | 11542 | 20927.9 | 0 | PROCESSED | 54679.3658217593 | 55048 | 54679.372974537 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P32 | 133.3695 | -46.8865 | 266.8467839 | -1.37881435 | 347.0018 | 54655.3279166667 | 54655.5648032407 | 503044010 | 11264.9 | 10000 | 11272.9 | 11264.9 | 0 | 11280.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8337.5 | 8337.5 | 20455.9 | 0 | PROCESSED | 54679.3747569444 | 55048 | 54679.381087963 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P33 | 133.4681 | -47.1616 | 267.10091899 | -1.50393046 | 347.0007 | 54655.5652777778 | 54656.0084837963 | 503045010 | 12015.5 | 10000 | 12015.5 | 12015.5 | 0 | 12015.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11011.6 | 11011.6 | 38289.9 | 0 | PROCESSED | 54679.4111342593 | 55048 | 54679.4195601852 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P34 | 132.1138 | -46.9499 | 266.35035002 | -2.0812575 | 347.0005 | 54656.0096990741 | 54656.2634143518 | 503046010 | 11042.1 | 10000 | 11058.1 | 11042.1 | 0 | 11058.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11130.6 | 11130.6 | 21916 | 0 | PROCESSED | 54670.2165740741 | 55037 | 54670.2236342593 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P35 | 132.966 | -46.9473 | 266.71715615 | -1.62954887 | 347.0008 | 54656.2642592593 | 54656.5141087963 | 503047010 | 11562.1 | 10000 | 11586.1 | 11562.1 | 0 | 11594.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9619.8 | 9619.8 | 21583.9 | 0 | PROCESSED | 54670.2250694444 | 55037 | 54670.2319212963 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P36 | 133.0606 | -47.2239 | 266.97132611 | -1.75647675 | 346.9998 | 54656.5145833333 | 54656.9168634259 | 503048010 | 11122.6 | 10000 | 11130.6 | 11122.6 | 0 | 11138.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9383.8 | 9383.8 | 34749.9 | 1 | PROCESSED | 54670.2613194444 | 55037 | 54670.2692361111 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P37 | 132.6136 | -47.1701 | 266.73640279 | -1.95651055 | 346.9993 | 54656.9174768518 | 54657.2418287037 | 503049010 | 12529.4 | 10000 | 12541.4 | 12529.4 | 0 | 12545.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12852.7 | 12852.7 | 28020 | 0 | PROCESSED | 54670.2703240741 | 55037 | 54670.278900463 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | VELA JR P38 | 132.2003 | -47.2308 | 266.60579829 | -2.21244802 | 347.0003 | 54657.2423958333 | 54657.5209953704 | 503050010 | 14043.6 | 10000 | 14043.6 | 14043.6 | 0 | 14059.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11426 | 11426 | 24063.9 | 0 | PROCESSED | 54670.249849537 | 55037 | 54670.2561111111 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | | WESTERLUND 2 | 156.0088 | -57.7448 | 284.2643696 | -0.3172737 | 343.7602 | 54687.6527199074 | 54689.327962963 | 503053010 | 73670 | 100000 | 73670 | 73670 | 0 | 73670 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86577.6 | 86577.6 | 144729.8 | 0 | PROCESSED | 54706.4623263889 | 55252 | 54706.476412037 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030059 | Although young open clusters with many massive stars have been recognized as gamma-ray sources, the emission mechanism of the gamma-ray is hardly known. We propose a Suzaku observation of an open cluster Westerlund 2 (RCW 49), from which gamma-ray emission has been detected with H.E.S.S. We observe this cluster to detect X-ray nonthermal emission from open clusters with TeV gamma-ray emission for the first time. We try to find out whether the emission comes from electrons or protons, and discuss the particle acceleration in open clusters. | GALACTIC DIFFUSE EMISSION | 5 | A | FUJITA | YUTAKA | NULL | NULL | JAP | 3 | AO3 | NONTHERMAL EMISSION FROM AN OPEN CLUSTER WESTERLUND 2 | XIS | Y | | WESTERLUND 2 | 155.9878 | -57.7462 | 284.25564056 | -0.32444098 | 166.5036 | 54866.5949189815 | 54867.1669444444 | 503053020 | 33492.4 | 30000 | 33500.4 | 33492.4 | 0 | 33500.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32073 | 32073 | 49415.9 | 1 | PROCESSED | 54963.3371180556 | 55329 | 54880.5574189815 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030059 | Although young open clusters with many massive stars have been recognized as gamma-ray sources, the emission mechanism of the gamma-ray is hardly known. We propose a Suzaku observation of an open cluster Westerlund 2 (RCW 49), from which gamma-ray emission has been detected with H.E.S.S. We observe this cluster to detect X-ray nonthermal emission from open clusters with TeV gamma-ray emission for the first time. We try to find out whether the emission comes from electrons or protons, and discuss the particle acceleration in open clusters. | GALACTIC DIFFUSE EMISSION | 5 | A | FUJITA | YUTAKA | NULL | NULL | JAP | 3 | AO3 | NONTHERMAL EMISSION FROM AN OPEN CLUSTER WESTERLUND 2 | XIS | Y | | RCW 38 | 134.7638 | -47.5154 | 267.93999829 | -1.06526988 | 109.8553 | 54788.5064351852 | 54790.699525463 | 503054010 | 81537.7 | 80000 | 81549.5 | 81537.7 | 0 | 81541.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60928.1 | 60928.1 | 189459.7 | 1 | PROCESSED | 54802.3985416667 | 55171 | 54811.741099537 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030069 | We propose to make Suzaku observation of HII region RCW 38 for 80 ksec in order to study non-thermal phenomena in a massive star-forming region. The region is thought to be a site of high energy particle acceleration by interaction of strong stellar wind from high-mass stars. The main purpose is to observe extended emission from RCW 38. The high resolution spectroscopy by XIS enables us to distinguish non-thermal emission from thermal component and to obtain properties of non-thermal component. In addition, HXD will detect non-thermal radiation from RCW 38. | GALACTIC DIFFUSE EMISSION | 5 | C | ODAKA | HIROKAZU | NULL | NULL | JAP | 3 | AO3 | SEARCH FOR NONTHERMAL RADIATION FROM MASSIVE STAR-FORMING REGION RCW 38 | XIS | Y | | CYGNUS LOOP (P11) | 312.4425 | 31.5127 | 74.4826992 | -7.83027866 | 49.9999 | 54595.9014814815 | 54596.7391087963 | 503055010 | 31894.7 | 25000 | 31902.7 | 31894.7 | 0 | 31910.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25073.8 | 25073.8 | 72359.9 | 0 | PROCESSED | 54606.1312731482 | 54972 | 54606.1436342593 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | | CYGNUS LOOP (P20) | 311.9894 | 31.1824 | 73.97872298 | -7.73281487 | 50.0002 | 54596.7397685185 | 54597.51 | 503056010 | 30112.9 | 25000 | 30112.9 | 30134.3 | 0 | 30120.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27205.7 | 27205.7 | 66533.9 | 0 | PROCESSED | 54606.1028819444 | 54972 | 54606.1121759259 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | | CYGNUS LOOP (P21) | 313.196 | 32.4197 | 75.60030214 | -7.75821821 | 61.9243 | 54619.9401967593 | 54620.2975 | 503057010 | 16170.3 | 15000 | 16178.3 | 16170.3 | 0 | 16178.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12890.3 | 12890.3 | 30863.9 | 0 | PROCESSED | 54636.2162615741 | 55003 | 54636.2238078704 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | | CYGNUS LOOP (P22) | 312.8353 | 32.4047 | 75.39493092 | -7.53123997 | 61.4354 | 54620.2981134259 | 54620.7522453704 | 503058010 | 19287.3 | 15000 | 19287.3 | 19287.3 | 0 | 19287.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17220.3 | 17220.3 | 39212 | 0 | PROCESSED | 54636.272337963 | 55003 | 54636.2807638889 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | | CYGNUS LOOP (P23) | 312.4772 | 32.3587 | 75.1675214 | -7.32455162 | 61.8892 | 54620.7530439815 | 54621.1473842593 | 503059010 | 19457 | 15000 | 19457 | 19457 | 0 | 19457 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17277.1 | 17277.1 | 34063.9 | 0 | PROCESSED | 54636.2250347222 | 55003 | 54636.2328240741 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | | CYGNUS LOOP (P24) | 312.134 | 32.2905 | 74.93132331 | -7.14055521 | 61.3941 | 54621.1479513889 | 54621.6271875 | 503060010 | 18504.6 | 15000 | 18504.6 | 18504.6 | 0 | 18504.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14999 | 14999 | 41397.9 | 1 | PROCESSED | 54636.2930787037 | 55003 | 54637.4594675926 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | | CYGNUS LOOP (P25) | 311.8608 | 32.1678 | 74.68970828 | -7.03578766 | 60.8878 | 54621.6278472222 | 54622.1488888889 | 503061010 | 25995.9 | 20000 | 25995.9 | 25995.9 | 0 | 25995.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23879.1 | 23879.1 | 45010 | 0 | PROCESSED | 54636.2414351852 | 55003 | 54636.2508217593 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | | CYGNUS LOOP (P26) | 314.1252 | 30.3135 | 74.46090737 | -9.70687059 | 49.7995 | 54599.1203587963 | 54599.5474421296 | 503062010 | 16924.7 | 15000 | 16924.7 | 16932.7 | 0 | 16932.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15441 | 15441 | 36892 | 1 | PROCESSED | 54609.1213078704 | 54975 | 54609.1293981482 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | | CYGNUS LOOP (P27) | 313.8328 | 30.0104 | 74.06049539 | -9.7037521 | 49.6211 | 54599.5480092593 | 54600.0494675926 | 503063010 | 22784.3 | 20000 | 22792.3 | 22784.3 | 0 | 22800.