DARTS/Astro Query System - SQL Search -

All the tables available for SQL Search and information on each table are listed in the Available Data page. Please see the User Guide for the usage of "SQL Search".

Call example

【Basic Syntax】

 SELECT {*|column, column, column,..}
 FROM table name
 [ WHERE conditions ]
 [ ORDER BY column, column,... ]
 [ LIMIT {ALL|number} ] [ OFFSET number ]
 ;

---------------------------------------------------------

This is an example query to obtain the first 10 rows of 
akari_fis_bsc_1 using radial search.

The akari_fis_bsc_1 is an catalogue, and each data has 
the coorinate position of the object. So, search the objects 
contained in the circle area you specify there.

Columns to display -> all
  Table name -> akari_fis_bsc_1
  Search condition -> radial search, 
   center position is (266.0, -28,0) and radius is 10 arcmin
  Displayed results -> from 1st to 10th

---------------------------------------------------------
Point:
  You can use functions of PgSphere(https://pgsphere.github.io/)
  on this system.

Data types:
    Point   ... spoint(coordinate, coordinate)
    Path    ... spath(spoint(), spoint(), ...)
    Circle  ... scircle(spoint(), radius)
    Polygon ... spoly(spoint(), spoint(), ...)

Operators:
    a @ b = '1' ... a contained by b
    a !@ b = '1' ... a is not contained by b
    a && b = '1' ... overlaped each other
    a !&& b = '1' ... do not overlaped each other

Ths function radians needs a parameter in degree.
  Operator '/' means division. 
  Note: integer division truncates the result.
   10.0 / 60.0 = 0.16666...
   10 / 60 = 0

---------------------------------------------------------

This is an example query to obtain the first 10 rows of 
ginga_observation_log using radial search.

The ginga_observation_log has pointing observations and 
scan observation. Each data has the coorinate of the 
observation start point and the end point, and the 
average point. So, search the pointing position contained 
in the circle area you specified, or the scan-path crossed 
over the area.

Columns to display -> all
  Table name -> ginga_observation_log
  Search condition -> radial search,
  center position is M31(10.7, 41.2) and radius is 1 degree
  Displayed results -> from 1st to 10th

---------------------------------------------------------
Point:
  You can use functions of PgSphere(https://pgsphere.github.io/)
  on this system.

Data types:
    Point   ... spoint(coordinate, coordinate)
    Path    ... spath(spoint(), spoint(), ...)
    Circle  ... scircle(spoint(), radius)
    Polygon ... spoly(spoint(), spoint(), ...)

Operators:
    a @ b  ... a contained by b
    a !@ b ... a is not contained by b
    a && b ... overlaped each other
    a !&& b ... do not overlaped each other

---------------------------------------------------------

This is an example query to obtain the data near the 
galactic center of suzaku_xis_observation_log using radial search.

The SUZAKU XIS has rectanglar field of view with 18 arcmin 
x 18 arcmin. Each data of suzaku_xis_observation_log has 
the coorinate of each corner position about field of view.
So, search the rectanglar area overlapd the circle area 
you specified.

Columns to display -> all
  Table name -> suzaku_xis_observation_log
  Search condition -> radial search,
    center position is (0.0, 0.0) with Galactic coordinates
    and radius is 1 arcmin
  Displayed results -> from 1st to 200th

---------------------------------------------------------
Point:

1. Use the column of Galactic coordinates.

2. You can use functions of PgSphere(https://pgsphere.github.io/)
   on this system.

Data types:
    Point   ... spoint(coordinate, coordinate)
    Path    ... spath(spoint(), spoint(), ...)
    Circle  ... scircle(spoint(), radius)
    Polygon ... spoly(spoint(), spoint(), ...)

Operators:
    a @ b  ... a contained by b
    a !@ b ... a is not contained by b
    a && b ... overlaped each other
    a !&& b ... do not overlaped each other

---------------------------------------------------------

This is an example query to obtain the data nearthe 
galactic center of suzaku_xis_observation_log using radial search.

The SUZAKU XIS has rectanglar field of view with 18 arcmin 
x 18 arcmin. Each data of suzaku_xis_observation_log has the 
coorinate of each corner position about field of view. 
So, search the rectanglar area overlapd the rectanglar area 
you specified.

Columns to display -> object_name, center_galactic_lon, 
   center_galactic_lat, data_access_url
  Table name -> suzaku_xis_observation_log
  Search condition -> rectanglar search,
    0.1(deg) <= Galactic Latitude <= .0.1(deg)
    and 0.1(deg) <= Galactic Latitude <= 0.1(deg)
  Displayed results -> from 1st to 100th

---------------------------------------------------------
Point:
  You can use functions of PgSphere(https://pgsphere.github.io/)
  on this system.

Data types:
    Point   ... spoint(coordinate, coordinate)
    Path    ... spath(spoint(), spoint(), ...)
    Circle  ... scircle(spoint(), radius)
    Polygon ... spoly(spoint(), spoint(), ...)

Operators:
    a @ b  ... a contained by b
    a !@ b ... a is not contained by b
    a && b ... overlaped each other
    a !&& b ... do not overlaped each other

---------------------------------------------------------

This is an example query to obtain the first 10 rows of 
akari_fis_bsc_1 using radial search.

The akari_fis_bsc_1 is an catalogue, and each data has 
the coorinate position of the object. So, search the objects 
contained in the circle area you specify there.

Columns to display -> all
  Table name -> akari_fis_bsc_1
  Search condition -> radial search, 
   center position is (266.0, -28,0) and radius is 10 arcmin
  Displayed results -> from 1st to 10th

---------------------------------------------------------
Point:
  You can use functions of PgSphere(https://pgsphere.github.io/)
  on this system.

Data types:
    Point   ... spoint(coordinate, coordinate)
    Path    ... spath(spoint(), spoint(), ...)
    Circle  ... scircle(spoint(), radius)
    Polygon ... spoly(spoint(), spoint(), ...)

Operators:
    a @ b = '1' ... a contained by b
    a !@ b = '1' ... a is not contained by b
    a && b = '1' ... overlaped each other
    a !&& b = '1' ... do not overlaped each other

Ths function radians needs a parameter in degree.
  Operator '/' means division. 
  Note: integer division truncates the result.
   10.0 / 60.0 = 0.16666...
   10 / 60 = 0

---------------------------------------------------------

This is an example query to obtain the first 10 rows of 
ginga_observation_log using radial search.

---------------------------------------------------------
Point:
  You can use functions of PgSphere(https://pgsphere.github.io/)
  on this system.

Data types:
    Point   ... spoint(coordinate, coordinate)
    Path    ... spath(spoint(), spoint(), ...)
    Circle  ... scircle(spoint(), radius)
    Polygon ... spoly(spoint(), spoint(), ...)

Operators:
    a @ b  ... a contained by b
    a !@ b ... a is not contained by b
    a && b ... overlaped each other
    a !&& b ... do not overlaped each other

---------------------------------------------------------

This is an example query to obtain the data near the 
galactic center of suzaku_xis_observation_log using radial search.

---------------------------------------------------------
Point:

1. Use the column of Galactic coordinates.

2. You can use functions of PgSphere(https://pgsphere.github.io/)
   on this system.

Data types:
    Point   ... spoint(coordinate, coordinate)
    Path    ... spath(spoint(), spoint(), ...)
    Circle  ... scircle(spoint(), radius)
    Polygon ... spoly(spoint(), spoint(), ...)

Operators:
    a @ b  ... a contained by b
    a !@ b ... a is not contained by b
    a && b ... overlaped each other
    a !&& b ... do not overlaped each other

---------------------------------------------------------

This is an example query to obtain the data nearthe 
galactic center of suzaku_xis_observation_log using radial search.

The SUZAKU XIS has rectanglar field of view with 18 arcmin 
x 18 arcmin. Each data of suzaku_xis_observation_log has the 
coorinate of each corner position about field of view. 
So, search the rectanglar area overlapd the rectanglar area 
you specified.

---------------------------------------------------------
Point:
  You can use functions of PgSphere(https://pgsphere.github.io/)
  on this system.

Data types:
    Point   ... spoint(coordinate, coordinate)
    Path    ... spath(spoint(), spoint(), ...)
    Circle  ... scircle(spoint(), radius)
    Polygon ... spoly(spoint(), spoint(), ...)