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20068.8 | 20068.8 | 43323.9 | 0 | PROCESSED | 54609.1316898148 | 54975 | 54609.1396990741 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | | CYGNUS LOOP (P28) | 313.4797 | 29.8934 | 73.77252886 | -9.54040793 | 49.1005 | 54600.0501273148 | 54600.5334953704 | 503064010 | 18169.3 | 15000 | 18177.3 | 18185.3 | 0 | 18169.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16443 | 16443 | 41756 | 0 | PROCESSED | 54609.1814814815 | 54975 | 54609.1904282407 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | | RABBIT | 214.6544 | -60.9713 | 313.31134091 | 0.131367 | 105.7763 | 54876.850787037 | 54877.5224421296 | 503071010 | 21274 | 20000 | 21282 | 21274 | 0 | 21290 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18012.6 | 18012.6 | 57984 | 0 | PROCESSED | 54962.2228356482 | 55330 | 54892.945162037 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030076 | K3/PSR J1420-6048 is one of the TeV gamma-ray pulsar wind nebulae detected by HESS, which are thought to be main particle accelerators to the Galactic Cosmic rays. It was also detected by EGRET and its X-ray spectrum is very hard. In order to reveal the radiation mechanism, we propose to observe the extended source for 50 ksec on HXD nominal position and contamination source for 20 ksec on XIS nominal position. The main purpose of this observation is to obtain the hard X-ray spectrum up to about 40 keV. | GALACTIC DIFFUSE EMISSION | 5 | C | KISHISHITA | TETSUICHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF TEV GAMMA-RAY PWN K3/PSR J1420-6048 | XIS | Y | | EXTENDED CHIMNEY | 265.9856 | -29.2095 | 359.57541621 | 0.16970004 | 69.9995 | 54896.1105555556 | 54899.1218171296 | 503072010 | 140573.3 | 133000 | 140573.3 | 140573.3 | 0 | 140573.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 135478.4 | 135478.4 | 260128 | 1 | PROCESSED | 54963.3178935185 | 55330 | 54916.5067361111 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030086 | We have discovered a chimney structure in the Sgr C region with Suzaku. The Suzaku spectrum of the chimney shows typical parameters of a super nova remnant. However, the chimney has a linear shape, which is inconsistent with a SNR. Thus, we are considering that the chimney is a blowout from super bubble in the Sgr C region. Another possible scenario is that the chimney would be a part of a shell structure formed by explosions (starburst activities, Sgr A*, magnetic reconnection) in the region of Sgr A and Sgr C. Thus, in this proposal, we would like to investigate the structure extending from the chimney. | GALACTIC DIFFUSE EMISSION | 5 | B | TSURU | TAKESHI | NULL | NULL | JAP | 3 | AO3 | THE CHIMNEY OF SGR C : A PART OF A SUPER BUBBLE = A SUPER SHELL ? | XIS | Y | | HESSJ1614-A | 243.5214 | -52.1022 | 331.29897546 | -0.76107386 | 283.3889 | 54729.7629050926 | 54730.562662037 | 503073010 | 53649.4 | 50000 | 53657.4 | 53649.4 | 0 | 53665.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40871.3 | 40871.3 | 69071.9 | 0 | PROCESSED | 54777.4405092593 | 55148 | 54780.4246990741 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030088 | The TeV image of HESSJ1614-518 is double peaked, and we observed one of them during the AO-1 with the Suzaku XIS. We discovered extended X-ray emission which coincides with the TeV emission. Then we propose to observe the other peak. We also found a bright object between the double peaks. HESSJ1614 may be a pulsar wind nebula, and the object may be a pulsar driving the nebula. However, the object was just at the edge of the XIS field of view, we could not study it in detail. Then, we propose another position to observe the object. Furthermore, we discovered soft diffuse emission around HESSJ1614. We propose the other position to study the spatial extension of the diffuse emission. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | MAPPING OBSERVATION OF HESSJ1614-518 | XIS | Y | | HESSJ1614-B | 243.5783 | -51.8962 | 331.46625372 | -0.63583262 | 283.7142 | 54730.5632291667 | 54731.2779166667 | 503074010 | 52634.2 | 50000 | 52642.2 | 52634.2 | 0 | 52634.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42953 | 42953 | 61735.9 | 0 | PROCESSED | 54777.6201157407 | 55148 | 54780.4609490741 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 030088 | The TeV image of HESSJ1614-518 is double peaked, and we observed one of them during the AO-1 with the Suzaku XIS. We discovered extended X-ray emission which coincides with the TeV emission. Then we propose to observe the other peak. We also found a bright object between the double peaks. HESSJ1614 may be a pulsar wind nebula, and the object may be a pulsar driving the nebula. However, the object was just at the edge of the XIS field of view, we could not study it in detail. Then, we propose another position to observe the object. Furthermore, we discovered soft diffuse emission around HESSJ1614. We propose the other position to study the spatial extension of the diffuse emission. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | MAPPING OBSERVATION OF HESSJ1614-518 | XIS | Y | | LOW_LATITUDE_97-10 | 311.8076 | 60.1112 | 96.61384914 | 10.40907029 | 101.0346 | 54571.1324652778 | 54572.8890509259 | 503075010 | 79811.9 | 80000 | 79819.9 | 79827.9 | 0 | 79811.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80810.5 | 80810.5 | 151749.8 | 2 | PROCESSED | 54581.3064236111 | 54953 | 54581.3271643518 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030105 | Suzaku observations of diffuse background emission indicate galactic-latitude dependence of OVII intensity. The result of our AO-2 observation strongly supports this dependence. This suggests that the major part of the emission is originating from the halo or the extended disk of our galaxy. In order to confirm the galactic-latitude dependency and to constrain the spatial distribution of the OVII emitting gas, we propose to observe diffuse radiation at a low galactic latitude of ~ 10 deg. | GALACTIC DIFFUSE EMISSION | 5 | B | YOSHINO | TOMOTAKA | NULL | NULL | JAP | 3 | AO3 | RESOLVING LARGE-SCALE SPATIAL DEPENDENCE OF SOFT X-RAY DIFFUSE EMISSION | XIS | Y | | HESSJ1741-A | 265.3548 | -30.1316 | 358.50289854 | 0.15030933 | 73.8229 | 54886.7117013889 | 54888.0419328704 | 503076010 | 52932.3 | 50000 | 52932.3 | 52932.3 | 0 | 52932.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43770.8 | 43770.8 | 114915.8 | 1 | PROCESSED | 54963.002025463 | 55330 | 54902.4869791667 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030113 | HESSJ1741-302 is one of the most darkest TeV unidentified objects which was discovered with the H.E.S.S. telescope recently. The location strongly suggests that the object is physically connected to the diffuse TeV gamma-ray emission along the Galactic plane. On the other hand, there is a pulsar near the object, and it may be an off-set pulsar wind nebula. To clarify the origin of the object, we propose to the observation of HESSJ1741. | GALACTIC DIFFUSE EMISSION | 5 | C | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302 | XIS | Y | | HESSJ1741-B | 265.2407 | -30.3098 | 358.29952005 | 0.1396669 | 74.0024 | 54888.0423611111 | 54889.4828587963 | 503077010 | 51261.6 | 50000 | 51269.6 | 51261.6 | 0 | 51269.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43707.2 | 43707.2 | 124423.9 | 1 | PROCESSED | 54962.9170949074 | 55330 | 54908.5791550926 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030113 | HESSJ1741-302 is one of the most darkest TeV unidentified objects which was discovered with the H.E.S.S. telescope recently. The location strongly suggests that the object is physically connected to the diffuse TeV gamma-ray emission along the Galactic plane. On the other hand, there is a pulsar near the object, and it may be an off-set pulsar wind nebula. To clarify the origin of the object, we propose to the observation of HESSJ1741. | GALACTIC DIFFUSE EMISSION | 5 | C | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302 | XIS | Y | | HESS_J1809-193_N | 272.4044 | -19.3551 | 11.02929838 | 0.07166066 | 112.001 | 54556.5874421296 | 54557.6877662037 | 503078010 | 51530.9 | 40000 | 51538.9 | 51530.9 | 0 | 51546.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34818.6 | 34818.6 | 95051.8 | 2 | PROCESSED | 54571.3490509259 | 54950 | 54571.3638888889 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030126 | A survey of the Galactic plane with H.E.S.S. has revealed the existance of several new very-high-energy (VHE) gamma-ray sources. As gamma rays are produced by interactions of relativistic particles, observing VHE emission reveals the acceleration sites of particles. Although it had been thought that such acceleration occur in the shock of SNR, it became clear that several VHE sources are pulsar wind nebulae (PWNe). This indicates that PWNe are also the acceleration sites of particles. HESS J1809-193 is a diffuse and a pulsar wind nebula candidate source, but details of the VHE emission mechanisms have been unclear yet. With the high sensitivity of XIS, we investigate spatial distribution of the spectrum around HESS J1809-193 and reveal its nature and the VHE emission mechanism. | GALACTIC DIFFUSE EMISSION | 5 | A | ANADA | TAKAYASU | NULL | NULL | JAP | 3 | AO3 | INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193 | XIS | Y | | HESS_J1809-193_S | 272.3365 | -19.5311 | 10.84429394 | 0.04252392 | 106.4999 | 54557.6901851852 | 54558.6161805556 | 503079010 | 44248.1 | 40000 | 44248.1 | 44248.1 | 0 | 44248.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32214.2 | 32214.2 | 79969.8 | 1 | PROCESSED | 54570.1730208333 | 54950 | 54570.1866666667 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030126 | A survey of the Galactic plane with H.E.S.S. has revealed the existance of several new very-high-energy (VHE) gamma-ray sources. As gamma rays are produced by interactions of relativistic particles, observing VHE emission reveals the acceleration sites of particles. Although it had been thought that such acceleration occur in the shock of SNR, it became clear that several VHE sources are pulsar wind nebulae (PWNe). This indicates that PWNe are also the acceleration sites of particles. HESS J1809-193 is a diffuse and a pulsar wind nebula candidate source, but details of the VHE emission mechanisms have been unclear yet. With the high sensitivity of XIS, we investigate spatial distribution of the spectrum around HESS J1809-193 and reveal its nature and the VHE emission mechanism. | GALACTIC DIFFUSE EMISSION | 5 | A | ANADA | TAKAYASU | NULL | NULL | JAP | 3 | AO3 | INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193 | XIS | Y | | CAS A | 351.0231 | 59.0265 | 111.88943817 | -1.95981315 | 208.1115 | 54876.0965740741 | 54876.8363310185 | 503080010 | 30035.5 | 30000 | 30035.5 | 30035.5 | 0 | 30035.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30073.1 | 30073.1 | 63913.9 | 0 | PROCESSED | 54963.3651388889 | 55330 | 54892.9889699074 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030127 | Cas A is the youngest supernova remnant(SNR) in our Galaxy. Recently, the Spitzer Space Telescope discovered moving structures nearly at the speed of light outside the shell of the SNR. These structures are likely infrared echoes, where interstellar dust is heated by the outward moving photon shell of a bright flash. The bright flash is probably due to a giant flare from the central point source of Cas A, and if so, it requires that the central point source is a magnetar. Magnetars are known to emit luminous flares in the X-ray band, so it is expected that we can detect Fe-K fluorescence emission accompanied by IR echo. Here, we propose to observe on IR-emitting cloud around Cas A for 30ks to search for Fe-K emission which is naturally expected if the central point source is a magnetar. | GALACTIC DIFFUSE EMISSION | 5 | C | AONO | HIROYUKI | NULL | NULL | JAP | 3 | AO3 | INVESTIGATION OF A X-RAY ECHO NEAR THE SUPERNOVA REMNANT CASSIOPEIA A | XIS | Y | | GC(0,-1.6) | 268.0544 | -29.7594 | 0.03481768 | -1.65633011 | 65.7488 | 54899.6540509259 | 54900.8168865741 | 503081010 | 59223.3 | 50000 | 59223.3 | 59223.3 | 0 | 59223.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57601.8 | 57601.8 | 100453.8 | 1 | PROCESSED | 54963.2991782407 | 55330 | 54916.3813194444 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030131 | We propose a 50 ksec observation of very enigmatic diffuse structure at 1.6 degree south from the Galactic center. We first discovered this structure with ROSAT. Then with ASCA, we found that the spectrum exhibits thin thermal emission accompanied with a hard tail which may be nonthermal radiation from high energy electrons. These results imply presence of a strong shock in this region, possibly due to a jet from Sgr A*. The diffuse emission may be a fossil of the past activities. With the observation of Suzaku, we obtain the richest statistics ever achieved. Then we will reveal the shock front from the image, and verify the past activities of the massive blackhole. | GALACTIC DIFFUSE EMISSION | 5 | B | MURAKAMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | NEW EVIDENCE OF THE PAST ACTIVITY IN THE GALACTIC CENTER REGION | XIS | Y | | VICINITY_OF_PKS_2155-1 | 329.2367 | -30.5281 | 17.16872193 | -51.86657338 | 55.8337 | 54585.7726736111 | 54588.3542592593 | 503082010 | 90181.2 | 80000 | 90181.2 | 90181.2 | 0 | 90181.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76792.1 | 76792.1 | 223023.7 | 4 | PROCESSED | 54608.3057291667 | 54975 | 54608.3373726852 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030135 | The highly ionized absorption lines of OVII, OVIII, and NeIX at z = 0 have been unambiguously detected toward the bright AGN PKS 2155-304 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII, OVIII and NeIX emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas. | GALACTIC DIFFUSE EMISSION | 5 | A | HAGIHARA | TOSHISHIGE | NULL | NULL | JAP | 3 | AO3 | STUDY OF WARM-HOT GAS TOWARD PKS 2155-304 | XIS | Y | | VICINITY_OF_PKS_2155-2 | 330.1861 | -29.9649 | 18.22929909 | -52.62033555 | 55.8323 | 54588.3553356482 | 54590.7293865741 | 503083010 | 87327.4 | 80000 | 87327.4 | 87327.4 | 0 | 87327.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75845.1 | 75845.1 | 205105.9 | 3 | PROCESSED | 54608.235625 | 54975 | 54608.2608912037 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 030135 | The highly ionized absorption lines of OVII, OVIII, and NeIX at z = 0 have been unambiguously detected toward the bright AGN PKS 2155-304 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII, OVIII and NeIX emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas. | GALACTIC DIFFUSE EMISSION | 5 | A | HAGIHARA | TOSHISHIGE | NULL | NULL | JAP | 3 | AO3 | STUDY OF WARM-HOT GAS TOWARD PKS 2155-304 | XIS | Y | | W49B | 287.7847 | 9.1157 | 43.28157058 | -0.18360003 | 89.2671 | 54919.1063888889 | 54920.4689583333 | 503084010 | 52154.9 | 40000 | 52154.9 | 52154.9 | 0 | 52154.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43951.2 | 43951.2 | 117709.9 | 2 | PROCESSED | 54963.0818171296 | 55330 | 54931.3622106482 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 030142 | Observations of the W49B supernova remnant for 40 ks is proposed to reveal whether it is a remnant of an anomalous Type Ia supernova or not. To determine the type of the supernova, detailed measurement of less abundand elements such as Cr and Mn will be performed, and abundance of Ni and Ti will be examined. The abundance pattern of those elements in W49B will be compared to that of Tycho's SNR we measured by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | C | TAMAGAWA | TORU | NULL | NULL | JAP | 3 | AO3 | IS W49B A REMNANT OF AN ANOMALOUS TYPE IA SUPERNOVA? | XIS | Y | | TYCHO SNR | 6.3139 | 64.1469 | 120.08177164 | 1.42013769 | 53.7834 | 54682.0646759259 | 54686.9529398148 | 503085010 | 312892 | 400000 | 312916 | 312892 | 0 | 312908 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 289949.4 | 289949.4 | 307869.9 | 3 | PROCESSED | 54706.9683680556 | 54557 | 54707.038287037 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 031003 | Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times. | GALACTIC DIFFUSE EMISSION | 5 | A | HUGHES | JOHN | NULL | NULL | USA | 3 | AO3 | SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS | XIS | Y | | TYCHO SNR | 6.3115 | 64.1447 | 120.08050675 | 1.41805528 | 43.1557 | 54689.3425578704 | 54690.918275463 | 503085020 | 102855.6 | 100000 | 102855.6 | 102855.6 | 0 | 102855.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91907.8 | 91907.8 | 136103.9 | 1 | PROCESSED | 54706.7655555556 | 54557 | 54706.7896412037 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 031003 | Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times. | GALACTIC DIFFUSE EMISSION | 5 | A | HUGHES | JOHN | NULL | NULL | USA | 3 | AO3 | SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS | XIS | Y | | G18.0-0.7 | 276.56 | -13.5781 | 18.00442084 | -0.69482715 | 92.0001 | 54909.8982060185 | 54911.080775463 | 503086010 | 52059.2 | 50000 | 52059.2 | 52067.2 | 0 | 52067.