Operators:
    a @ b  ... a contained by b
    a !@ b ... a is not contained by b
    a && b ... overlaped each other
    a !&& b ... do not overlaped each other

---------------------------------------------------------

SQL query

Format

total 133

Download WgetScript

No.	object_name	center_ra	center_dec	proposal_type	proposal_priority	awarded_exposure	pi_name	proposal_title	proposal_abstract
1	JUPITER	0	0	PV	C	100.000	YUICHIRO EZOE	REVEALING TRANSPORTATION AND ACCELERATION OF PARTICLES IN JUPITER'S MAGNETOSPHERE	We propose observation of Jupiter to investigate long standing issues, i.e., the plasma transportation and the global acceleration of particles in Jupiter's magnetosphere. It is the most luminous planet in X-rays. The X-ray emission is composed of aurorae and disk. The former is due to charge exchange (CX) of several MeV/u ions and bremsstrahlung by keV electrons. The latter is due to scattering of solar X-rays. Suzaku found a sign of diffuse X-ray emission from inner radiation belts, possibly arising from inverse Compton scattering of solar photons by tens MeV electrons. With Resolve, we investigate CX emission lines to reveal the origin and kinematics of the ions and constrain the diffuse X-ray emission with Xtend.
2	C/2021 S3 PanSTARRS	0	0	PV	A	100.000	YUICHIRO EZOE	DIAGNOSTICS OF CHARGE EXCHANGE EMISSION FROM COMET C/2017 K2	We propose observation of comets to diagnose charge exchange (CX) models and databases and to investigate the chemical abundance of solar wind ions and cometary neutrals. The cometary X-rays are mainly produced by the CX process between highly charged ions in solar winds and neutral atoms or molecules in cometary coma. CX plays an important role in other astronomical objects such as solar system planets, supernova remnants, and clusters of galaxies. Among these objects, cometary X-ray emission represents the best laboratory for investigating the CX process itself. Only Resolve with high energy resolution for the diffuse X-ray emission can clearly measure the CX emission lines from high charge state ions. With Xtend, we will observe the spatial distribution of neutrals in the cometary coma.
3	TYCHO NW MAPPING 1	6.21667	64.17306	PV	A	75.000	BRIAN WILLIAMS	XRISM OBSERVATIONS OF TYCHO'S SUPERNOVA REMNANT	Tycho s SNR is one of the best studied Type Ia remnants in the sky, yet there remains much we do not know, such as ion temperatures of the ejecta species, abundances of rare elements like Cr and Mn (sensitive discriminators of the progenitor model), and the doppler velocities of elements beyond Si. We propose here for observations of both the center of the remnant and the SE Fe-rich knot for 75 ks each as a minimal observation goal. Ideally, we would map the remnant with a series of pointings, determining the spatial distribution of the ion temperature for various elements, and go even deeper on the Fe-rich knot in the SE to pull out any faint features.
4	TYCHO SW MAPPING 2	6.21667	64.12028	PV	C	20.000	BRIAN WILLIAMS	XRISM OBSERVATIONS OF TYCHO'S SUPERNOVA REMNANT	Tycho s SNR is one of the best studied Type Ia remnants in the sky, yet there remains much we do not know, such as ion temperatures of the ejecta species, abundances of rare elements like Cr and Mn (sensitive discriminators of the progenitor model), and the doppler velocities of elements beyond Si. We propose here for observations of both the center of the remnant and the SE Fe-rich knot for 75 ks each as a minimal observation goal. Ideally, we would map the remnant with a series of pointings, determining the spatial distribution of the ion temperature for various elements, and go even deeper on the Fe-rich knot in the SE to pull out any faint features.
5	TYCHO CENTER	6.33333	64.13861	PV	A	75.000	BRIAN WILLIAMS	XRISM OBSERVATIONS OF TYCHO'S SUPERNOVA REMNANT	Tycho s SNR is one of the best studied Type Ia remnants in the sky, yet there remains much we do not know, such as ion temperatures of the ejecta species, abundances of rare elements like Cr and Mn (sensitive discriminators of the progenitor model), and the doppler velocities of elements beyond Si. We propose here for observations of both the center of the remnant and the SE Fe-rich knot for 75 ks each as a minimal observation goal. Ideally, we would map the remnant with a series of pointings, determining the spatial distribution of the ion temperature for various elements, and go even deeper on the Fe-rich knot in the SE to pull out any faint features.
6	TYCHO N MAPPING 3	6.33333	64.19083	PV	C	20.000	BRIAN WILLIAMS	XRISM OBSERVATIONS OF TYCHO'S SUPERNOVA REMNANT	Tycho s SNR is one of the best studied Type Ia remnants in the sky, yet there remains much we do not know, such as ion temperatures of the ejecta species, abundances of rare elements like Cr and Mn (sensitive discriminators of the progenitor model), and the doppler velocities of elements beyond Si. We propose here for observations of both the center of the remnant and the SE Fe-rich knot for 75 ks each as a minimal observation goal. Ideally, we would map the remnant with a series of pointings, determining the spatial distribution of the ion temperature for various elements, and go even deeper on the Fe-rich knot in the SE to pull out any faint features.
7	TYCHO S MAPPING 4	6.33333	64.0875	PV	C	20.000	BRIAN WILLIAMS	XRISM OBSERVATIONS OF TYCHO'S SUPERNOVA REMNANT	Tycho s SNR is one of the best studied Type Ia remnants in the sky, yet there remains much we do not know, such as ion temperatures of the ejecta species, abundances of rare elements like Cr and Mn (sensitive discriminators of the progenitor model), and the doppler velocities of elements beyond Si. We propose here for observations of both the center of the remnant and the SE Fe-rich knot for 75 ks each as a minimal observation goal. Ideally, we would map the remnant with a series of pointings, determining the spatial distribution of the ion temperature for various elements, and go even deeper on the Fe-rich knot in the SE to pull out any faint features.
8	TYCHO NE MAPPING 5	6.45	64.165	PV	C	20.000	BRIAN WILLIAMS	XRISM OBSERVATIONS OF TYCHO'S SUPERNOVA REMNANT	Tycho s SNR is one of the best studied Type Ia remnants in the sky, yet there remains much we do not know, such as ion temperatures of the ejecta species, abundances of rare elements like Cr and Mn (sensitive discriminators of the progenitor model), and the doppler velocities of elements beyond Si. We propose here for observations of both the center of the remnant and the SE Fe-rich knot for 75 ks each as a minimal observation goal. Ideally, we would map the remnant with a series of pointings, determining the spatial distribution of the ion temperature for various elements, and go even deeper on the Fe-rich knot in the SE to pull out any faint features.
9	TYCHO SE KNOT	6.45417	64.11639	PV	C	20.000	BRIAN WILLIAMS	XRISM OBSERVATIONS OF TYCHO'S SUPERNOVA REMNANT	Tycho s SNR is one of the best studied Type Ia remnants in the sky, yet there remains much we do not know, such as ion temperatures of the ejecta species, abundances of rare elements like Cr and Mn (sensitive discriminators of the progenitor model), and the doppler velocities of elements beyond Si. We propose here for observations of both the center of the remnant and the SE Fe-rich knot for 75 ks each as a minimal observation goal. Ideally, we would map the remnant with a series of pointings, determining the spatial distribution of the ion temperature for various elements, and go even deeper on the Fe-rich knot in the SE to pull out any faint features.
10	E0102	16.005	-72.0312	Regular	A	30.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
11	E0102	16.005	-72.0312	Regular	A	30.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
12	1ES0229+201	38.2026	20.2882	Regular	A	75.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
13	PERSEUS CLUSTER	49.767	41.576	PV	A	100.000	IRINA ZHURAVLEVA	XRISM OBSERVATIONS OF THE PERSEUS CLUSTER	We propose a large observational program of the Perseus Cluster - the X-ray brightest nearby galaxy cluster. The program is designed to address several key science questions, including the physics of AGN feedback, gas motions that are driven by AGN feedback and mergers with infalling subclusters, the role of turbulence in particle acceleration, metallicity of the hot gas and search for rare elements, search for charge exchange and 3.5 keV line. The cluster is uniquely suitable to address these questions with reasonable exposure time and with an unparalleled degree of systematic robustness.
14	PERSEUS CLUSTER	49.829	41.554	PV	A	80.000	IRINA ZHURAVLEVA	XRISM OBSERVATIONS OF THE PERSEUS CLUSTER	We propose a large observational program of the Perseus Cluster - the X-ray brightest nearby galaxy cluster. The program is designed to address several key science questions, including the physics of AGN feedback, gas motions that are driven by AGN feedback and mergers with infalling subclusters, the role of turbulence in particle acceleration, metallicity of the hot gas and search for rare elements, search for charge exchange and 3.5 keV line. The cluster is uniquely suitable to address these questions with reasonable exposure time and with an unparalleled degree of systematic robustness.
15	PERSEUS CLUSTER	49.889	41.534	PV	A	50.000	IRINA ZHURAVLEVA	XRISM OBSERVATIONS OF THE PERSEUS CLUSTER	We propose a large observational program of the Perseus Cluster - the X-ray brightest nearby galaxy cluster. The program is designed to address several key science questions, including the physics of AGN feedback, gas motions that are driven by AGN feedback and mergers with infalling subclusters, the role of turbulence in particle acceleration, metallicity of the hot gas and search for rare elements, search for charge exchange and 3.5 keV line. The cluster is uniquely suitable to address these questions with reasonable exposure time and with an unparalleled degree of systematic robustness.