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46303.6 | 46303.6 | 102145.8 | 2 | PROCESSED | 54962.5928009259 | 55329 | 54923.3684490741 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031203 | By studying pulsar wind nebulae, the synchrotron nebulae powered by a neutron star's loss of rotational energy, it is possible to determine the energetics of both the progenitor supernova and central neutron star. This requires estimates of the expansion velocity and mass swept-up the pulsar wind nebulae, best obtained by analyzing the spectrum of the thermal X-rays emitting by this material. In the proposal, we request a 50ks observation of four of the most energetic pulsar wind nebulae in the Milky Way to both detect such thermal X-ray emission and use the measured spectral properties to infer the ejecta mass and kinetic energy of their progenitor supernova and the initial spin period of the central neutron star -- all currently unmeasurable using the currently available information. | GALACTIC DIFFUSE EMISSION | 5 | C | GELFAND | JOSEPH | NULL | NULL | USA | 3 | AO3 | STUDYING THE PROGENITOR SUPERNOVA AND CENTRAL NEUTRON STAR OF PULSAR WIND NEBULAE | XIS | Y | | G12.8-0.0 | 273.3975 | -17.831 | 12.81826803 | -0.01988984 | 90.5577 | 54894.8233680556 | 54896.1050810185 | 503087010 | 56202.6 | 50000 | 56202.6 | 56202.6 | 0 | 56205.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51531.2 | 51531.2 | 110727.8 | 1 | PROCESSED | 54963.0907986111 | 55329 | 54908.5701388889 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031203 | By studying pulsar wind nebulae, the synchrotron nebulae powered by a neutron star's loss of rotational energy, it is possible to determine the energetics of both the progenitor supernova and central neutron star. This requires estimates of the expansion velocity and mass swept-up the pulsar wind nebulae, best obtained by analyzing the spectrum of the thermal X-rays emitting by this material. In the proposal, we request a 50ks observation of four of the most energetic pulsar wind nebulae in the Milky Way to both detect such thermal X-ray emission and use the measured spectral properties to infer the ejecta mass and kinetic energy of their progenitor supernova and the initial spin period of the central neutron star -- all currently unmeasurable using the currently available information. | GALACTIC DIFFUSE EMISSION | 5 | C | GELFAND | JOSEPH | NULL | NULL | USA | 3 | AO3 | STUDYING THE PROGENITOR SUPERNOVA AND CENTRAL NEUTRON STAR OF PULSAR WIND NEBULAE | XIS | Y | | B1920+10(1) | 293.0298 | 10.9618 | 47.34140504 | -3.87470613 | 252.2888 | 54772.350462963 | 54774.137662037 | 503090010 | 73603.3 | 70000 | 73612.4 | 73603.3 | 0 | 73611.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 66668.2 | 66668.2 | 154403.9 | 3 | PROCESSED | 54788.2123263889 | 55154 | 54788.4472337963 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 031204 | A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps. | GALACTIC DIFFUSE EMISSION | 5 | C | MISANOVIC | ZDENKA | NULL | NULL | USA | 3 | AO3 | STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU | XIS | Y | | B1920+10(2) | 292.8971 | 10.8605 | 47.18977478 | -3.80874006 | 248.6642 | 54783.7420833333 | 54785.8981365741 | 503091010 | 100457.7 | 100000 | 100457.7 | 100457.7 | 0 | 100457.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93873.1 | 93873.1 | 186248 | 0 | PROCESSED | 54797.1290856482 | 55167 | 54797.1537731482 | 2.2.11.22 | 1 | Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 | 031204 | A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps. | GALACTIC DIFFUSE EMISSION | 5 | C | MISANOVIC | ZDENKA | NULL | NULL | USA | 3 | AO3 | STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU | XIS | Y | | HESS J1023-575 | 155.5616 | -57.7533 | 284.06754503 | -0.45248582 | 284.3289 | 54617.1411458333 | 54617.4515509259 | 503092010 | 13826 | 10000 | 13826 | 13826 | 0 | 13826 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11057.3 | 11057.3 | 26815.9 | 1 | PROCESSED | 54630.1961574074 | 54999 | 54633.6961458333 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 031207 | We propose to search the neighborhood of two extended TeV sources to determine if there are X-ray sources that are potentially pulsar wind nebulae powering them. One source is near the colliding wind binary RCW 49, which has been suggested as the accelerator, and would therefore represent a new source class if there is no other plausible accelerator in the neighborhood. The other is a very bright source first detected by MILAGRO in the Galactic plane, which has been shown to be a large, extended source by HESS. While there is in each case a proposed X-ray counterpart, only a part of each nebula has been imaged in hard X-rays, and so it is unknown if there are other, more plausible counterparts. | GALACTIC DIFFUSE EMISSION | 5 | B | ROBERTS | MALLORY | NULL | NULL | USA | 3 | AO3 | SEARCHING FOR X-RAY COUNTERPARTS OF TWO GALACTIC TEV SOURCES | XIS | Y | | SNR 0049-73.6 | 12.7817 | -73.3677 | 302.96274339 | -43.76053264 | 62.7682 | 54629.4818518518 | 54632.7605787037 | 503094010 | 120478 | 120000 | 120486 | 120478 | 0 | 120486 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 107707.9 | 107707.9 | 283241.9 | 3 | PROCESSED | 54642.5679398148 | 55008 | 54642.6050694444 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 031211 | We propose to observe the O-rich supernova remnant (SNR) 0049-73.6 in the Small Magellanic Cloud (SMC). SNR 0049-73.6 shares some similarities and differences with another O-rich SNR 0103-72.6 in the SMC. High resolution X-ray spectroscopy of these SNRs with Suzaku/XIS observations should provide a useful insight for the details of thermal evolution of a core-collapse SNR. We began this program with an AO1 Suzaku/XIS observation of SNR 0103-72.6. We here propose to continue this program with our AO3 Suzaku observation of 0049-73.6. We request for a 120 ks Suzaku/XIS observation of 0049-73.6. | GALACTIC DIFFUSE EMISSION | 5 | B | PARK | SANGWOOK | NULL | NULL | USA | 3 | AO3 | OXYGEN-RICH SUPERNOVA REMNANT 0049-73.6 IN THE SMC | XIS | Y | | VELA FRAGMENT C | 136.2696 | -44.691 | 266.51473212 | 1.58715492 | 269.3614 | 54580.6978703704 | 54582.3056481482 | 503095010 | 84116.7 | 70000 | 84116.7 | 84116.7 | 0 | 84116.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91354.7 | 91354.7 | 138901.8 | 2 | PROCESSED | 54594.2301273148 | 54960 | 54594.2480324074 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 031212 | Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM. | GALACTIC DIFFUSE EMISSION | 5 | B | GAETZ | TERRANCE | NULL | NULL | USA | 3 | AO3 | SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS | XIS | Y | | VELA FRAGMENT E | 119.9016 | -44.3755 | 259.34445053 | -7.61175769 | 281.1138 | 54582.309224537 | 54583.7849421296 | 503096010 | 79200.4 | 70000 | 79218.9 | 79200.4 | 0 | 79232.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84252.9 | 84252.9 | 127489.9 | 1 | PROCESSED | 54594.1961805556 | 54960 | 54594.2098842593 | 2.2.7.18 | 1 | Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 | 031212 | Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM. | GALACTIC DIFFUSE EMISSION | 5 | B | GAETZ | TERRANCE | NULL | NULL | USA | 3 | AO3 | SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS | XIS | Y | | GCL1 | 265.1726 | -28.5274 | 359.7799359 | 1.13423351 | 69.7267 | 54900.8188425926 | 54901.4557175926 | 503099010 | 29706 | 25000 | 29724.1 | 29722 | 0 | 29706 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30564.9 | 30564.9 | 55020 | 1 | PROCESSED | 54963.1238310185 | 55329 | 54916.3706828704 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | YUSEF-ZADEH | FARHAD | NULL | NULL | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | | GCL2 | 264.8888 | -28.9255 | 359.31035513 | 1.13376438 | 106.9569 | 54905.2789467593 | 54905.9169444444 | 503100010 | 25717.9 | 25000 | 25717.9 | 25717.9 | 0 | 25717.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24146 | 24146 | 55119.9 | 1 | PROCESSED | 54963.2315162037 | 55329 | 54917.3744675926 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | YUSEF-ZADEH | FARHAD | NULL | NULL | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | | GCL3 | 265.2728 | -28.8569 | 359.5469331 | 0.88519 | 106.9023 | 54906.6133912037 | 54907.3252777778 | 503101010 | 33891.1 | 25000 | 33899.1 | 33899.1 | 0 | 33891.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30830.9 | 30830.9 | 61497.9 | 0 | PROCESSED | 54962.8099537037 | 55329 | 54917.3115393518 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | YUSEF-ZADEH | FARHAD | NULL | NULL | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | | GCL4 | 265.3437 | -29.192 | 359.29532739 | 0.65531706 | 106.9407 | 54907.3257986111 | 54908.0711111111 | 503102010 | 33655.4 | 25000 | 33679.4 | 33655.8 | 0 | 33655.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30052.1 | 30052.1 | 64389.9 | 0 | PROCESSED | 54963.2037847222 | 55329 | 54920.054837963 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | YUSEF-ZADEH | FARHAD | NULL | NULL | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | | SLX 1737-282 | 265.2352 | -28.3094 | 359.99405573 | 1.20298654 | 69.9745 | 54901.4562384259 | 54901.8035648148 | 503103010 | 18316 | 10000 | 18332.4 | 18332 | 0 | 18316 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16365.9 | 16365.9 | 30001.9 | 0 | PROCESSED | 54963.2700115741 | 55329 | 54916.9907638889 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | C | YUSEF-ZADEH | FARHAD | NULL | NULL | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | | ARC_BACKGROUND | 39.2055 | -35.7283 | 240.48717091 | -66.02341726 | 233.8071 | 54830.2554861111 | 54835.3468055556 | 503104010 | 201877.5 | 140000 | 201957.5 | 201877.5 | 0 | 201981.