16	PERSEUS CLUSTER	49.921	41.467	PV	A	50.000	IRINA ZHURAVLEVA	XRISM OBSERVATIONS OF THE PERSEUS CLUSTER	We propose a large observational program of the Perseus Cluster - the X-ray brightest nearby galaxy cluster. The program is designed to address several key science questions, including the physics of AGN feedback, gas motions that are driven by AGN feedback and mergers with infalling subclusters, the role of turbulence in particle acceleration, metallicity of the hot gas and search for rare elements, search for charge exchange and 3.5 keV line. The cluster is uniquely suitable to address these questions with reasonable exposure time and with an unparalleled degree of systematic robustness.
17	Perseus Cluster	49.9467	41.5131	Regular	A	40.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
18	Perseus Cluster	49.9467	41.5131	Regular	A	40.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
19	PERSEUS CLUSTER	49.949	41.513	PV	C	200.000	IRINA ZHURAVLEVA	XRISM OBSERVATIONS OF THE PERSEUS CLUSTER	We propose a large observational program of the Perseus Cluster - the X-ray brightest nearby galaxy cluster. The program is designed to address several key science questions, including the physics of AGN feedback, gas motions that are driven by AGN feedback and mergers with infalling subclusters, the role of turbulence in particle acceleration, metallicity of the hot gas and search for rare elements, search for charge exchange and 3.5 keV line. The cluster is uniquely suitable to address these questions with reasonable exposure time and with an unparalleled degree of systematic robustness.
20	NGC 1365	53.40154	-36.14039	PV	A	250.000	ERIN KARA	STUDYING PHOTOIONISED OUTFLOWS IN A LUMINOUS STAR-FORMING AGN	NGC 1365 is a Seyfert 1.8 galaxy with a rich spectrum of narrow emission and absorption lines. It shows the most robust evidence for four Fe XXV/Fe XXVI K-alpha/K-beta absorption lines from a highly ionised outflow. It shows variable obscuration on timescales as short as days, and relativistically broadened iron line. As it is highly variable down to timescales of hours, it is an ideal target for timing analysis with the Xtend+Resolve instruments. It is also a beautiful example of a luminous AGN in a highly star-forming galaxy, providing an opportunity to probe the AGN-starburst connection. With Resolve, we will, for the first time, robustly measure P Cygni profiles from an ionised wind in an AGN to make an independent estimate of the radius, therefore constraining the launching mechanism.
21	HR 1099	54.197	0.5878	Regular	A	50.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
22	Abell 478	63.3363	10.4764	Regular	A	15.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
23	Abell 478	63.3363	10.4764	Regular	A	15.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
24	Abell 478	63.3363	10.4764	Regular	A	15.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
25	Abell 478	63.3363	10.4764	Regular	A	10.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
26	NGC 1550	64.908	2.4099	Regular	A	100.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
27	IRAS F05189-2524	80.25583	-25.36258	PV	C	100.000	HIROFUMI NODA	XRISM STUDIES OF ULTRA LUMINOUS IR GALAXY IRAS F05189-2524	IRAS F05189-2524 is an ultra-luminous IR galaxy which harbors an AGN and strong starburst activity together, and a late-stage merger showing the brightest Fe-K emission lines. In this source, we explore a binary supermassive black hole by resolving dual Fe-Kalpha lines at 6.4 keV. It is also the best target to study properties of starburst plasmas and their connection to the AGN activity by resolving Fe XXV and Fe XXVI lines from starburst activity. We furthermore aim to determine the detailed profile of an UFO absorption line at 7.8 keV, and constrain its connection to molecular outflows in the host galaxy.
28	N132D	81.26375	-69.64094	Regular	A	50.000	Makoto Tashiro	Early Release Science Targets	NOT_FILLED
29	AB Dor	82.187	-65.4487	Regular	A	50.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
30	AB Dor	82.187	-65.4487	Regular	A	50.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
31	Crab	83.6013	22.0439	Regular	A	5.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
32	Crab	83.6013	21.985	Regular	A	5.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
33	Crab stray light	83.6331	22.0145	Regular	A	45.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
34	Crab	83.6585	21.9909	Regular	A	5.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
35	Crab	83.6649	22.0439	Regular	A	9.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
36	Crab	83.678	22.0562	Regular	A	9.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
37	SN 1987A	83.86675	-69.26975	PV	A	100.000	YUKIKATSU TERADA	TIME EVOLUTION OF YOUNG NEI PLASMA IN SN 1987A	The nascent core-collapse supernova remnant SN1987A presents a unique opportunity to observe the rapid time evolution of a non-equilibrium ionization (NEI) collisional plasma at early evolutionary timescales. During the XRISM mission life, the NEI plasma emission from the ejecta is expected to become dominant as compared to the emission from the surrounding equatorial ring and HII regions. The minimal goal is to separate and characterize the ejecta emission by the high-resolution spectra. The ideal goal is to measure the time evolution with two observations to directly study the structure and chemical composition of the ejecta to limit progenitor types. Another bonus is to observationally verify the Rankine-Hugoniot relation from ion temperatures by species.
38	LMC X-1	84.9118	-69.7432	Regular	A	5.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
39	LMC X-1	84.9118	-69.7432	Regular	A	5.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
40	LMC X-1	84.9118	-69.7432	Regular	A	5.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
41	LMC X-1	84.9118	-69.7432	Regular	A	5.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
42	LMC X-1	84.9118	-69.7432	Regular	A	5.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
43	LMC X-1	84.9118	-69.7432	Regular	A	5.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
44	VELA X-1	135.52833	-40.55469	PV	C	70.000	TIMOTHY KALLMAN	PROBING THE WIND-COMPACT OBJECT INTERACTION IN VELA X-1	We propose to observe Vela X-1, the prototypical High Mass X-ray Binary in order to study the spectrum and its variability. The observation is designed to study the variability with the X-ray pulse and the variability with the binary orbit. This will allow constraints on the shape of the pulsar beam, which has previously been done only very crudely. It will allow us to determine the mean density of gas in the wind as it interacts with the pulsar, and to constrain iron peak abundances. We will search for pulsations in the lines, which will provide information about the pulsar beam as seen by many different lines of sight at once. Observations of Vela X-1 are virtually guaranteed to produce spectra which are of high statistical significance and rich in line features. They will provide
45	2S0921-630	140.64446	-63.29481	PV	C	80.000	CHRIS DONE	THE LAUNCH MECHANISM OF ACCRETION DISC WINDS: THE BEST TESTS FROM THE NEUTRON STAR BINARIES GX13+1 AND 2S0921-630	Accretion disc winds are clearly seen in black hole and neutron star binaries, but their origin is controversial. Are they magnetically driven, connecting them to the jet as well as to the accretion process itself, or are they thermal/radiative, driven by X-ray irradiation of the outer disc? GX13+1 persistently shows a massive wind in absorption, and is the most reliable LMXRB wind source to address the key question of the origin of the wind. A 30ks Resolve observation can directly measure the wind velocity profile along the line of sight, which will distinguish between magnetic and thermal-radiative acceleration. An additional 80ks observation of 2S0921 will instead shows the wind in emission, as its very high inclination angle means the X-ray source is obscured by the disc.
46	M81	148.88825	69.06536	PV	C	100.000	JON MILLER	A RADIATIVELY INEFFICIENT ACCRETION FLOW IN THE LINER M81*	Up to 40% of all galaxies may harbor low-ionization nuclear emission region (LINERs) and low-luminosity AGN (LLAGN). Well-developed theory suggests that the inner flow should be advective and radiatively inefficient, with a standard thin disk truncated far from the black hole. Resolve spectroscopy of M81* offers the best chance to finally reveal the geometry and dynamics of a radiatively inefficient accretion flow (RIAF) onto a black hole. M81* is the brightest LINER /LLAGN in X-rays. Prior Chandra/HETG spectra reveal low-ionization and He-like and H-like Fe K emission lines that are likely redshifted. A 100 ks exposure with Resolve can make unique tests of RIAF models.
47	M82	148.96967	69.67939	PV	A	50.000	IKUYUKI MITSUISHI	DIRECT VELOCITY MEASUREMENT OF X-RAY EMITTING HOT GAS IN STARBURST-DRIVEN OUTFLOWS IN M82 AND NGC 253 WITH XRISM/RESOLVE	Observational facts that metals in the intergalactic medium are found at low and high redshifts suggest that some part of all metals ever created now reside outside galaxies. Galactic-scale starburst-driven outflows are one of the best-studied and most common form of outflow capable of transporting substantial amount of materials inside galaxies into intergalactic space. To verify the scenario, we propose to observe the most prominent nearby galactic-scale starburst phenomena occurred around the nuclear regions of M82 and NGC253. Resolve observations would realize direct measurements of outflow velocity for X-ray emitting hot gas which is a link between galaxies and intergalactic space and the results would yield new insights in the both chemical and dynamical evolution of the Universe.
48	ABELL1060	159.1784	-27.5283	Regular	A	50.000	Makoto Tashiro	Early Release Science Targets	NOT_FILLED
49	CARINA NORTH	160.96071	-59.64275	PV	C	30.000	KENJI HAMAGUCHI	ORIGIN AND DYNAMICS OF DIFFUSE X-RAY EMISSION FROM THE CARINA NEBULA	The Carina nebula, one of the most massive star-forming regions in our neighborhood, is accompanied by bright diffuse X-ray emission, whose origin is not understood. Previous Suzaku and Chandra observations found substantial spatial variations in the Fe L, and Si and O K emission lines. If they reflect abundance variations, the diffuse plasma is probably a supernova remnant or merged multiple supernova remnants. However, the spectra also show multiple unidentified emission lines, which may suggest complicated plasma conditions. We propose XRISM observations of two regions in the Carina nebula to resolve emission lines in their spectra for the first time. We will also measure the Doppler motions of these emission lines.