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 5502.8 | 5502.8 | 14506 | 0 | PROCESSED | 54959.3581481482 | 55328 | 54851.4354166667 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 031235 | Aside from the lengthy bright arcs in the northern sky, few X-ray bright, high latitude regions are understood. Yet, studying this gas is important for understanding the Galactic halo. Here, we propose to study a medium-sized (~7 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make Suzaku observations of the arc and nearby background. With them and an existing Suzaku observation, we will be able to determine the thermal properties of the arc plasma and if the arc is the bright limb of a hot bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | SHELTON | ROBIN | NULL | NULL | USA | 3 | AO3 | A CLOSER LOOT AT HOT HALO GAS: A SUZAKU STUDY OF AN X-RAY BRIGHT ARC | XIS | Y | | HESS J1718-385 | 259.5578 | -38.4584 | 348.92137939 | -0.45364037 | 266.9006 | 54706.233599537 | 54706.9286342593 | 503108010 | 23509.7 | 20000 | 23509.7 | 23509.7 | 0 | 23509.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19440.2 | 19440.2 | 60047.9 | 1 | PROCESSED | 54720.299849537 | 55093 | 54720.4386689815 | 2.2.8.20 | 1 | Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 | 032026 | HESS J1718-385 is a newly discovered Very High Energy (VHE) source with an unusually hard energy spectrum, close to an energetic pulsar. The classification as a VHE Pulsar Wind Nebula (PWN) was confirmed by observations of the region with XMM-Newton and Suzaku. XMM showed a compact X-ray PWN around the pulsar, whereas Suzaku revealed low surface brightness emission close to the VHE source. To morphologically connect this low surface brightness emission to the X-ray PWN, we propose another short, 20 ksec Suzaku pointing, aiming between the VHE source center and the pulsar location. The data will allow to identify the new Suzaku source with the compact X-ray PWN. The spectra will be used to investigate the unusual particle energy distribution that is derived from the hard VHE spectrum. | GALACTIC DIFFUSE EMISSION | 5 | A | PUEHLHOFER | GERD | NULL | NULL | EUR | 3 | AO3 | SUZAKU OBSERVATIONS OF THE LOW SURFACE BRIGHTNESS X-RAY PULSAR WIND NEBULA CANDIDATE ASSOCIATED WITH HESS J1718-385 | XIS | Y | | K3/PSR J1420-6048 | 215.0274 | -60.7627 | 313.55205119 | 0.26755801 | 90.771 | 54842.5598263889 | 54843.8801388889 | 503110010 | 50269 | 50000 | 50269 | 50269 | 0 | 50269 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 50061.8 | 50061.8 | 114063.9 | 2 | PROCESSED | 54959.4244212963 | 55328 | 54854.3728703704 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 033076 | K3/PSR J1420-6048 is one of the TeV gamma-ray pulsar wind nebulae detected by HESS, which are thought to be main particle accelerators to the Galactic Cosmic rays. It was also detected by EGRET and its X-ray spectrum is very hard. In order to reveal the radiation mechanism, we propose to observe the extended source for 50 ksec on HXD nominal position and contamination source for 20 ksec on XIS nominal position. The main purpose of this observation is to obtain the hard X-ray spectrum up to about 40 keV. | GALACTIC DIFFUSE EMISSION | 5 | C | KISHISHITA | TETSUICHI | ROMANI | ROGER | JUS | 3 | AO3 | SUZAKU OBSERVATION OF TEV GAMMA-RAY PWN K3/PSR J1420-6048 | HXD | Y | | HESS J1745-303A | 265.7791 | -30.3241 | 358.53258375 | -0.26269922 | 103.33 | 55253.3854166667 | 55254.6758796296 | 504001010 | 51153.8 | 50000 | 51161.8 | 51153.8 | 0 | 51168.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42219.6 | 42219.6 | 111458.1 | 1 | PROCESSED | 55267.237337963 | 55636 | 55267.2568634259 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040001 | The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY | XIS | Y | | HESS J1745-303B | 266.0577 | -30.545 | 358.47050833 | -0.58308172 | 102.2921 | 55254.6768634259 | 55255.9515509259 | 504002010 | 53060.9 | 50000 | 53060.9 | 53060.9 | 0 | 53060.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46585 | 46585 | 110121.9 | 1 | PROCESSED | 55267.2540162037 | 55636 | 55267.2715856482 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040001 | The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY | XIS | Y | | HESS J1745-303C | 266.3881 | -30.6242 | 358.55151469 | -0.86700864 | 101.7444 | 55252.1897800926 | 55253.3842476852 | 504003010 | 50906.5 | 50000 | 50914.5 | 50914.5 | 0 | 50906.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41270.8 | 41270.8 | 103187.8 | 3 | PROCESSED | 55264.3705671296 | 55632 | 55264.3901157407 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040001 | The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY | XIS | Y | | SGR_B2 | 266.8776 | -28.4437 | 0.63615824 | -0.0985299 | 266.3663 | 55095.6093518518 | 55096.0418287037 | 504004010 | 10057.2 | 200000 | 10057.2 | 10057.2 | 0 | 10057.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9432.8 | 9432.8 | 37340.9 | 0 | PROCESSED | 55110.1937152778 | 55476 | 55110.2035763889 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040002 | The Galactic center diffuse X-ray emission (GCDX) consists of the hot plasma, neutral iron line, and hard tail. While we have demonstrated the hot plasma truly extending, origins of the others are still under discussion. We found time variability of the neutral Fe line intensity and marginally detected neutral lines of S, Ar, and Ca from Sagittarius B2. Our purpose is to clearly detect the neutral lines of S, Ar, Ca, and time variability of the hard tail of the GCDX up to 40 keV. This observation will resolve the remaining mysteries of the GCDX. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUKAWA | MASAYOSHI | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION- | XIS | Y | | SGR_B2 | 266.8788 | -28.4436 | 0.63679 | -0.09938091 | 266.4718 | 55096.836412037 | 55102.6667592593 | 504004020 | 202094.5 | 200000 | 202094.5 | 202102.5 | 0 | 202094.5 | 3 | 4 | 0 | 3 | 1 | 0 | 0 | 178283.1 | 178283.1 | 303543.7 | 4 | PROCESSED | 55126.8329282407 | 55500 | 55133.4505092593 | 2.4.12.27 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040002 | The Galactic center diffuse X-ray emission (GCDX) consists of the hot plasma, neutral iron line, and hard tail. While we have demonstrated the hot plasma truly extending, origins of the others are still under discussion. We found time variability of the neutral Fe line intensity and marginally detected neutral lines of S, Ar, and Ca from Sagittarius B2. Our purpose is to clearly detect the neutral lines of S, Ar, Ca, and time variability of the hard tail of the GCDX up to 40 keV. This observation will resolve the remaining mysteries of the GCDX. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUKAWA | MASAYOSHI | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION- | XIS | Y | | RIM1 | 311.6421 | 31.883 | 74.34868893 | -7.06658523 | 247.7276 | 55152.9451273148 | 55153.9488888889 | 504005010 | 40747.3 | 38000 | 40747.3 | 40747.3 | 0 | 40747.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34511.2 | 34511.2 | 86715.9 | 0 | PROCESSED | 55166.4741087963 | 55534 | 55166.4923148148 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | RIM2 | 311.426 | 31.5946 | 74.00572356 | -7.09996284 | 246.8661 | 55153.9497337963 | 55154.4843055556 | 504006010 | 26305.9 | 24000 | 26305.9 | 26305.9 | 0 | 26305.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22237 | 22237 | 46183.9 | 0 | PROCESSED | 55166.4350231482 | 55534 | 55166.4447916667 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | RIM3 | 311.3232 | 31.2993 | 73.71675058 | -7.21258663 | 246.4181 | 55154.4849189815 | 55155.1204166667 | 504007010 | 21556.6 | 19000 | 21556.6 | 21556.6 | 0 | 21556.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17481 | 17481 | 54903.9 | 0 | PROCESSED | 55166.4161342593 | 55534 | 55166.4304166667 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | RIM4 | 311.4678 | 31.0131 | 73.56601773 | -7.48621797 | 246.0303 | 55155.1210763889 | 55155.3579166667 | 504008010 | 12102.5 | 10000 | 12102.5 | 12118.5 | 0 | 12110.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8666 | 8666 | 20455.9 | 0 | PROCESSED | 55166.3924189815 | 55534 | 55166.425787037 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | RIM5 | 311.5286 | 30.6813 | 73.33464134 | -7.73161485 | 255.8951 | 55155.3611689815 | 55155.7953356482 | 504009010 | 15850.2 | 15000 | 15850.2 | 15850.2 | 0 | 15850.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12289.1 | 12289.1 | 37503.9 | 0 | PROCESSED | 55166.4004861111 | 55534 | 55166.4265277778 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | RIM6 | 314.3771 | 31.4503 | 75.4881661 | -9.14820234 | 247.047 | 55155.7987615741 | 55156.1745833333 | 504010010 | 14327.5 | 11000 | 14347.5 | 14343.5 | 0 | 14327.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10715.2 | 10715.2 | 32468 | 0 | PROCESSED | 55166.4021180556 | 55534 | 55166.4272916667 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | BLOWOUT1 | 312.2225 | 31.7347 | 74.53998499 | -7.54540267 | 244.0864 | 55158.2754166667 | 55158.9655555556 | 504011010 | 24185.4 | 23000 | 24201.4 | 24185.4 | 0 | 24193.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19476.8 | 19476.8 | 59603.9 | 1 | PROCESSED | 55176.1888541667 | 55545 | 55176.2112731482 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | BLOWOUT2 | 311.9515 | 31.5359 | 74.23825049 | -7.48819964 | 243.427 | 55158.9662615741 | 55159.5106944444 | 504012010 | 26549.4 | 23000 | 26565.4 | 26549.4 | 0 | 26573.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19940.1 | 19940.1 | 47031.9 | 1 | PROCESSED | 55176.2151851852 | 55545 | 55176.2336921296 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | BLOWOUT3 | 311.7021 | 31.3134 | 73.92913651 | -7.4588166 | 242.4356 | 55160.1363888889 | 55160.4723611111 | 504013010 | 16159.9 | 16000 | 16159.9 | 16159.9 | 0 | 16159.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11810.1 | 11810.1 | 29021.9 | 0 | PROCESSED | 55176.2158680556 | 55545 | 55176.2365740741 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | BLOWOUT4 | 312.7282 | 31.6832 | 74.77065214 | -7.91349372 | 242.7253 | 55160.4733564815 | 55161.0044444445 | 504014010 | 17769.6 | 15000 | 17825.7 | 17769.6 | 0 | 17825.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 14265.7 | 14265.7 | 45876 | 0 | PROCESSED | 55176.2561111111 | 55545 | 55176.2692939815 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | BLOWOUT5 | 312.2204 | 31.3402 | 74.2273165 | -7.78955911 | 225.5762 | 55176.0660532407 | 55176.7307175926 | 504015010 | 30406.4 | 25000 | 30406.4 | 30406.4 | 0 | 30406.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28692.1 | 28692.1 | 57423.9 | 0 | PROCESSED | 55189.2573148148 | 55555 | 55189.2693981482 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | BLOWOUT6 | 311.7638 | 30.9468 | 73.67127235 | -7.72686898 | 241.7587 | 55165.8330787037 | 55166.2883449074 | 504016010 | 21000 | 19000 | 21008 | 21016 | 0 | 21000 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17712.9 | 17712.9 | 39327.9 | 0 | PROCESSED | 55181.2533680556 | 55547 | 55181.2630324074 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | FESI1 | 313.4345 | 30.6099 | 74.31119672 | -9.05841998 | 226.3696 | 55182.5546180556 | 55183.3334837963 | 504017010 | 32287.6 | 24000 | 32287.6 | 32287.6 | 0 | 32287.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27212.9 | 27212.9 | 67285.9 | 0 | PROCESSED | 55204.2505092593 | 55575 | 55204.4679976852 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | FESI2 | 313.183 | 30.3797 | 73.99193661 | -9.03499466 | 225.2405 | 55174.9860300926 | 55175.7904398148 | 504018010 | 34590.4 | 34000 | 34590.4 | 34590.4 | 0 | 34590.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30318 | 30318 | 69493.9 | 0 | PROCESSED | 55189.1496180556 | 55555 | 55189.1622916667 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | | RXJ1713-3946_ID1 | 257.9616 | -39.5166 | 347.33828294 | -0.06271892 | 87.0007 | 55242.129375 | 55243.2502199074 | 504027010 | 61533.1 | 60000 | 61557.8 | 61533.1 | 0 | 61573.8 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 46725.9 | 46725.9 | 96823.8 | 0 | PROCESSED | 55253.4576967593 | 55622 | 55253.4734259259 | 2.4.12.27 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040021 | We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y | | RXJ1713-3946_ID2 | 258.3083 | -40.2394 | 346.91054647 | -0.70324775 | 87.0013 | 55243.7284722222 | 55244.1258564815 | 504028010 | 19009.3 | 20000 | 19009.3 | 19017.3 | 0 | 19017.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11826.3 | 11826.3 | 34331.9 | 0 | PROCESSED | 55256.0447337963 | 55622 | 55256.0518171296 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040021 | We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y | | RXJ1713-3946_ID3 | 258.1658 | -40.0306 | 347.01547145 | -0.49239611 | 87.0009 | 55244.1262847222 | 55244.4779398148 | 504029010 | 20871.6 | 20000 | 20903.6 | 20903.6 | 0 | 20871.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20886.8 | 20886.8 | 30375.9 | 0 | PROCESSED | 55256.0651388889 | 55622 | 55256.0720601852 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040021 | We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y | | RXJ1713-3946_ID4 | 258.9125 | -40.0131 | 347.36417887 | -0.94594655 | 86.0017 | 55244.4787384259 | 55244.8903587963 | 504030010 | 22153.4 | 20000 | 22177.4 | 22169.4 | 0 | 22153.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19719.3 | 19719.3 | 35557.9 | 1 | PROCESSED | 55256.0741319444 | 55622 | 55256.0824768518 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040021 | We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y | | HESS J1731-347 SW | 263.0074 | -34.9458 | 353.3803333 | -0.77058494 | 92.6086 | 55245.72 | 55246.5231365741 | 504031010 | 41861.5 | 40000 | 41877.9 | 41861.5 | 0 | 41869.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34102.8 | 34102.8 | 69382 | 0 | PROCESSED | 55257.0362037037 | 55623 | 55257.0493981482 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040026 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1731-347 is one of only 3 TeV SNRs which have a radio shell and possible thermal X-rays. With good statistics and low background observation of Suzaku XIS, we will detect thermal X-rays from the shell of HESS J1731-347 for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | B | BAMBA | AYA | NULL | NULL | JAP | 4 | AO4 | DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347 | XIS | Y | | HESS J1731-347 N | 262.8483 | -34.6425 | 353.56257635 | -0.49517094 | 91.6366 | 55244.8937037037 | 55245.7189699074 | 504032010 | 41526.3 | 40000 | 41526.3 | 41526.3 | 0 | 41526.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32865.3 | 32865.3 | 71271.9 | 0 | PROCESSED | 55256.998599537 | 55623 | 55257.0108449074 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040026 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1731-347 is one of only 3 TeV SNRs which have a radio shell and possible thermal X-rays. With good statistics and low background observation of Suzaku XIS, we will detect thermal X-rays from the shell of HESS J1731-347 for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | B | BAMBA | AYA | NULL | NULL | JAP | 4 | AO4 | DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347 | XIS | Y | | HESS J1427-608 | 216.9609 | -60.8505 | 314.40487303 | -0.14444396 | 90.5578 | 55209.5761458333 | 55212.1891666667 | 504034010 | 104137.9 | 100000 | 104137.9 | 104137.9 | 0 | 104137.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71261.1 | 71261.1 | 225737.8 | 1 | PROCESSED | 55225.4505439815 | 55594 | 55225.4958449074 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040066 | Pulsar wind nebula (PWN) has began to be recognized as the best candidate of a large fraction of the HESS-unidentified (unID) sources. It could be true for some sources like HESS J1825-137, while other PWN candidates are sometimes listed simply because they satisfy one or two of the necessary conditions (e.g., there is an energetic pulsar nearby). We then propose a Suzaku observation of HESS J1427-608, which is the most ``unlike'' HESS-unID source to be a PWN. The advantage that we can safely exclude a PWN for its candidate allows us to identify the emission mechanism/origin of HESS J1427-608 more unambiguously compared to other unID sources. We request a 150 ks exposure to constrain the ratio between X-ray and TeV fluxes, which is a good measure of the emission mechanism of TeV sources. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 4 | AO4 | A SUZAKU OBSERVATION OF HESS J1427-608 | XIS | Y | | W49B | 287.7847 | 9.1153 | 43.2812159 | -0.18378496 | 89.2674 | 54921.5302662037 | 54923.0613425926 | 504035010 | 61782.5 | 100000 | 61790.5 | 61784.5 | 0 | 61782.5 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 55155.6 | 55155.6 | 132273.9 | 3 | PROCESSED | 54949.0816203704 | 55324 | 54949.4493287037 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040075 | Observation of the W49B supernova remnant for 100 ksec is proposed to detect Ti emission line at the 3 sigma confidence level. In order to reveal whether it is a remnant of Type Ia supernova or not, detailed measurement of the rare metal elements such as Cr, Mn, Ni, and Ti is essential. We determine the type by Ti to Cr, Mn to Cr, and Ni to Fe ratios. Furthermore, we investigate whether its plasma is in the overionized status or not. | GALACTIC DIFFUSE EMISSION | 5 | B | OZAWA | MIDORI | NULL | NULL | JAP | 4 | AO4 | UNMASK THE NATURE OF W49B ! | XIS | Y | | TORNADO | 265.1272 | -30.949 | 357.70572925 | -0.11631727 | 269.1137 | 55072.5037037037 | 55075.0093055556 | 504036010 | 125069.2 | 120000 | 125069.2 | 125077.2 | 0 | 125077.