50	ETA CARINAE	161.26479	-59.68444	PV	A	100.000	KENJI HAMAGUCHI	DYNAMICS OF THE COLLISIONAL SHOCKS DRIVEN BY THE MASSIVE BINARY ETA CARINAE	A massive mass-loss wind from the evolved supermassive star, eta Carinae, collides with a fast wind from its hidden companion and produces hot plasma at ~50 MK. The X-ray spectra show strong He-like iron K lines from the hot plasma and iron K fluorescence produced by absorption and reemission of the hard X-ray emission at the primary wind. These emission lines should hold crucial information on the shocked gas at the head-on collision, which would flow with a few hundred to thousand km s-1. The star is also surrounded by a ring-shaped diffuse soft X-ray nebula, whose emission lines may show Doppler broadening or shift if the nebula originates from a supernova imposter event in the 1840s. We aim to resolve these emission line features for the first time with XRISM/Resolve.
51	CEN X-3	170.31287	-60.62378	PV	A	90.000	MASAHIRO TSUJIMOTO	MAPPING WIND MASS LOSS IN A NEUTRON STAR HOSTING BINARY WITH X-RAYS	Binary evolution is a fundamental ingredient in astronomy. For NS-hosting HMXBs, which are of particular interests for the most plausible NS-NS merger progenitors, the standard binary evolution theory meets some serious challenges. One thing that is not considered well in the standard theory is the non-isotropy of the wind mass loss from the high-mass donor. Doppler tomography is an established method in the optical/UV band for the velocity mapping of a binary system, which can be applied in the X-ray band for the first time by using Resolve. Cen X-3 is the target of choice. The wind velocity field can be mapped using photo-ionized X-ray emission lines. Here, we propose a Resolve observation for one entire orbit (2.1 days) to construct a phase-resolved high-resolution X-ray spectra.
52	NGC 3783	174.75733	-37.73867	PV	A	200.000	JELLE KAASTRA	THROUGH DARKNESS AND LIGHT: THE MANY FACES OF THE OUTFLOWS IN NGC 3783	NGC 3783 is the flagship Seyfert 1 galaxy for AGN wind studies. Its outflow has been studied extensively for the lower ionization components, but the highest ionized gas has barely been detected despite >Ms exposures with Chandra. A deep 200 ks exposure with XRISM, lasting 4 days, will yield the full velocity-resolved absorption measure distribution, from the lowest to the highest ionization stages. Its variability constrains its distance. Finding ultra-fast outflows or obscuration events, both transient phenomena, is another exciting opportunity.
53	GT MUS	174.87329	-65.39778	PV	A	90.000	MASAHIRO TSUJIMOTO	NON-THERMAL SIGNATURES DURING STELLAR FLARES	A sudden release of energy in solar flares is, in practice, the only astronomical phenomenon that affects our daily lives in the timescale of a man. The largest class flares that affect can only be quantified by studying other stars like the Sun. Investigations of stellar flares in the X-rays provide unique information on the non-thermal aspects of flares, which made steady progress in the last decade. Spectroscopy with an X-ray micro-calorimeter will make a giant leap by providing a new toolbox that has not been realized even in the X-ray observations of the Sun. Here, we propose a MAXI-triggered ToO observation of GT Mus, or other star with a slow development, for the Doppler shifts and off-CIE plasma diagnostics to investigate the non-thermal aspects of stellar flares.
54	NGC 4151	182.63575	39.40572	PV	A	45.000	JON MILLER	SHAPING NEW AGN HORIZONS WITH NGC 4151	NGC 4151 is the brightest Seyfert-1 in the sky in the Fe~K band, with the strongest "narrow" Fe K line. This source can address more of the key science questions identified by the Extragalactic Compact Objects team than any other. Flagship observations of NGC 4151 will accomplish boundary-shifting science that will shape how the AGN community uses XRISM. First, flagship observations of NGC 4151 can clearly demonstrate and leverage reverberation mapping using the narrow Fe K emission line. This represents a new means of measuring black hole mass and the geometry of the inner and intermediate accretion flow. Second, in NGC 4151 the duty cycle of UFOs can be measured. It is the duty cycle that determines whether these flows can supply the feedback needed to shape host galaxies.
55	NGC 4151	182.63575	39.40572	PV	A	45.000	JON MILLER	SHAPING NEW AGN HORIZONS WITH NGC 4151	NGC 4151 is the brightest Seyfert-1 in the sky in the Fe~K band, with the strongest "narrow" Fe K line. This source can address more of the key science questions identified by the Extragalactic Compact Objects team than any other. Flagship observations of NGC 4151 will accomplish boundary-shifting science that will shape how the AGN community uses XRISM. First, flagship observations of NGC 4151 can clearly demonstrate and leverage reverberation mapping using the narrow Fe K emission line. This represents a new means of measuring black hole mass and the geometry of the inner and intermediate accretion flow. Second, in NGC 4151 the duty cycle of UFOs can be measured. It is the duty cycle that determines whether these flows can supply the feedback needed to shape host galaxies.
56	NGC 4151	182.63575	39.40572	PV	A	45.000	JON MILLER	SHAPING NEW AGN HORIZONS WITH NGC 4151	NGC 4151 is the brightest Seyfert-1 in the sky in the Fe~K band, with the strongest "narrow" Fe K line. This source can address more of the key science questions identified by the Extragalactic Compact Objects team than any other. Flagship observations of NGC 4151 will accomplish boundary-shifting science that will shape how the AGN community uses XRISM. First, flagship observations of NGC 4151 can clearly demonstrate and leverage reverberation mapping using the narrow Fe K emission line. This represents a new means of measuring black hole mass and the geometry of the inner and intermediate accretion flow. Second, in NGC 4151 the duty cycle of UFOs can be measured. It is the duty cycle that determines whether these flows can supply the feedback needed to shape host galaxies.
57	NGC 4151	182.63575	39.40572	PV	A	45.000	JON MILLER	SHAPING NEW AGN HORIZONS WITH NGC 4151	NGC 4151 is the brightest Seyfert-1 in the sky in the Fe~K band, with the strongest "narrow" Fe K line. This source can address more of the key science questions identified by the Extragalactic Compact Objects team than any other. Flagship observations of NGC 4151 will accomplish boundary-shifting science that will shape how the AGN community uses XRISM. First, flagship observations of NGC 4151 can clearly demonstrate and leverage reverberation mapping using the narrow Fe K emission line. This represents a new means of measuring black hole mass and the geometry of the inner and intermediate accretion flow. Second, in NGC 4151 the duty cycle of UFOs can be measured. It is the duty cycle that determines whether these flows can supply the feedback needed to shape host galaxies.
58	MRK766	184.61046	29.81292	PV	C	80.000	ELISA COSTANTINI	ABSORPTION AND EMISSION UNDER EXTREME CONDITIONS: THE CASE OF MRK766	We propose to observe the highly accreting AGN Mrk 766 in order to characterize its emission spectrum and its peculiar, variable, absorption features. In this source also an ultra-fast outflow was reported. Only XRISM is able to characterize the behaviour of spectral features in a highly accreting object as a function of time.
59	NGC 4388	186.44479	12.66208	PV	C	100.000	YOSHIHIRO UEDA	RESOLVING CIRCUMNUCLEAR STRUCTURE IN SEYFERT 2 GALAXY NGC 4388	High resolution spectroscopy with Resolve will enable us to perform unprecedented studies of the circumnuclear structure of AGN using the detailed velocity structure of the narrow Fe-Ka fluorescence line. Here we propose to observe NGC 4388, which exhibits the brightest narrow Fe-Ka emission line among Compton-thin Seyfert 2 Galaxies. The bright narrow Fe-Ka line, Compton-thin absorption, and high inclination make it the best target for studying the ``torus'' and inner region. With Resolve, we can for the first time measure the detailed line profile itself, leading to unbiased determination of matter distribution profile around the nucleus.
60	3C273	187.2779	2.0524	Regular	A	50.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
61	3C273	187.2779	2.0524	Regular	A	50.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
62	3C273	187.2779	2.0524	Regular	A	50.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
63	M87 SW_ARM	187.66096	12.35708	PV	A	150.000	AURORA SIMIONESCU	SUPERMASSIVE BLACK HOLE FEEDBACK IN M87	We propose a mosaic of XRISM/Resolve pointings designed to study supermassive black hole feedback in the nearest and second brightest cool core cluster in spatially resolved detail. The most striking features in M87 are the 6 arcmin-long, X-ray bright arms thought to be filaments of multi-phase, metal-rich gas uplifted by the buoyant AGN radio lobes. XRISM measurements will reveal the kinematics of this uplift and quantify the amount of metals being transported outwards by the AGN. The relatively low ambient temperature of M87 corresponds to a line-rich spectrum that will perfectly showcase the soft X-ray capabilities of Resolve.
64	M87 NW	187.67862	12.43481	PV	A	100.000	AURORA SIMIONESCU	SUPERMASSIVE BLACK HOLE FEEDBACK IN M87	We propose a mosaic of XRISM/Resolve pointings designed to study supermassive black hole feedback in the nearest and second brightest cool core cluster in spatially resolved detail. The most striking features in M87 are the 6 arcmin-long, X-ray bright arms thought to be filaments of multi-phase, metal-rich gas uplifted by the buoyant AGN radio lobes. XRISM measurements will reveal the kinematics of this uplift and quantify the amount of metals being transported outwards by the AGN. The relatively low ambient temperature of M87 corresponds to a line-rich spectrum that will perfectly showcase the soft X-ray capabilities of Resolve.