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 97091.3 | 97091.3 | 216459.8 | 3 | PROCESSED | 55088.2749884259 | 55454 | 55088.3064814815 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040076 | The Tornado is an unusual and intense radio source located in the galactic center region. It has a polarized non-thermal radio spectrum. t has very unique morphology of elongated and loop-like structure. However, no crucial observational result determining the nature has been obtained. With the Suzaku AO3 observation of the Tornado (50ks), we found interesting signs of 2.45-keV He like S-K line, diffuse emission from the "tail" and the whole "head". The purpose of this observation is to obtain precise spectrum and spatial distribution. If the thermal S-K line is confirmed and it has a high metal abundance, the nature of the Tornado is an SNR. We also investigate the extreme structure of the tail and search for power-law component in spectra. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 4 | AO4 | REVEALING THE UNUSUAL SOURCE, THE NATURE OF THE "TORNADO", IN THE GALACTIC CENTER REGION | XIS | Y | | GALACTICDISC3-1 | 15.309 | 67.9759 | 123.85392042 | 5.12169353 | 244.2747 | 55214.8348148148 | 55216.0225 | 504038010 | 55227.9 | 50000 | 55227.9 | 55227.9 | 0 | 55227.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43332.9 | 43332.9 | 102599.8 | 2 | PROCESSED | 55228.1780324074 | 55594 | 55228.2005092593 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040097 | To elucidate the vertical structure of the yet-not-understood excess soft X-ray emission from the galactic disk, we propose to observe two offset directions from the plane along l = 123 degree. We expect the spectra contains the 0.75 keV emission component which we discovered in the energy spectra of two midplane observations. The proposed observations will strongly constrain the nature of the sources which are responsible for the excess emission, in particular the vertical distribution in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | C | KIMURA | SHUNSUKE | NULL | NULL | JAP | 4 | AO4 | STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE | XIS | Y | | GALACTICDISC3-2 | 16.1096 | 72.7817 | 123.90816526 | 9.93459858 | 241.5401 | 55216.0250115741 | 55217.5772685185 | 504039010 | 73528.2 | 70000 | 73528.2 | 73528.2 | 0 | 73528.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54648 | 54648 | 134105.8 | 1 | PROCESSED | 55236.0900694444 | 55602 | 55236.1178240741 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040097 | To elucidate the vertical structure of the yet-not-understood excess soft X-ray emission from the galactic disk, we propose to observe two offset directions from the plane along l = 123 degree. We expect the spectra contains the 0.75 keV emission component which we discovered in the energy spectra of two midplane observations. The proposed observations will strongly constrain the nature of the sources which are responsible for the excess emission, in particular the vertical distribution in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | C | KIMURA | SHUNSUKE | NULL | NULL | JAP | 4 | AO4 | STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE | XIS | Y | | ASO0382 | 265.491 | -20.8915 | 6.43327069 | 4.9108593 | 101.5727 | 55276.7369328704 | 55277.3869675926 | 504040010 | 21222.3 | 20000 | 21222.3 | 21222.3 | 0 | 21222.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 3974 | 3974 | 56108.9 | 2 | PROCESSED | 55298.6755902778 | 55665 | 55299.411875 | 2.5.16.28 | 2 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | ASO0078 | 59.472 | 32.09 | 162.76236061 | -16.0043339 | 83.0007 | 55045.8202777778 | 55046.3273032407 | 504041010 | 21312 | 20000 | 21320 | 21320 | 0 | 21312 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21295.9 | 21295.9 | 43799.9 | 0 | PROCESSED | 55064.031099537 | 55430 | 55064.0383912037 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | ASO0402 | 273.3436 | -12.7608 | 17.24676471 | 2.45193699 | 68.9842 | 55277.3929513889 | 55277.9793287037 | 504042010 | 25712.5 | 20000 | 25712.5 | 25712.5 | 0 | 25712.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16015.2 | 16015.2 | 50655.9 | 1 | PROCESSED | 55417.0765740741 | 55784 | 55417.0893865741 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | ASO0431 | 286.9632 | 6.0295 | 40.16756672 | -0.88470452 | 90.0004 | 54936.153287037 | 54936.8141666667 | 504043010 | 24522.2 | 20000 | 24522.2 | 24522.2 | 0 | 24522.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18105 | 18105 | 57073.9 | 0 | PROCESSED | 54949.3871296296 | 55324 | 54949.5652777778 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | ASO0449 | 299.6429 | 28.7759 | 65.87759933 | -0.32938525 | 56.1427 | 54974.6386921296 | 54975.5786342593 | 504044010 | 38733.7 | 20000 | 38733.7 | 38741.7 | 0 | 38741.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35220 | 35220 | 81199.9 | 2 | PROCESSED | 54987.0954861111 | 55356 | 54987.4424652778 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | ASO0218 | 157.1332 | -58.313 | 285.06973918 | -0.48663651 | 315.2825 | 55020.3423148148 | 55020.9467476852 | 504045010 | 22844.9 | 20000 | 22844.9 | 22844.9 | 0 | 22844.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21154.4 | 21154.4 | 52217.9 | 1 | PROCESSED | 55034.2615740741 | 55400 | 55034.2716898148 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | ASO0447 | 298.557 | 28.6365 | 65.2636943 | 0.41202338 | 90.516 | 54928.7514699074 | 54929.253587963 | 504046010 | 20545.7 | 20000 | 20545.7 | 20545.7 | 0 | 20545.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16907.1 | 16907.1 | 43377.9 | 1 | PROCESSED | 54949.0673032407 | 55324 | 54949.4485300926 | 2.3.12.25 | 2 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | ASO0147 | 98.4346 | 6.5402 | 205.09585789 | -0.932863 | 292.0552 | 54931.9181481482 | 54932.5036921296 | 504047010 | 24041.3 | 20000 | 24041.3 | 24041.3 | 0 | 24041.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23240.9 | 23240.9 | 50562 | 1 | PROCESSED | 54949.2968402778 | 55324 | 54949.5271180556 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | ASO0505 | 339.5988 | 59.0734 | 106.55945745 | 0.49758229 | 62.7751 | 55001.185775463 | 55001.7494675926 | 504048010 | 26361.6 | 20000 | 26369.6 | 26361.6 | 0 | 26377.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23841.6 | 23841.6 | 48695.9 | 1 | PROCESSED | 55015.2421296296 | 55381 | 55015.2523148148 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | ASO0376 | 263.1417 | -31.5448 | 356.29011362 | 0.99386623 | 267.5095 | 55082.1506365741 | 55083.1084606482 | 504049010 | 37227.8 | 20000 | 38987.8 | 39259.8 | 0 | 37227.8 | 5 | 4 | 0 | 4 | 1 | 0 | 0 | 31813.4 | 31813.4 | 82729.9 | 1 | PROCESSED | 55113.2099537037 | 55479 | 55113.2260069444 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | | (L,B)=(0.107,-1.425) | 267.8602 | -29.5833 | 0.10035042 | -1.42140103 | 68.0986 | 55261.1636226852 | 55263.893275463 | 504050010 | 100399.1 | 100000 | 100431.1 | 100399.1 | 0 | 100423.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80536 | 80536 | 235821.8 | 1 | PROCESSED | 55278.4197453704 | 55645 | 55278.4832523148 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040109 | In order to resolve origin of the Galactic bulge/ridge emission, we propose to observe the blank field 1.5 deg from the Galactic center where Chandra recently performed the deepest exposure (900 ksec) aiming to resolve the Galactic "diffuse" emission into point sources. Goals of the present observation are the following: (1) Resolve the three iron emission lines (6.41 keV, 6.67 keV and 6.97 keV) with Suzaku, and compare with the point source population determined by Chandra to clarify what kinds of sources are responsible for which emission line. (2) Study Galactic latitudinal variation of the three emission lines comparing with the existent Suzaku observation at (l,b)=(0.0, -2.0). (3) Constrain the hard-tail emission above 10 keV, and study its Galactic latitudinal variation. | GALACTIC DIFFUSE EMISSION | 5 | B | EBISAWA | KEN | NULL | NULL | JAP | 4 | AO4 | RESOLVING ORIGIN OF THE IRON EMISSION LINES FROM THE GALACTIC BULGE | XIS | Y | | ASO0418 | 279.775 | -5.7085 | 26.44714681 | 0.13153934 | 86.843 | 54934.6472800926 | 54935.7578587963 | 504052010 | 41068.4 | 40000 | 41080.2 | 41084.4 | 0 | 41068.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33525.8 | 33525.8 | 95937.8 | 0 | PROCESSED | 54949.4674884259 | 55324 | 54949.5662268518 | 2.3.12.25 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040112 | We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y | | ASO0215 | 154.6836 | -58.9426 | 284.32918046 | -1.70077172 | 314.5017 | 55019.3141782407 | 55020.3404976852 | 504053010 | 40086.8 | 40000 | 40086.8 | 40086.8 | 0 | 40086.