65	M87	187.70413	12.38961	PV	A	100.000	AURORA SIMIONESCU	SUPERMASSIVE BLACK HOLE FEEDBACK IN M87	We propose a mosaic of XRISM/Resolve pointings designed to study supermassive black hole feedback in the nearest and second brightest cool core cluster in spatially resolved detail. The most striking features in M87 are the 6 arcmin-long, X-ray bright arms thought to be filaments of multi-phase, metal-rich gas uplifted by the buoyant AGN radio lobes. XRISM measurements will reveal the kinematics of this uplift and quantify the amount of metals being transported outwards by the AGN. The relatively low ambient temperature of M87 corresponds to a line-rich spectrum that will perfectly showcase the soft X-ray capabilities of Resolve.
66	M87 E_ARM	187.75871	12.39075	PV	A	150.000	AURORA SIMIONESCU	SUPERMASSIVE BLACK HOLE FEEDBACK IN M87	We propose a mosaic of XRISM/Resolve pointings designed to study supermassive black hole feedback in the nearest and second brightest cool core cluster in spatially resolved detail. The most striking features in M87 are the 6 arcmin-long, X-ray bright arms thought to be filaments of multi-phase, metal-rich gas uplifted by the buoyant AGN radio lobes. XRISM measurements will reveal the kinematics of this uplift and quantify the amount of metals being transported outwards by the AGN. The relatively low ambient temperature of M87 corresponds to a line-rich spectrum that will perfectly showcase the soft X-ray capabilities of Resolve.
67	NGC4636	190.70762	2.68778	PV	A	100.000	KOSUKE SATO	AGN FEEDBACK IN BRIGHT ELLIPTICAL GALAXY NGC4636	We propose a 100 ks observation of the NGC4636 galaxy with XRISM/Resolve. The XRISM field of view will cover the brightest r ∼ 7.5 kpc region of the galaxy allowing high-resolution spectral studies of the region dominated by the AGN feedback physics. This observation plays key roles for revealing the role of gas motions in the cooling-heating balance in massive galaxies , understanding the origin of the chemical elements in massive galaxies and probing the star formation history, and calibrating the atomic data below 1.5 keV.
68	CENTAURUS CLUSTER	192.19958	-41.30778	PV	A	150.000	KOSUKE SATO	XRISM OBSERVATIONS OF THE CENTAURUS CLUSTER	Chemical enrichment and production of heavy elements is one of the key science questions related to the physics of galaxy clusters that XRISM will address. The hot intracluster medium in the Centaurus cluster has the highest metallicity among the X-ray brightest clusters in the sky. Its central iron abundance is about 1.5 times the solar value, which suggests an effective enrichment by Type Ia supernovae. Thus the Centaurus cluster is an ideal target to study detailed chemical enrichment through XRISM observations.
69	COMA CENTER	194.94292	27.94583	PV	A	200.000	MAXIM MARKEVITCH	FIRST DIRECT MEASUREMENT OF THE POWER SPECTRUM OF INTERGALACTIC TURBULENCE	We propose the first direct measurement of the power spectrum of turbulence in the intracluster medium. The spectrum determines the flow of kinetic energy down the turbulent cascade and the amount that dissipates into heat and feeds cosmic ray acceleration and magnetic field amplification. The nearby Coma cluster is the best system for such a measurement, as it does not have a cool core or a powerful AGN, thus all gas motions should be merger-generated and the turbulence should develop in an isotropic, textbook fashion. Our full mosaic of 5 pointings will yield a measurement of the power spectrum normalization and injection scale, a combination that determines the energy flow. Our minimum case is the first detection of turbulence in a merging cluster using the central pointing.
70	COMA OFFSET S	194.94292	27.84583	PV	C	100.000	MAXIM MARKEVITCH	FIRST DIRECT MEASUREMENT OF THE POWER SPECTRUM OF INTERGALACTIC TURBULENCE	We propose the first direct measurement of the power spectrum of turbulence in the intracluster medium. The spectrum determines the flow of kinetic energy down the turbulent cascade and the amount that dissipates into heat and feeds cosmic ray acceleration and magnetic field amplification. The nearby Coma cluster is the best system for such a measurement, as it does not have a cool core or a powerful AGN, thus all gas motions should be merger-generated and the turbulence should develop in an isotropic, textbook fashion. Our full mosaic of 5 pointings will yield a measurement of the power spectrum normalization and injection scale, a combination that determines the energy flow. Our minimum case is the first detection of turbulence in a merging cluster using the central pointing.
71	NGC 5044 CORE	198.84987	-16.38556	PV	C	100.000	MICHAEL LOEWENSTEIN	ASTROPHYSICS OF THE HOT PLASMA IN NGC 5044	The interplay of AGN feedback, cooling, and mixing of gas in different phases in elliptical galaxies are reflected in the thermal and velocity structure of the hot interstellar media. A 100 ks XRISM Resolve exposure of the center of NGC 5044 will measure turbulence to 30 km/sec, constrain the thermal and chemical structure in the disturbed central ISM, and search for signatures of charge exchange in the multi-phase medium. An additional 150 ks offset observation constrains the kinematical, thermal and chemical properties in the evidently undisturbed outer region to compare with the central region.
72	CENTAURUS A	201.36508	-43.01911	PV	A	100.000	JON MILLER	THE JET-LAUNCHING DISK AND ACCRETION FLOW IN CENTAURUS A	A full understanding of the AGN that drive the most powerful jets - those that reshape clusters and galaxies - requires that we study the accretion disk in such systems. However, in most cases, the accretion inflow is obscured, hidden, or otherwise inaccessible. Cen A is a nearby radio galaxy (d
73	MCG-6-30-15	202.33933	37.41403	PV	A	100.000	LAURA BRENNEMAN	A DETAILED EXPLORATION OF REFLECTION AND ABSORPTION IN MCG 6-30-15 WITH XRISM	The bright, narrow-line Seyfert 1 galaxy MCG 6-30-15 harbors one of the most studied AGN in high-energy astrophysics, boasting one of the most prominent, broadest Fe Kα lines ever seen, as well as the first warm absorber in which time variability was detected. The launch of XRISM will offer a revolutionary new perspective on this fascinating source, giving us the ability to characterize its spectral signatures in unprecedented detail. These features include narrow emission lines from distant reflection, a broadened and skewed Fe Kα line from inner disk reflection, and outflowing winds in absorption that span orders of magnitude in their physical and kinematic properties. Herein, we propose two observing scenarios for MCG6 during the PV phase of the XRISM mission.
74	M51	202.49125	47.21008	PV	C	70.000	EDMUND HODGES-KLUCK	THE NATURE OF THE HOT ISM IN THE GRAND DESIGN SPIRAL M51	The hot ISM is a byproduct and an agent of stellar feedback that regulates star formation, disperses metals, confines clouds, and is the major interface with the circumgalactic medium. However, the mass, energy, ionization history, and distribution of this galactic cytoplasm remain poorly constrained because it has primarily been studied at low spectral resolution (~100 eV) where the principal line complexes are unresolved. Here we propose a XRISM observation of the hot ISM in the nuclear and spiral arm regions of M51, from which we will derive the emission measure distribution as a function of temperature, map chemical abundances, and search for signs of non-equilibrium ionization and charge exchange. M51 is an X-ray bright, but otherwise typical, late-type galaxy and this observation wil
75	V834 CEN	212.28037	-45.28778	PV	A	100.000	YUKIKATSU TERADA	NEW PLASMA DIAGNOSTICS USING RESONANCE LINES ON MCV PLASMA	The scientific goal of this proposal is to demonstrate the NEW plasma diagnostics of ``optically-thin'' thermal plasma using the ``optically-thick'' resonance photons, since the later carries the information on the plasma shape. The minimal goal is to demonstrate the anisotropic radiative transfer of resonance photons of Fe-K line in the accretion column by the spin-phase-resolved high-resolution spectra with 50 ksec observation of V834 Cen. The ideal goals is to perform the independent measurement of the density using the resonance lines in 10% accuracy and to detect the multi-temperature structure of the accretion column and constrain the plasma shape using atomic lines of O, Mg, Si, S, and Fe with 100 ksec observation.
76	CIRCINUS GALAXY	213.29146	-65.33922	PV	A	100.000	YOSHIHIRO UEDA	UNVEILING NATURE OF COMPTON-THICK TORUS IN CIRCINUS GALAXY	We propose to observe the Circinus galaxy with XRISM, the most nearby (4.2 Mpc) Compton-thick AGN showing the brightest narrow Fe-Ka line among all known AGNs. The bright fluorescence lines and Compton-thick nature make it the best target for studying the torus itself through high resolution spectroscopy. We use the Compton shoulder structure of Fe-Ka and the properties of other fluorescence lines to unveil the torus structure. The Resolve spectrum will also reveal the origins and kinematics of the extended soft X-ray emission.
77	RCW86 NE	221.25146	-62.28744	PV	C	100.000	AYA BAMBA	MEASURING STOLEN ENERGY BY PARTICLE ACCELERATION FROM THE NORTHEASTERN SHOCK OF THE YOUNG SNR RCW 86	Shocks of supervnova remnants are primary candidates of Galactic cosmic ray origin. Efficient acceleration drains the energy from the shock and the downstream plasma cannot be heated up to the ideal gas Rankine-Hugoniot situation. We aim to measure ion temperature of shocks with the emission line width in NE and E shocks of the ideal target RCW86, to estimate the drained energy into particle acceleration and the efficiency changes with various environments. Our minimum requirements need 100+50 ks.
78	RCW86 E	221.35054	-62.41128	PV	C	50.000	AYA BAMBA	MEASURING STOLEN ENERGY BY PARTICLE ACCELERATION FROM THE NORTHEASTERN SHOCK OF THE YOUNG SNR RCW 86	Shocks of supervnova remnants are primary candidates of Galactic cosmic ray origin. Efficient acceleration drains the energy from the shock and the downstream plasma cannot be heated up to the ideal gas Rankine-Hugoniot situation. We aim to measure ion temperature of shocks with the emission line width in NE and E shocks of the ideal target RCW86, to estimate the drained energy into particle acceleration and the efficiency changes with various environments. Our minimum requirements need 100+50 ks.
79	SN1006_NW	225.545	-41.781	PV	A	60.000	HIROYA YAMAGUCHI	COLLISIONLESS SHOCK HEATING AND NON-EQUILIBRIUM PLASMA IN SN 1006	SN1006 offers an ideal laboratory to probe into the physics of the collisionless processes, because of its high shock velocity and the low ambient density. Here we propose Resolve observations of the two SNR rims, SE and NW, both dominated by thermal X-ray emission from the extremely low-ionized plasma, but with different shock velocities. The minimal goal is to accurately measure the ion (neon) and electron temperatures to constrain the efficiency of the collisionless electron heating and its velocity dependence. The ideal goal is to measure the temperatures of various heavy elements (N, O, Ne, Mg, Si, and Fe) to investigate the relationship between their temperatures and atomic mass. A short observation of the SNR Center is also proposed to demonstrate the wide FoV of the Xtend.
80	SN1006_CENTER	225.788	-41.962	PV	A	20.000	HIROYA YAMAGUCHI	COLLISIONLESS SHOCK HEATING AND NON-EQUILIBRIUM PLASMA IN SN 1006	SN1006 offers an ideal laboratory to probe into the physics of the collisionless processes, because of its high shock velocity and the low ambient density. Here we propose Resolve observations of the two SNR rims, SE and NW, both dominated by thermal X-ray emission from the extremely low-ionized plasma, but with different shock velocities. The minimal goal is to accurately measure the ion (neon) and electron temperatures to constrain the efficiency of the collisionless electron heating and its velocity dependence. The ideal goal is to measure the temperatures of various heavy elements (N, O, Ne, Mg, Si, and Fe) to investigate the relationship between their temperatures and atomic mass. A short observation of the SNR Center is also proposed to demonstrate the wide FoV of the Xtend.
81	SN1006_SE	225.899	-42.118	PV	C	80.000	HIROYA YAMAGUCHI	COLLISIONLESS SHOCK HEATING AND NON-EQUILIBRIUM PLASMA IN SN 1006	SN1006 offers an ideal laboratory to probe into the physics of the collisionless processes, because of its high shock velocity and the low ambient density. Here we propose Resolve observations of the two SNR rims, SE and NW, both dominated by thermal X-ray emission from the extremely low-ionized plasma, but with different shock velocities. The minimal goal is to accurately measure the ion (neon) and electron temperatures to constrain the efficiency of the collisionless electron heating and its velocity dependence. The ideal goal is to measure the temperatures of various heavy elements (N, O, Ne, Mg, Si, and Fe) to investigate the relationship between their temperatures and atomic mass. A short observation of the SNR Center is also proposed to demonstrate the wide FoV of the Xtend.
82	A2029 CENTER P1	227.73346	5.74425	PV	A	20.000	ERIC MILLER	NON-THERMAL PRESSURE SUPPORT IN RELAXED GALAXY CLUSTERS	We propose XRISM Resolve observations to measure the turbulence and bulk motion of the intracluster medium (ICM) in the outer regions of a relaxed galaxy cluster, Abell 2029. Such non-thermal pressure support causes a bias in cluster masses measured from X-rays under the assumption of hydrostatic equilibrium, and understanding its magnitude has broad implications for cosmological results that use cluster mass scaling relations. These will be the first direct measurements of the kinematic ICM structure outside the cluster core, and they will also confront predictions from numerical simulations that suggest non-thermal pressure support could be substantial here. We will simultaneously obtain Xtend spectral imaging at the virial radius to a depth exceeding existing Suzaku observations.
83	A2029 NORTH P2	227.73346	5.79425	PV	A	50.000	ERIC MILLER	NON-THERMAL PRESSURE SUPPORT IN RELAXED GALAXY CLUSTERS	We propose XRISM Resolve observations to measure the turbulence and bulk motion of the intracluster medium (ICM) in the outer regions of a relaxed galaxy cluster, Abell 2029. Such non-thermal pressure support causes a bias in cluster masses measured from X-rays under the assumption of hydrostatic equilibrium, and understanding its magnitude has broad implications for cosmological results that use cluster mass scaling relations. These will be the first direct measurements of the kinematic ICM structure outside the cluster core, and they will also confront predictions from numerical simulations that suggest non-thermal pressure support could be substantial here. We will simultaneously obtain Xtend spectral imaging at the virial radius to a depth exceeding existing Suzaku observations.
84	A2029 NORTH P3	227.73346	5.84425	PV	A	250.000	ERIC MILLER	NON-THERMAL PRESSURE SUPPORT IN RELAXED GALAXY CLUSTERS	We propose XRISM Resolve observations to measure the turbulence and bulk motion of the intracluster medium (ICM) in the outer regions of a relaxed galaxy cluster, Abell 2029. Such non-thermal pressure support causes a bias in cluster masses measured from X-rays under the assumption of hydrostatic equilibrium, and understanding its magnitude has broad implications for cosmological results that use cluster mass scaling relations. These will be the first direct measurements of the kinematic ICM structure outside the cluster core, and they will also confront predictions from numerical simulations that suggest non-thermal pressure support could be substantial here. We will simultaneously obtain Xtend spectral imaging at the virial radius to a depth exceeding existing Suzaku observations.
85	CIRCINUS X-1	230.17021	-57.16669	PV	C	40.000	TERUAKI ENOTO	DYNAMIC CHANGE OF ACCRETION STRUCTURE IN THE YOUNGEST X-RAY BINARY CIRCINUS X-1 HOSTING A WEAKLY MAGNETIZED NEUTRON STAR	The peculiar X-ray binary Circinus X-1 hosts a weakly magnetized neutron star and B5-A0 supergiant. Discovery of a natal supernova remnant makes Circinus X-1 the youngest X-ray binary hosting a neutron star in our Galaxy. Around the periastron passage, different types of X-ray flares, originating from disk or wind accretion, have been found with rich Fe-line structures, P-Cygni, emission, absorption, and edge features. XRISM provides accretion geometry and stellar wind information of this new-born peculiar binary.
86	T CORONA BOREALIS	239.87567	25.92017	PV	A	150.000	KOJI MUKAI	GRAVITATIONALLY REDSHIFTED 6.4 KEV LINE IN T CORONAE BOREALIS	We propose to measure the gravitational redshift at the surface of a massive accreting white dwarf (WD) in T CrB. It is a hard X-ray luminous symbiotic recurrent nova, with an estimated WD mass of >1.15 Msun, above the likely upper limit of WD birth mass. If confirmed, it implies that the WD in T CrB is growing in mass, establishing a subset of symbiotic stars as a viable progenitor channel of Type Ia supernovae. The primary X-ray source is located just above the WD surface, and it is the latter that produces the reflection continuum and the Fe Kalpha and Kbeta fluorescent lines. Measuring the centroids of both will enable us to determine the ionization state of the WD photosphere and the WD mass.
87	4U 1624-490	247.02304	-49.21111	PV	A	50.000	MARIA DIAZ TRIGO	MAPPING THE ACCRETION DISC WITH IONISED PLASMAS IN DIPPING SOURCES	We propose a 50 ks observation of the high-inclination dipping low-mass X-ray binary (LMXB) 4U 1916 (minimal) and a 50 ks of the dipping LMXB 4U 1624 (ideal). We will characterise the absorbers throughout the orbit (column densities, degree of ionisation and velocity width and shift) and determine their density and location. We will use the changes in the absorbers' properties to model the complex spectral changes throughout the orbit, including during dips, and to trace the variability of the absorber associated with changes in the source luminosity and hardness. We will use this information to make a full map of the accretion disc and identify potential zones of wind launching in LMXBs, shielded regions in the disc or zones that attenuate the central emission such as hot coronae.
88	GX340+00	251.44875	-45.61111	PV	A	150.000	ELISA COSTANTINI	THE X-RAY VIEW OF INTERSTELLAR DUST FROM SILICON TO IRON	We propose to observe the bright X-ray binary GX340+00 for 150 ks in order to explore the chemical and physical properties of the intervening interstellar dust. This source is the ideal candidate to study dense, never explored before, regions of the Galaxy. We will model the Si, S, Ca and Fe K-edges due to dust absorption. This will allow us to assess the silicate content (through Si and Fe) and its Ca inclusion in the core, as well as the sulphate content (through S and Fe). Additional science includes the study of the intrinsic highly ionized absorber/emitter.
89	PDS 456	262.0825	-14.2655	PV	A	150.000	KOUICHI HAGINO	THE DEFINITIVE PROOF OF AN ULTRA-FAST OUTFLOW	PDS 456 is host to the archetypical ultra-fast outflow (UFO) observed through its blue-shifted (0.25c and higher) H-like Fe absorption trough. This UFO is both of high statistical significance and per- sistent; it has been observed several times both in the Fe-K and in the soft X-ray band. Resolve will be able for the first time to measure the velocity profiles of the absorption lines, and in the ideal case their inner kinematic structure, which will shed light on the physical nature of the wind. The high throughput of Resolve in the ideal case will further allow to measure the variability of the UFO over shorter time scales than ever before.
90	KEPLER'S SNR	262.67192	-21.49064	PV	C	50.000	SATORU KATSUDA	THE PROGENITOR SYSTEM AND EXPLOSION PHYSICS FOR KEPLER'S SNR	We propose to observe Kepler's supernova remnant (SNR), which is a rare Type-Ia SNR associated with N-rich circumstellar medium (CSM). Our minimal goals are (1) to measure elemental abundances of the CSM and (2) to study electron-ion temperature nonequilibration. The CSM abundance will constrain the mass of the donor star in the progenitor system. If we are awarded 200 ks, then we will perform spatially-resolved spectroscopy, and we will reveal the CSM distribution. We will also clearly detect outermost ejecta materials, i.e., O and C (if present), from the southern rim, where the CSM contribution is much weaker than in the north. The amount of the outermost ejecta will allow us to infer explosion physics which also helps reveal the subclass of Kepler's SN.
91	GALACTICCENTER_3	266.30471	-29.17558	PV	C	100.000	MASAYOSHI NOBUKAWA	INVESTIGATION OF THE ACTIVITIES IN THE GALACTIC CENTER	The Galactic center (GC) contains many remarkable features resulting from high energy activities: the supermassive black hole (SMBH) Sgr A*, unresolved X-ray emission called as the Galactic center X-ray emission (GCXE), bipolar outflow structures, and X-ray reflection nebulae (XRNe). The main goal of this proposal is to elucidate the origin of the GCXE and to understand the past and present activities in the GC region by plasma diagnostics and measurement of gas dynamics using XRISM.
92	GALACTICCENTER_1	266.424	-29.00489	PV	A	100.000	MASAYOSHI NOBUKAWA	INVESTIGATION OF THE ACTIVITIES IN THE GALACTIC CENTER	The Galactic center (GC) contains many remarkable features resulting from high energy activities: the supermassive black hole (SMBH) Sgr A*, unresolved X-ray emission called as the Galactic center X-ray emission (GCXE), bipolar outflow structures, and X-ray reflection nebulae (XRNe). The main goal of this proposal is to elucidate the origin of the GCXE and to understand the past and present activities in the GC region by plasma diagnostics and measurement of gas dynamics using XRISM.
93	GALACTICCENTER_2	266.54292	-28.83411	PV	A	100.000	MASAYOSHI NOBUKAWA	INVESTIGATION OF THE ACTIVITIES IN THE GALACTIC CENTER	The Galactic center (GC) contains many remarkable features resulting from high energy activities: the supermassive black hole (SMBH) Sgr A*, unresolved X-ray emission called as the Galactic center X-ray emission (GCXE), bipolar outflow structures, and X-ray reflection nebulae (XRNe). The main goal of this proposal is to elucidate the origin of the GCXE and to understand the past and present activities in the GC region by plasma diagnostics and measurement of gas dynamics using XRISM.
94	GX13+1	273.63125	-17.15742	PV	A	30.000	CHRIS DONE	THE LAUNCH MECHANISM OF ACCRETION DISC WINDS: THE BEST TESTS FROM THE NEUTRON STAR BINARIES GX13+1 AND 2S0921-630	Accretion disc winds are clearly seen in black hole and neutron star binaries, but their origin is controversial. Are they magnetically driven, connecting them to the jet as well as to the accretion process itself, or are they thermal/radiative, driven by X-ray irradiation of the outer disc? GX13+1 persistently shows a massive wind in absorption, and is the most reliable LMXRB wind source to address the key question of the origin of the wind. A 30ks Resolve observation can directly measure the wind velocity profile along the line of sight, which will distinguish between magnetic and thermal-radiative acceleration. An additional 80ks observation of 2S0921 will instead shows the wind in emission, as its very high inclination angle means the X-ray source is obscured by the disc.
95	GX 13+1	273.63146	-17.15742	PV	A	60.000	LIA CORRALES	HOW LARGE DO INTERSTELLAR DUST GRAINS GET?	X-ray dust scattering cross-sections are particularly sensitive to the radius (a) of interstellar dust (ISD). High resolution X-ray spectroscopy of dust scattering halos can reveal X-ray scattering fine structure (XSFS) that arises in complement to X-ray absorption fine structure (XAFS). We propose a XRISM Resolve observation of the dust scattering halo of GX 13+1 that will test the hypothesis of a population of 0.05-0.5 micron sized silicate ISD grains (e.g., Zeegers et al. 2017).
96	RXJ 1856	284.1463	-37.9085	Regular	A	40.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
97	3C397 E	286.91812	7.13775	PV	C	100.000	HIROSHI NAKAJIMA	PROBING CENTRAL DENSITY OF TYPE IA SUPERNOVA PROGENITOR IN SINGLE DEGENERATE SYSTEM BY AN OBSERVATION OF 3C 397	Yield of Fe-peak elements (Cr, Mn, Fe, Ni) and Ti in Type Ia supernovae is the critical information for understanding their explosion mechanism. Especially in single degenerate systems where the progenitor mass is near the Chandrasekhar mass limit, mass ratios among Fe-peak elements and Ti are greatly sensitive to the central density of the progenitor. Here we propose a XRISM observation of 3C 397, a remnant of single degenerate Type Ia supernova. Utilizing the extremely high energy resolution of Resolve, we put strong constraint of {Cr,Mn,Ni}/Fe and Ti/Fe. We will observationally probe the central density of the progenitor for the first time.
98	W49B WEST	287.78042	9.11069	PV	A	100.000	MAKOTO SAWADA	TRACING A MISSING BRANCH IN THE SNR EVOLUTION: RECOMBINING PLASMA IN W49B	The Suzaku's discovery of recombining plasma in supernova remnants (SNRs) was a surprise because it is never expected in the fiducial Sedov model. We propose to observe the brightest recombining SNR W49B to reveal the origin of this new class of SNRs based on the high-resolution spectroscopy using XRISM/Resolve. We will identify the cooling process that formed the recombining state based on measurements of the electron temperature, ion temperature, and charge-state distribution. We will also constrain the progenitor type that regulates the SN environment, by bias-free measurements of the ejecta mass ratios of the Fe-group elements. Additionally, as an ideal goal, we will search for the signature of interaction with supra-thermal electrons and constrain the injection efficiency.
99	W49B EAST	287.79758	9.10211	PV	A	100.000	MAKOTO SAWADA	TRACING A MISSING BRANCH IN THE SNR EVOLUTION: RECOMBINING PLASMA IN W49B	The Suzaku's discovery of recombining plasma in supernova remnants (SNRs) was a surprise because it is never expected in the fiducial Sedov model. We propose to observe the brightest recombining SNR W49B to reveal the origin of this new class of SNRs based on the high-resolution spectroscopy using XRISM/Resolve. We will identify the cooling process that formed the recombining state based on measurements of the electron temperature, ion temperature, and charge-state distribution. We will also constrain the progenitor type that regulates the SN environment, by bias-free measurements of the ejecta mass ratios of the Fe-group elements. Additionally, as an ideal goal, we will search for the signature of interaction with supra-thermal electrons and constrain the injection efficiency.
100	SS 4433	287.9565	4.98272	PV	A	80.000	MEGUMI SHIDATSU	INVESTIGATING JET STRUCTURE OF SS 433	We propose an 80 ks observation of the Galactic microquasar SS 433 around an eclipse phase, consisting of a 50 ks exposure in eclipse and 30 ks out of eclipse, to investigate the jet structure by measuring the line widths of ionized metal lines emitted from different regions in the jets. High resolution X-ray spectroscopy of SS 433 with Resolve gives unique opportunity to understand the jet structure at supercritical accretion rates. The jet collimation of SS 433 can be resolved by comparing the velocity dispersions of Fe XXVI and Si XIV Ly alpha lines, and more direct evidence can be obtained from a comparison between the line structures in eclipse and and non-eclipse phases.
101	4U 1916-053	289.69946	-5.23808	PV	A	50.000	MARIA DIAZ TRIGO	MAPPING THE ACCRETION DISC WITH IONISED PLASMAS IN DIPPING SOURCES	We propose a 50 ks observation of the high-inclination dipping low-mass X-ray binary (LMXB) 4U 1916 (minimal) and a 50 ks of the dipping LMXB 4U 1624 (ideal). We will characterise the absorbers throughout the orbit (column densities, degree of ionisation and velocity width and shift) and determine their density and location. We will use the changes in the absorbers' properties to model the complex spectral changes throughout the orbit, including during dips, and to trace the variability of the absorber associated with changes in the source luminosity and hardness. We will use this information to make a full map of the accretion disc and identify potential zones of wind launching in LMXBs, shielded regions in the disc or zones that attenuate the central emission such as hot coronae.
102	CYGNUS X-1	299.59033	35.20161	PV	A	100.000	JON MILLER	WARPS, WINDS, AND REFLECTION IN THE BLACK HOLE CYGNUS X-1	Cygnus X-1 is the archetype stellar-mass black hole. It is persistent, and bright (0.25-0.75~Crab in soft X-rays), making it a popular testing ground for accretion flow models of all types. Among many other potential tests, observations with Resolve can reveal a warped disk, test models of binary evolution, and discover whether or not winds are launched from small disks in wind-fed systems. Studies related to the massive, 09.7 Iab supergiant companion wind in Cygnus X-1 are not the focus of this proposal, but issues central to massive stars can also be explored with Resolve. Apart from addressing important science, Cygnus X-1 is an important PV-phase test case for bright sources that will inform similar observations in normal mission cycles.
103	ABELL 3667 CF IN	303.23958	-56.88617	PV	C	180.000	YUTO ICHINOHE	GAS DYNAMICS IN THE MOST STRIKING CLUSTER COLD FRONT	Cluster mergers are the most energetic events in the Universe since the Big Bang. A large fraction of the merger energy is dissipated in the ICM, a process that depends on a number of unknown microphysical properties of the ICM. Resolve will provide the first opportunity to detect and map the bulk and turbulent velocities in the ICM of nearby merging systems. We propose to observe a textbook example of a cold front in A3667, a striking phenomenon caused by a merger. Resolve observations of this cold front would yield the bulk and turbulent velocities across the front, determining the origin of the front and providing a basis for the derivation of microphysical constraints from cold fronts, and answer a host of other interesting questions.
104	CYG X-3	308.10708	40.95775	PV	A	40.000	TIMOTHY KALLMAN	UNVEILING THE BLACK HOLE IN CYG X-3	We propose a 40 ks (minimal)/80 ks (ideal) observation of the unique and enigmatic high mass X-ray binary (HMXB) Cyg X-3. The iron line region in the Cyg X-3 spectrum contains hints of the dynamical effects of the black hole in this system. Improved measurements of the iron line radial velocity curve can be used to refine mass estimates for the black hole. In the soft state, there is surprising absorption from intermediate ion stages of iron, superimposed on a broad and complex emission. In the hard state the line is narrow and components of the line may have shifts indicative of the relativistic jet.
105	P7_IN	313.593	32.251	PV	A	30.000	HIROYUKI UCHIDA	DETECTING CHARGE EXCHANGE X-RAY EMISSIONS FROM THE CYGNUS LOOP	Charge exchange (CX) is an important process in shock physics. While the presence of CX X-ray emission from SNRs has been theoretically predicted, there is no robust evidence so far since conventional detectors cannot resolve cascade lines from higher excited states due to CX. Our recent observations of the Cygnus Loop with Suzaku and XMM-Newton revealed several promising results for the presence of CX. Here we propose to observe the remnant with XRISM for the purpose of a sure discovery of the CX for the first time from an SNR shell.
106	P7_OUT	313.631	32.288	PV	A	50.000	HIROYUKI UCHIDA	DETECTING CHARGE EXCHANGE X-RAY EMISSIONS FROM THE CYGNUS LOOP	Charge exchange (CX) is an important process in shock physics. While the presence of CX X-ray emission from SNRs has been theoretically predicted, there is no robust evidence so far since conventional detectors cannot resolve cascade lines from higher excited states due to CX. Our recent observations of the Cygnus Loop with Suzaku and XMM-Newton revealed several promising results for the presence of CX. Here we propose to observe the remnant with XRISM for the purpose of a sure discovery of the CX for the first time from an SNR shell.
107	Cygnus Loop	313.9091	31.0038	Regular	A	30.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
108	Cygnus Loop	313.9091	31.0038	Regular	A	30.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
109	NE	314.07	31.715	PV	A	20.000	HIROYUKI UCHIDA	DETECTING CHARGE EXCHANGE X-RAY EMISSIONS FROM THE CYGNUS LOOP	Charge exchange (CX) is an important process in shock physics. While the presence of CX X-ray emission from SNRs has been theoretically predicted, there is no robust evidence so far since conventional detectors cannot resolve cascade lines from higher excited states due to CX. Our recent observations of the Cygnus Loop with Suzaku and XMM-Newton revealed several promising results for the presence of CX. Here we propose to observe the remnant with XRISM for the purpose of a sure discovery of the CX for the first time from an SNR shell.
110	SE	314.102	30.081	PV	C	40.000	HIROYUKI UCHIDA	DETECTING CHARGE EXCHANGE X-RAY EMISSIONS FROM THE CYGNUS LOOP	Charge exchange (CX) is an important process in shock physics. While the presence of CX X-ray emission from SNRs has been theoretically predicted, there is no robust evidence so far since conventional detectors cannot resolve cascade lines from higher excited states due to CX. Our recent observations of the Cygnus Loop with Suzaku and XMM-Newton revealed several promising results for the presence of CX. Here we propose to observe the remnant with XRISM for the purpose of a sure discovery of the CX for the first time from an SNR shell.
111	SS CYGNI	325.67829	43.58611	PV	A	100.000	MANABU ISHIDA	OBSERVATIONS OF SS CYGNI IN QUIESCENCE AND OUTBURST	SS Cygni is one of the prototypical dwarf novae, which shows transitions between an optically quiescent state and an outburst state. In the outburst state, hard X-ray emission is thought to arise from coronae over an accretion disc, but their location is unclear. We will understand the corona geometry by measuring profiles of the coronal emission lines with the Resolve. In the quiescent state, on the other hand, it is commonly understood that the hard X-ray emission emanates from the optically thin boundary layer, yet its heating mechanism and radial profile of the BL plasma are both poorly understood. We will try to make them clear by means of spectroscopy of the emission lines from the plasma and the fluorescent iron K-alpha emission line with the Resolve.
112	SS CYGNI	325.67829	43.58611	PV	A	100.000	MANABU ISHIDA	OBSERVATIONS OF SS CYGNI IN QUIESCENCE AND OUTBURST	SS Cygni is one of the prototypical dwarf novae, which shows transitions between an optically quiescent state and an outburst state. In the outburst state, hard X-ray emission is thought to arise from coronae over an accretion disc, but their location is unclear. We will understand the corona geometry by measuring profiles of the coronal emission lines with the Resolve. In the quiescent state, on the other hand, it is commonly understood that the hard X-ray emission emanates from the optically thin boundary layer, yet its heating mechanism and radial profile of the BL plasma are both poorly understood. We will try to make them clear by means of spectroscopy of the emission lines from the plasma and the fluorescent iron K-alpha emission line with the Resolve.
113	CYG X-2	326.17146	38.34808	PV	C	40.000	LIA CORRALES	HOW DOES INTERSTELLAR OXYGEN AND IRON BECOME SOLID?	High resolution X-ray spectroscopy can probe the chemical composition and mineral structure of solid interstellar material in situ, more directly than any other wavelength, by observing X-ray absorption fine structure (XAFS). XAFS features produce complementary X-ray scattering fine structure (XSFS), which is imprinted on the spectrum of the dust scattering halos that are seen around bright Galactic point sources. We propose Resolve observations of the Cyg X-2 dust scattering halo that will measure XSFS from: (i) solid interstellar Oxygen, the most abundant interstellar metal, observed to easily change between solid and gas phases in the ISM, and (ii) solid interstellar Iron, a highly depleted heavy metal with an unknown pathway for incorporation into interstellar dust.
114	Cyg X-2	326.1715	38.3214	Regular	A	2.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
115	Cyg X-2	326.1715	38.3214	Regular	A	2.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
116	Cyg X-2	326.1715	38.3214	Regular	A	2.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
117	Cyg X-2	326.1715	38.3214	Regular	A	5.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
118	Cyg X-2	326.1715	38.3214	Regular	A	21.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
119	Cyg X-2	326.1715	38.3214	Regular	A	4.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
120	Cyg X-2	326.1715	38.3214	Regular	A	2.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
121	Cyg X-2	326.1715	38.3214	Regular	A	2.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
122	CYG X-2	326.22458	38.37444	PV	C	200.000	LIA CORRALES	HOW DOES INTERSTELLAR OXYGEN AND IRON BECOME SOLID?	High resolution X-ray spectroscopy can probe the chemical composition and mineral structure of solid interstellar material in situ, more directly than any other wavelength, by observing X-ray absorption fine structure (XAFS). XAFS features produce complementary X-ray scattering fine structure (XSFS), which is imprinted on the spectrum of the dust scattering halos that are seen around bright Galactic point sources. We propose Resolve observations of the Cyg X-2 dust scattering halo that will measure XSFS from: (i) solid interstellar Oxygen, the most abundant interstellar metal, observed to easily change between solid and gas phases in the ISM, and (ii) solid interstellar Iron, a highly depleted heavy metal with an unknown pathway for incorporation into interstellar dust.
123	PKS2155	329.7169	-30.2256	Regular	A	2.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
124	PKS2155	329.7169	-30.2256	Regular	A	2.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
125	PKS2155	329.7169	-30.2256	Regular	A	2.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
126	PKS2155	329.7169	-30.2256	Regular	A	2.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
127	PKS2155	329.7169	-30.2256	Regular	A	3.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
128	PKS2155	329.7169	-30.2256	Regular	A	3.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
129	PKS2155	329.7169	-30.2256	Regular	A	3.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
130	PKS2155	329.7169	-30.2256	Regular	A	3.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
131	PKS2155	329.7169	-30.2256	Regular	A	3.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
132	PKS2155	329.7169	-30.2256	Regular	A	5.000	ERIC MILLER	NOT_FILLED	NOT_FILLED
133	CAS A E/JET	350.92825	58.83358	PV	A	50.000	JACCO VINK	OBSERVING CAS A WITH XRISM: FROM A SUPERNOVA'S INNER WORKINGS TO THE IMPRINTS OF COSMIC-RAY ACCELERATION	Cas A is the archetypal young core-collapse SNR, with X-ray knots dominated by O-, Si-, and Fe-rich plasma, and a pair of Si-rich jets. Cas A is a bright source of IR dust emission. The primary observational goals are to detect emission from Na, Al, P, Cl, K, Cr in different ejecta layers, and spectral dust signatures: fluorescence lines, and low ionisation Si and Mg continuously injected into the plasma by grain sputtering. This results in a red tail to Mg/Si K-lines, in contrast to Ne/S K-lines. Secondary goals are accurate mapping of plasma parameters, and measuring Doppler shifts/broadening due to bulk motion and thermal broadening. Previous results based on centroiding were affected by varying line-blends, which can be disentangled by Resolve.

Used SQL

SELECT
object_name,center_ra,center_dec,
proposal_type,proposal_priority,awarded_exposure,pi_name,proposal_title,proposal_abstract
FROM xrism_proposal
WHERE proposal_priority IN ('A', 'C') AND center_RA > -1
order by center_ra

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