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35478.2 | 35478.2 | 88659.8 | 0 | PROCESSED | 55029.2327199074 | 55399 | 55029.2468055556 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040112 | We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y | | ASO0304 | 213.3355 | -62.0808 | 312.3597658 | -0.71761471 | 280.2937 | 55036.9044907407 | 55038.1453935185 | 504054010 | 44248.5 | 40000 | 44248.5 | 44248.5 | 0 | 44248.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41083.9 | 41083.9 | 107201.8 | 1 | PROCESSED | 55048.3005208333 | 55415 | 55048.3203819444 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040112 | We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y | | ASO0319 | 224.8822 | -60.8823 | 317.89227503 | -1.78687667 | 277.7774 | 55049.7078125 | 55051.0238425926 | 504055010 | 42361.3 | 40000 | 42361.3 | 42366.8 | 0 | 42377.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37523.3 | 37523.3 | 113685.9 | 0 | PROCESSED | 55062.2726967593 | 55430 | 55062.2941782407 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040112 | We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y | | HESSJ1616_PSRJ1617 | 244.3756 | -50.9175 | 332.50297445 | -0.27465368 | 270.0711 | 55059.1110763889 | 55060.8328009259 | 504056010 | 65833.1 | 50000 | 65889.1 | 65833.1 | 0 | 65897.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41750.4 | 41750.4 | 148725.8 | 0 | PROCESSED | 55071.2290625 | 55437 | 55071.2513425926 | 2.4.12.26 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040115 | HESSJ1616-508 is one of the most energetic unidentified TeV object. Previously, we showed that there is no clear X-ray counterpart to this object with a Suzaku observation, and hence we argued that the object is a real dark particle accelerator. However, there is a young energetic pulsar PSRJ1617-5055 10 arcmin away from HESSJ1616, and another possibility has been proposed that HESSJ1616 is an offset pulsar wind nebula (PWN) driven by the pulsar. If this possibility is correct, a powerful X-ray PWN should be observed as HESSJ1825-137, but such PWN has not been reported. The lack of the detection may be due to small sensitivity of Chandra and XMM-Newton for a diffuse hard X-ray emission. We propose to observe PSRJ1617 to see if there is an extended PWN around this pulsar. | GALACTIC DIFFUSE EMISSION | 5 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | IS THE MOST ENERGETIC UNIDENTIFIED TEV OBJECT HESSJ1616-508 A PULSAR WIND NEBULA? | XIS | Y | | VICINITY OF NGC 4051 | 180.4686 | 44.1146 | 150.13143213 | 70.30340869 | 109.3717 | 55184.3459606482 | 55186.5140509259 | 504062010 | 89630.5 | 80000 | 89638.5 | 89646.5 | 0 | 89630.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 37075.8 | 37075.8 | 187281.9 | 2 | PROCESSED | 55209.2126273148 | 55581 | 55209.4570833333 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040120 | The highly ionized absorption lines of OVII and OVII at z = 0 have been unambiguously detected toward the bright AGN NGC 4051 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII and OVIII emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas. | GALACTIC DIFFUSE EMISSION | 5 | C | HAGIHARA | TOSHISHIGE | NULL | NULL | JAP | 4 | AO4 | STUDY OF WARM-HOT GAS TOWARD NGC 4051 | XIS | Y | | VELA SOUTHWEST 1 | 126.2671 | -48.2152 | 264.99036518 | -5.99332729 | 119.5649 | 55164.9700925926 | 55165.818900463 | 504063010 | 32733.1 | 30000 | 32749.2 | 32733.1 | 0 | 32741.1 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 23767.4 | 23767.4 | 73309.9 | 0 | PROCESSED | 55179.2546990741 | 55546 | 55179.268587963 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 040121 | We propose 2 pointing-observations of south western part of Vela supernova remnant. Vela SNR has the largest angular size of 8 degree in diameter, so it is suitable to carry out spatial resolved spectroscopy with Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | C | HIRAGA | JUNKO | NULL | NULL | JAP | 4 | AO4 | X-RAY STUDY ON THE NEAREST SUPERNOVA REMNANT, VELA | XIS | Y | | W51NW | 290.6858 | 14.2133 | 49.11550833 | -0.31636783 | 105.4558 | 55283.4893634259 | 55284.555 | 504066010 | 44112.5 | 40000 | 44120.5 | 44120.5 | 0 | 44112.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8896.1 | 8896.1 | 92063.9 | 0 | PROCESSED | 55302.488912037 | 55671 | 55302.5003240741 | 2.5.16.28 | 2 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 040129 | We propose to observe the supernova remnant (SNR) W51C with Suzaku XIS. The thermal energy of plasma in W51C, ~3x10^51ergs, is much larger than typical kinetic energy of supernova and can give a large amount of energy to cosmic-ray acceleration. The SNR interactes with the giant molecler cloud and is expected to emit gamma-rays from cosmic-ray interaction. We search for non-thermal X-ray diffuse emission from electron bremsstrahlung or synchrotron emission of secondary electrons produced by decaying charged pions created by p-p interaction. | GALACTIC DIFFUSE EMISSION | 5 | C | KATAGIRI | HIDEAKI | NULL | NULL | JAP | 4 | AO4 | ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C | XIS | Y | | W51SW | 290.8908 | 14.1062 | 49.1149541 | -0.54215584 | 104.3698 | 55285.3081944444 | 55286.3752314815 | 504067010 | 43728.7 | 40000 | 43728.7 | 43728.7 | 0 | 43728.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9813.7 | 9813.7 | 92179.9 | 0 | PROCESSED | 55302.2257175926 | 55671 | 55302.2468055556 | 2.5.16.28 | 1 | Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 | 040129 | We propose to observe the supernova remnant (SNR) W51C with Suzaku XIS. The thermal energy of plasma in W51C, ~3x10^51ergs, is much larger than typical kinetic energy of supernova and can give a large amount of energy to cosmic-ray acceleration. The SNR interactes with the giant molecler cloud and is expected to emit gamma-rays from cosmic-ray interaction. We search for non-thermal X-ray diffuse emission from electron bremsstrahlung or synchrotron emission of secondary electrons produced by decaying charged pions created by p-p interaction. | GALACTIC DIFFUSE EMISSION | 5 | C | KATAGIRI | HIDEAKI | NULL | NULL | JAP | 4 | AO4 | ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C | XIS | Y | | SEP #1 | 89.966 | -66.5774 | 276.40322057 | -29.82494721 | 141.7136 | 55149.1175925926 | 55150.2141087963 | 504069010 | 51862.1 | 50000 | 51870.1 | 51862.1 | 0 | 51870.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48353.4 | 48353.4 | 94725.9 | 2 | PROCESSED | 55160.1364236111 | 54922 | 55160.1496296296 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | | NEP #1 | 270.0492 | 66.5597 | 96.38280784 | 29.79186901 | 217.1802 | 55150.229212963 | 55151.1953587963 | 504070010 | 56336.7 | 50000 | 56336.7 | 56344.7 | 0 | 56344.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 41434.5 | 41434.5 | 83471.9 | 2 | PROCESSED | 55162.1951851852 | 54922 | 55162.2062268518 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | | SEP #2 | 89.966 | -66.5714 | 276.39630454 | -29.82495373 | 163.7813 | 55170.9454166667 | 55172.4863194444 | 504071010 | 57999.1 | 50000 | 58007.1 | 57999.1 | 0 | 58007.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35415.2 | 35415.2 | 133112 | 1 | PROCESSED | 55187.4636226852 | 54922 | 55187.4854398148 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | | NEP #2 | 270.0521 | 66.5655 | 96.38949161 | 29.79071779 | 194.6438 | 55172.5015162037 | 55173.6411342593 | 504072010 | 48697.7 | 50000 | 48697.7 | 48697.7 | 0 | 48697.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38458.2 | 38458.2 | 98456 | 1 | PROCESSED | 55190.0016203704 | 54922 | 55190.01875 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | | SEP #3 | 89.9578 | -66.5683 | 276.39273536 | -29.82821774 | 172.4885 | 55179.5059259259 | 55180.9169444444 | 504073010 | 44408 | 50000 | 44408 | 44416 | 0 | 44416 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23878.4 | 23878.4 | 121901.8 | 1 | PROCESSED | 55200.2330555556 | 54922 | 55200.462337963 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | | NEP #3 | 270.0483 | 66.5696 | 96.39421541 | 29.79223028 | 188.0738 | 55180.9320949074 | 55182.0557638889 | 504074010 | 50176.9 | 50000 | 50176.9 | 50176.9 | 0 | 50176.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33337.4 | 33337.4 | 97049.9 | 1 | PROCESSED | 55200.3194212963 | 54922 | 55200.4707291667 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | | SEP #4 | 89.9798 | -66.5683 | 276.39272547 | -29.81946932 | 185.1981 | 55192.0059490741 | 55193.3995833333 | 504075010 | 49956.6 | 50000 | 49956.6 | 49956.6 | 0 | 49956.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45143 | 45143 | 120393.9 | 1 | PROCESSED | 55225.2945717593 | 54922 | 55225.3094907407 | 2.4.12.27 | 1 | Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant co