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 377

Download WgetScript

No.	observation_id	object_name	center_ra	center_dec	center_ra_b1950	center_dec_b1950	center_ecliptic_lon	center_ecliptic_lat	center_galactic_lon	center_galactic_lat	roll_angle	observation_start_time_mjd	observation_start_time	observation_end_time_mjd	observation_end_time	exposure	awarded_exposure	resolve_exposure	xtend_exposure	resolve_data_mode	resolve_with_filter_be	resolve_with_filter_fe55	resolve_with_filter_nd	resolve_with_filter_poly	resolve_with_filter_open	resolve_with_filter_undef	is_resolve_gatevalve_closed	is_resolve_mxs1	is_resolve_mxs2	is_resolve_mxs3	is_resolve_mxs4	xtend_number_modes	xtend_dataclass_file1	xtend_dataclass_file2	xtend_window1_exposure	xtend_window2_exposure	xtend_window1_burst_exposure	xtend_window2_burst_exposure	xtend_code	resolve_code	gen_code	processing_status	processing_date	public_date	distribution_date	processing_version	caldb_version	processing_software	proposal_id	proposal_abstract	proposal_category	proposal_category_code	proposal_priority	pi_name	co_pi_name	proposal_affiliated_country	proposal_cycle	proposal_type	proposal_title	observation_status	data_access_url	xtend_data_mode1	xtend_data_mode2	processing_count	remarks
1	202089010	Perseus_C2	49.94473	41.56233	49.11694	41.38167	58.61674	22.38793	150.54332	-13.22143	264.61225	61065.24241	2026-01-25 05:49:04	61066.64241	2026-01-26 15:25:04	64.238	59.000	64.238	61.705	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		61.705	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2026-01-30 12:50:48	2099-12-31 00:00:00	2026-01-31 12:50:49	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000024011	Active Galactic Nuclei (AGN) feedback regulates cooling and star formation in galaxy clusters. Its sphere of influence, imprinted on the intracluster medium (ICM), offers key insights into feedback physics and serves as a robust diagnostic for numerical models. We propose three pointings (166 ks total) to map the feedback sphere of influence in the Perseus cluster. This will yield the most detailed ICM kinematic map to date, covering the transition between feedback- and merger-dominated regions. We will investigate azimuthal variations in gas kinematics and metallicity, and address how AGN bubbles and sloshing arms transport and confine energy. Together with multiwavelength data, we will explore if/how AGN-driven turbulence triggers the radio mini-halo and thermal instabilities in the ICM.	GROUPS AND CLUSTERS OF GALAXIES	2	A	CONGYAO ZHANG		EUR	2	NOR	MAPPING THE AGN FEEDBACK SPHERE OF INFLUENCE IN PERSEUS	preprocessed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202089010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
2	102008010	Perseus_CAL2	49.95107	41.51144	49.1236	41.33081	58.60645	22.33771	150.57622	-13.26126	264.59599	61064.20421	2026-01-24 04:54:04	61065.24241	2026-01-25 05:49:04	47.116	40.000	47.116	42.085	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	31100010	320000A0	45.075	42.085	0.000	0.000	11110	313430	11310	PROCESSED	2026-01-30 11:42:26	2023-09-06 00:00:00	2026-01-31 11:42:27	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	2	CAL	AO2 Calibration Targets (1)	preprocessed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102008010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
3	102007010	Perseus_CAL1	49.95135	41.51161	49.12388	41.33099	58.60672	22.33782	150.5763	-13.261	264.61313	61063.16741	2026-01-23 04:01:04	61064.20421	2026-01-24 04:54:04	43.945	40.000	43.945	42.152	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		42.152	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2026-01-27 11:14:25	2023-09-06 00:00:00	2026-01-28 11:14:26	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	2	CAL	AO2 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102007010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
4	902002010	GS1354-64	209.53991	-64.73415	208.61407	-64.49075	236.1089	-48.24567	309.97731	-2.779	102.0024	61060.15144	2026-01-20 03:38:04	61063.16741	2026-01-23 04:01:04	128.637	100.000	128.637	13.468	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	107.524	0.000	0.000	13.468	11110	313430	11310	PROCESSED	2026-01-27 12:48:47	2023-09-06 00:00:00	2026-01-28 12:48:47	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029006	A new outburst is currently taking place in the black hole X-ray binary system known as GS 1354-64. The level of its flux has reached 100 milli-Crab, and it is continuing to rise. Based on the hard X-ray data with NuSTAR, the source is supposed to be a black hole candidate that is spinning at a high rate; however, XRISM has never been observed such a kind of binaries. In order to resolve the iron line region of GS 1354-64, we request a 100 kilo-seconds XRISM observation using Resolve. This could be helpful in isolating any narrow characteristics that were not able to be resolved by the CCD-resolution data that was collected in the past, and it could also yield more accurate measurements of the black hole spin.	BH AND NS BINARIES	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF GS 1354-64	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902002010/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
5	202034010	AWM7_P2	43.55685	41.60485	42.74777	41.40179	53.6692	23.84376	146.28442	-15.6323	269.99929	61055.37991	2026-01-15 09:07:04	61060.15144	2026-01-20 03:38:04	218.122	200.000	218.122	209.941	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		209.941	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2026-01-24 10:32:18	2027-01-29 00:00:00	2026-01-25 10:32:18	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022156	AGN feedback regulates gas cooling in galaxy clusters, but the precise role of AGN-driven turbulence remains unclear. We propose three XRISM observations of the cool-core cluster AWM 7 to map its ICM velocity dispersion and directly compare with Perseus Cluster PV studies. Unlike Perseus, AWM 7 shows no signs of active AGN feedback, but shares similar redshift and sloshing signatures. By matching radial and line-of-sight scales, these observations test whether small-scale gas motions found in Perseus arise from AGN feedback. Our goals include measuring turbulence, non-thermal pressure support, chemical abundance profiles, and resonant scattering. AWM 7, as a bright feedback-free cluster, provides a unique opportunity to isolate the kinematic role of AGN feedback in cluster cores.	GROUPS AND CLUSTERS OF GALAXIES	2	B	HANNAH MCCALL		USA	2	NOR	A TALE OF TWO DRIVERS: UNDERSTANDING THE KINEMATIC ROLE OF AGN FEEDBACK	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202034010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
6	102004010	3C273	187.27573	2.05376	186.63636	2.3301	185.86695	4.7739	289.94531	64.36088	112.45079	61054.44796	2026-01-14 10:45:04	61055.37991	2026-01-15 09:07:04	37.094	30.000	37.094	30.379	PX_NORMAL	N	Y	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	32.495	30.379	0.000	0.000	11110	313430	11310	PROCESSED	2026-01-20 09:04:05	2023-09-06 00:00:00	2026-01-21 09:04:06	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	2	CAL	AO2 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102004010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
7	202008010	MRK841	226.00502	10.43815	225.40136	10.63256	220.18937	26.59297	11.2096	54.63225	120.00025	61050.05005	2026-01-10 01:12:04	61054.44796	2026-01-14 10:45:04	180.205	150.000	180.205	153.640	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		153.640	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2026-01-20 12:50:38	2027-01-22 00:00:00	2026-01-21 12:50:38	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022095	Mrk 841 is a bright Seyfert 1 galaxy with an X-ray spectrum rich in spectral features, making it an ideal target to investigate both emission and absorption processes. Observations by major X-ray observatories have revealed a multi-component Fe Kalpha emission line, characterized by a persistent narrow core and a transient broad component. The detection of relativistically redshifted narrow emission features and blueshifted absorption lines points to the presence of a Kerr black hole at the galaxy s center and of material outflowing at mildly relativistic velocities. We propose a 150 ks XRISM observation to resolve these spectral features with unprecedented precision, providing new insights into the structure, dynamics, and variability of the circumnuclear environment of Mrk 841.	NON-JET-DOMINATED AGN	2	B	VITTORIA GIANOLLI		USA	2	NOR	THE MANY FACES OF MRK 841: UNVEILING EMISSION AND ABSORPTION FEATURES WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202008010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
8	202076010	ABELL3571_SE	206.92589	-32.9046	206.20502	-32.65555	217.04039	-20.31512	316.35768	28.49603	90.00387	61048.18755	2026-01-08 04:30:04	61050.05005	2026-01-10 01:12:04	69.345	60.000	69.345	63.723	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		63.723	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2026-01-14 06:10:50	2027-01-17 00:00:00	2026-01-15 06:10:52	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000021432	We propose six XRISM pointing observations of A3571, totaling 300 ks to constrain the velocity field and reveal how sloshing redistributes energy, metals, and entropy throughout the core. Velocity, temperature, and metal abundance map from AO1, covering three 150x150 kpc regions, exhibit patterns consistent with sloshing motions viewed nearly edge-on, likely triggered by the passage of the nearby A3572 cluster, which is X-ray faint relative to its concentration of galaxies. With the proposed observations, we will expand coverage out to 200-300 kpc from the BCG. A3571, despite its regular elliptical morphology, shows no strong evidence of a cool core, making it an ideal target for mapping ICM velocity fields driven by sloshing.	GROUPS AND CLUSTERS OF GALAXIES	2	A	KYOKO MATSUSHITA		JAP	2	NOR	SETTLING DOWN AFTER MASSIVE DISTURBANCE: HEATING, SLOSHING AND METAL UPLIFT IN ABELL 3571	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202076010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
9	202035010	ESP39607	11.58624	-40.09706	10.99168	-40.37015	351.25705	-40.69624	307.26157	-76.98834	256.37097	61045.96741	2026-01-05 23:13:04	61048.18755	2026-01-08 04:30:04	112.123	90.000	112.123	102.357	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		102.357	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2026-01-14 06:40:05	2027-01-17 00:00:00	2026-01-15 06:40:06	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022171	We propose to investigate a 4.8 keV absorption feature in the z=0.201 AGN ESP39607, recently detected in two NuSTAR observations (>4sigma combined significance) and identified as a potential sustained ultra-fast inflow (UFI). The feature, likely arising from Fe XXV and/or Fe XXVI Ka transitions, suggests inflow velocities of 0.15-0.20c and has persisted across two epochs (2023 and 2024). With XRISM, we aim to: 1) confirm the feature at >6sigma, and 2) conduct detailed spectroscopy to determine its origin and physical properties. This would provide the clearest evidence of a UFI to date, as previous detections never exceeded 3-3.5sigma. The year-long persistence of the feature offers a rare and time-sensitive opportunity to capture this phenomenon before it potentially fades.	NON-JET-DOMINATED AGN	2	A	ALESSANDRO PECA		USA	2	NOR	PROBING A SUSTAINED ULTRA-FAST INFLOW WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202035010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
10	202053010	AB_DORADUS	82.18765	-65.44704	82.15146	-65.485	15.71947	-86.63608	275.29884	-33.04549	200.09533	61040.82157	2025-12-31 19:43:04	61045.96741	2026-01-05 23:13:04	351.366	200.000	351.366	313.488	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	335.323	313.488	0.000	0.000	11110	313430	11310	PROCESSED	2026-01-09 10:30:02	2027-01-13 00:00:00	2026-01-10 10:30:03	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000021259	Young Sun-like stars frequently produce superflares, generating hot coronal upflows and coronal mass ejections that shape early planetary atmospheres. However, their coronal dynamics remain poorly understood, limiting our ability to model their impact on planets. We propose a 200 ks XRISM observation of the young Sun-like star AB Doradus. We expect to detect at least five superflares with a 97% probability. Our goal is to detect Doppler blueshift components mainly from the Fe line profile above 6.7 keV, the most promising diagnostic of coronal dynamics. This will reveal the properties/origins of flare-driven outflows and test whether they align with solar physics. The results will advance models of early Sun's activity and constrain key plasma/radiation parameters for early planets.	STELLAR CORONAE, WINDS, AND YOUNG STARS	2	A	KOSUKE NAMEKATA		JAP	2	NOR	UNVEILING CORONAL DYNAMICS DURING FLARES ON YOUNG SUN-LIKE STAR AB DORADUS: A PROXY FOR SPACE WEATHER FROM THE EARLY SUN	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202053010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
11	202086010	A1689	197.87167	-1.34055	197.22922	-1.07511	196.99411	5.77226	313.35253	61.12491	115.00173	61035.39519	2025-12-26 09:29:04	61040.82157	2025-12-31 19:43:04	227.079	200.000	227.079	221.275	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		221.275	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2026-01-06 10:42:53	2027-01-09 00:00:00	2026-01-07 10:42:54	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000023003	Determining cluster mass accurately is important for precision cosmology with clusters. As the X-ray hydrostatic equilibrium mass is subject to the bias from the bulk motion and turbulence in the intracluster medium (ICM), it is important to understand the X-ray mass - lensing mass comparison, as the latter measure also has its own systematics. In this proposal, we request XRISM data of one of the best studied cluster in lensing A1689 to study the line-of-sight (LoS) merger in its core, which is suggested from the previous studies and may hold the key to understand the X-ray mass - lensing mass discrepancy in the cluster. We will search for multiple LoS velocity components to constrain the ICM distribution along the LoS. The ICM turbulence in its weak cool core will also be constrained.	GROUPS AND CLUSTERS OF GALAXIES	2	A	MING SUN	NOBUHIRO OKABE	USJ	2	NOR	STUDYING HOT GAS KINEMATICS IN A1689 WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202086010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
12	202046010	GX301-2	186.65548	-62.7713	185.95575	-62.4945	221.51974	-52.6288	300.09771	-0.03619	98.71507	61032.64519	2025-12-23 15:29:04	61035.39519	2025-12-26 09:29:04	144.372	100.000	144.372	124.571	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	133.247	124.571	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-30 10:13:36	2027-01-08 00:00:00	2025-12-31 10:13:36	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022228	Despite decades of theoretical and observational studies, wind-driven accretion in High-Mass X-ray binaries is poorly understood. Our understanding is limited because matter accreted from stellar wind by a compact object has never been directly observed. A XRISM observation of GX 301-2 on February 1st, 2025, which caught the end of the pre-periastron flare, produced clear spectroscopic evidence of highly ionized plasma moving towards the neutron star. This makes GX 301-2 unique in its potential for studying infalling matter in wind-driven accretion. The pre-periastron flare is hypothesized to originate from the neutron star crossing a high-density stream. XRISM provides an opportunity to test the stream hypothesis and constrain the models of wind-fed accretion onto pulsars. Since the previ	BH AND NS BINARIES	2	A	MAURICE LEUTENEGGER		USA	2	NOR	DIRECT OBSERVATION OF WIND-FED ACCRETION IN GX301-2	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202046010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
13	202098010	TYCHO_SW	6.22479	64.11357	5.52573	63.83671	42.75701	53.76434	120.03968	1.39096	250.99852	61030.20213	2025-12-21 04:51:04	61032.64519	2025-12-23 15:29:04	160.732	100.000	160.732	104.038	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		104.038	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-26 12:54:21	2026-12-31 00:00:00	2025-12-27 12:54:22	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000024044	We propose a 100 ks observation to unveil the 3D ejecta properties of the southwest region of Tycho's supernova remnant to constrain the explosion mechanism and environment of a Type Ia progenitor. We will 1) resolve the line complexes, measure temperatures, non-equilibrium ionization times and abundances, distinguish line redshifts from the front and rear emitting shells, determine broadenings of individual elements from silicon to iron, and quantify the presence of rare elements; 2) study the impact of the environment by comparing with the northeast observation of Tycho s SNR where the remnant interacts with a denser interstellar medium; 3) determine the plasma properties where bright nonthermal stripes are located and in Si and iron knots associated with radio structures.	SUPERNOVA REMNANTS	2	A	ANNE DECOURCHELLE		EUR	2	NOR	UNVEILING THE 3D EJECTA PROPERTIES IN TYCHO'S SNR: HIGH RESOLUTION SPECTROSCOPY AT THE SOUTHWEST REGION	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202098010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
14	202065010	A3376_CORE	90.55619	-39.9467	90.1488	-39.945	90.95179	-63.38415	246.49429	-25.98686	169.9929	61022.04588	2025-12-13 01:06:04	61030.20213	2025-12-21 04:51:04	345.901	300.000	345.901	310.581	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		310.581	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-26 19:27:48	2026-12-31 00:00:00	2025-12-27 19:27:49	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000021398	We propose 450 ks XRISM observations of a late-phase merging cluster Abell 3376 to determine the bulk motion and turbulence of the intracluster medium (ICM) within a statistical error of ~23-53 km/s (1 sigma). Two pointings are proposed. Priority A (Core, 300 ks): We determine the direction of the gas flow around the second brightest cluster galaxy (BCG) which represents the peculiar bent radio jets. We will distinguish between the stripping and slingshot mechanisms at a 5 sigma level. Priority B (Downstream, 150 ks): We discover the developed turbulence, conservative 200~km/s, at a 3 sigma level. We will confirm the growth of Kelvin-Helmholtz instability with a large Reynolds number.	GROUPS AND CLUSTERS OF GALAXIES	2	B	TAKUYA AKAHORI		JAP	2	NOR	UNTANGLING NEW MYSTERY OF ICM MOTION IN ABELL 3376 WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202065010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
15	202001020	NGC4839	194.29993	27.48928	193.6945	27.75937	181.16117	30.70722	49.01408	88.67016	133.82568	61020.27019	2025-12-11 06:29:04	61022.04588	2025-12-13 01:06:04	81.403	75.000	81.403	78.936	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		78.936	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-17 10:50:39	2026-12-19 00:00:00	2025-12-18 10:50:39	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022046	We propose to observe the inner part of the ram pressure stripped tail of the galaxy group NGC 4839, which is infalling into the Coma cluster, for 190ks with Resolve. A surface brightness fluctuation analysis of the inner tail with Chandra has revealed a turbulent Mach number of 0.5, which should result in a velocity dispersion of 320km/s. The low redshift of the system makes this the brightest stripped tail in X-rays and mitigates the complicating factor of XRISM's large PSF, which combined with its high metallicity of 0.8 Z_solar makes it the only tail whose velocity dispersion can be measured with a realistic exposure time with XRISM. This system therefore provides a unique opportunity to probe the generation of turbulence due to merging activity in galaxy clusters.	GROUPS AND CLUSTERS OF GALAXIES	2	A	STEPHEN WALKER		USA	2	NOR	XRISM OBSERVATIONS OF TURBULENCE IN A RAM PRESSURE STRIPPED GALAXY GROUP TAIL FALLING THROUGH THE COMA CLUSTER	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202001020/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
16	202058010	2S0921-630	140.64536	-63.2945	140.35523	-63.07963	195.11902	-68.90255	281.83551	-9.33925	122.64673	61016.41046	2025-12-07 09:51:04	61020.27019	2025-12-11 06:29:04	167.666	135.000	167.666	127.901	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		127.901	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-16 15:13:07	2026-12-18 00:00:00	2025-12-17 15:13:08	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000021320	In most XRISM programs, spectral lines observed with Resolve are formed in the NLTE conditions. For proper interpretations of the observed spectra, spectral synthesis based on the numerical RT calculation is a requisite. Recently, intensive efforts have been made to develop widely-used RT codes to be applicable to the high-resolution X-ray spectroscopy. Resolve observations of X-ray binaries are producing gorgeous datasets with many new Fe features critical to benchmarking the RT code developments and deriving key plasma parameters. The next obvious step is to extend the diagnostics to lower-Z elements, for which Resolve has advantages. We propose to observe 2S 0921 630, the brightest ADC source with a log xi=2-3 plasma.	BH AND NS BINARIES	2	B	MASAHIRO TSUJIMOTO		JAP	2	NOR	BENCHMARKING THE RADIATIVE TRANSFER CODES WITH AN ACCRETION DISK CORONA SOURCE 2S0921-630	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202058010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
17	202096010	NGC7469	345.81562	8.8739	345.18562	8.60437	350.47256	13.75891	83.09906	-45.46705	248.10312	61013.80838	2025-12-04 19:24:04	61016.41046	2025-12-07 09:51:04	109.552	100.000	109.552	102.388	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		102.388	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-13 07:06:08	2026-12-18 00:00:00	2025-12-14 07:06:09	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000024042	We propose a 100 ks XRISM observation of the Seyfert galaxy NGC 7469 to investigate the interplay of accretion and ejection phenomena in its nuclear region. Recent XMM and Chandra HETG data revealed a complex Fe K structure with narrow and broad FeII k\alpha, outflowing ionized Fe XXV/XXVI emission, candidate inflow features (at v_in~0.09c), and a persistent ultra-fast outflow (v_out~0.42c), one of the fastest ever observed, challenging current radiation-driving models. XRISM/Resolve will resolve the Fe K complex, confirm and characterize the inflow features, and precisely measure the UFO properties, offering unique insights into the dynamics, ionization, and launching mechanisms of AGN winds, and providing stringent constraints on AGN feeding and feedback models.	NON-JET-DOMINATED AGN	2	B	GIORGIO LANZUISI		EUR	2	NOR	THE XRISM UNPRECEDENTED VIEW OF THE OUTFLOW/INFLOW IN NGC 7469	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202096010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
18	202001010	NGC4839	194.30011	27.48879	193.69467	27.75888	181.16159	30.70684	48.99175	88.67014	133.82507	61010.67435	2025-12-01 16:11:04	61013.80838	2025-12-04 19:24:04	137.095	190.000	137.095	127.540	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		127.540	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-09 11:10:57	2026-12-19 00:00:00	2025-12-10 11:10:57	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022046	We propose to observe the inner part of the ram pressure stripped tail of the galaxy group NGC 4839, which is infalling into the Coma cluster, for 190ks with Resolve. A surface brightness fluctuation analysis of the inner tail with Chandra has revealed a turbulent Mach number of 0.5, which should result in a velocity dispersion of 320km/s. The low redshift of the system makes this the brightest stripped tail in X-rays and mitigates the complicating factor of XRISM's large PSF, which combined with its high metallicity of 0.8 Z_solar makes it the only tail whose velocity dispersion can be measured with a realistic exposure time with XRISM. This system therefore provides a unique opportunity to probe the generation of turbulence due to merging activity in galaxy clusters.	GROUPS AND CLUSTERS OF GALAXIES	2	A	STEPHEN WALKER		USA	2	NOR	XRISM OBSERVATIONS OF TURBULENCE IN A RAM PRESSURE STRIPPED GALAXY GROUP TAIL FALLING THROUGH THE COMA CLUSTER	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202001010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
19	202009020	1ES1927+654	291.8332	65.56517	291.7599	65.46181	3.66292	81.13211	96.98442	20.9601	224.05952	61007.86046	2025-11-28 20:39:04	61010.67435	2025-12-01 16:11:04	129.106	130.000	129.106	131.230	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		131.230	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-05 10:50:13	2099-12-31 00:00:00	2025-12-06 10:50:13	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022103	1ES~1927+654 is an enigmatic post-changing-look active galaxy (CL-AGN) which has shown a recent rise in the soft X-ray flux (by 10 times) and radio flux (by 60 times) in a few months, followed by detection of radio outflows (v=0.2c) with VLBA. In December 2024 for the first time a 2% linear polarization (in VLA X-band radio) was detected (priv comm.), revealing a real-time magnetic field alignment at the core of the AGN as the jet/UFO forms and evolves. Here we propose to observe the source with XRISM for a 200 ks snapshot to detect and characterize the emerging Fe K emission line and the UFOs in the 7-9 keV energy band. An affirmative detection of UFOs with XRISM will be the first ever `direct' (real-time) evidence of involvement of magnetic fields in the launching of UFOs.	NON-JET-DOMINATED AGN	2	A	SIBASISH LAHA		USA	2	NOR	AN ONGOING MAGNETIC FIELD ALIGNMENT CONTEMPORANEOUS WITH A JET/UFO LAUNCH IN THE POST-CHANGING-LOOK AGN 1ES~1927+654.	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202009020/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
20	902001140	C2025_N1	182.41588	-0.23706	181.77521	0.04115	182.31097	0.74321	281.08434	60.85033	109.48244	61007.71880	2025-11-28 17:15:04	61007.86046	2025-11-28 20:39:04	6.374	60.000	6.374	6.336	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		6.336	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 10:33:20	2023-09-06 00:00:00	2025-12-04 10:33:20	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001140/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
21	902001130	C2025_N1	182.52798	-0.27664	181.88731	0.00155	182.42958	0.75144	281.32842	60.84989	109.4821	61007.58616	2025-11-28 14:04:04	61007.71880	2025-11-28 17:15:04	5.937	60.000	5.937	6.336	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		6.336	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 10:11:51	2023-09-06 00:00:00	2025-12-04 10:11:51	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001130/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
22	902001120	C2025_N1	182.64021	-0.31645	181.99952	-0.03828	182.5484	0.75951	281.57287	60.84883	109.48209	61007.45352	2025-11-28 10:53:04	61007.58616	2025-11-28 14:04:04	4.169	60.000	4.169	3.970	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		3.970	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 10:15:58	2023-09-06 00:00:00	2025-12-04 10:15:58	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001120/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
23	902001110	C2025_N1	182.739	-0.3514	182.0983	-0.07325	182.65294	0.7667	281.78795	60.84762	109.48254	61007.32088	2025-11-28 07:42:04	61007.45352	2025-11-28 10:53:04	3.556	60.000	3.556	3.335	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		3.335	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 10:18:07	2023-09-06 00:00:00	2025-12-04 10:18:07	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001110/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
24	902001100	C2025_N1	182.85376	-0.3921	182.21306	-0.11398	182.77444	0.77495	282.03789	60.84568	109.48144	61007.17991	2025-11-28 04:19:04	61007.32088	2025-11-28 07:42:04	3.544	60.000	3.544	3.002	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		3.002	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 10:08:44	2023-09-06 00:00:00	2025-12-04 10:08:45	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001100/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
25	902001090	C2025_N1	182.97252	-0.43375	182.3318	-0.15565	182.89997	0.78391	282.29616	60.84363	109.48248	61007.04449	2025-11-28 01:04:04	61007.17991	2025-11-28 04:19:04	4.034	60.000	4.034	4.228	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		4.228	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 09:54:36	2023-09-06 00:00:00	2025-12-04 09:54:36	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001090/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
26	902001080	C2025_N1	183.08616	-0.47389	182.44543	-0.19582	183.02022	0.79221	282.54347	60.84093	109.48284	61006.92435	2025-11-27 22:11:04	61007.04449	2025-11-28 01:04:04	4.764	60.000	4.764	5.961	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		5.961	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 09:40:27	2023-09-06 00:00:00	2025-12-04 09:40:27	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001080/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
27	902001070	C2025_N1	183.1967	-0.51303	182.55595	-0.23498	183.13722	0.8002	282.78403	60.83777	109.48131	61006.79171	2025-11-27 19:00:04	61006.92435	2025-11-27 22:11:04	5.950	60.000	5.950	6.342	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		6.342	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 09:39:21	2023-09-06 00:00:00	2025-12-04 09:39:21	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001070/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
28	902001060	C2025_N1	183.30718	-0.55183	182.66642	-0.27381	183.25403	0.80847	283.02423	60.8345	109.48287	61006.65977	2025-11-27 15:50:04	61006.79171	2025-11-27 19:00:04	5.892	60.000	5.892	6.344	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		6.344	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 09:34:14	2023-09-06 00:00:00	2025-12-04 09:34:14	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001060/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
29	902001050	C2025_N1	183.41771	-0.59118	182.77693	-0.31319	183.3711	0.81625	283.26478	60.83028	109.48141	61006.52782	2025-11-27 12:40:04	61006.65977	2025-11-27 15:50:04	4.994	60.000	4.994	4.878	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		4.878	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 09:27:07	2023-09-06 00:00:00	2025-12-04 09:27:07	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001050/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
30	902001040	C2025_N1	183.52717	-0.63	182.88638	-0.35204	183.48699	0.82408	283.50287	60.82581	109.4828	61006.39449	2025-11-27 09:28:04	61006.52782	2025-11-27 12:40:04	2.764	60.000	2.764	3.572	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		3.572	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 09:04:55	2023-09-06 00:00:00	2025-12-04 09:04:55	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001040/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
31	902001030	C2025_N1	183.62518	-0.66446	182.98437	-0.38652	183.59062	0.83137	283.71579	60.82175	109.48242	61006.27088	2025-11-27 06:30:04	61006.39449	2025-11-27 09:28:04	1.159	60.000	1.159	2.820	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		2.820	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 08:56:37	2023-09-06 00:00:00	2025-12-04 08:56:37	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001030/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
32	902001020	C2025_N1	183.74044	-0.70522	183.09962	-0.42732	183.7126	0.83971	283.96628	60.8163	109.48136	61006.12019	2025-11-27 02:53:04	61006.27088	2025-11-27 06:30:04	4.564	60.000	4.564	3.480	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	1	300000A0		3.480	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 08:57:44	2023-09-06 00:00:00	2025-12-04 08:57:44	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001020/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
33	902001010	C2025_N1	183.85607	-0.74641	183.21524	-0.46854	183.83509	0.8478	284.21766	60.81008	109.48118	61005.97296	2025-11-26 23:21:04	61006.12019	2025-11-27 02:53:04	4.410	60.000	4.410	4.902	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		4.902	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 08:52:31	2023-09-06 00:00:00	2025-12-04 08:52:31	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000029002	C/2025 N1 represents the first credible opportunity to detect soft X-ray emission from solar wind charge exchange (SWCX) in an interstellar comet. Interstellar comets are important because they provide direct samples of volatile substances from other planetary systems, preserving the chemical composition of exsolar protoplanetary discs and enabling comparisons between extrasolar planet-formation environments and our own. When active near perihelion, their neutral comae can attain scales of 10^5--10^6 km. SWCX emissions from this extensive "halo" identify the content and spatial distribution of neutral gas and volatile material, a capability beyond that of optical and infrared studies.	SOLAR SYSTEM	9	A	XRISM Collaboration		DDT	2	DDT-TOO	DDT TOO REQUEST OF THE INTERLOPER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/902001010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
34	202009010	1ES1927+654	291.83237	65.56521	291.75907	65.46185	3.66254	81.13245	96.98434	20.96043	224.05994	61004.36324	2025-11-25 08:43:04	61005.97296	2025-11-26 23:21:04	34.587	200.000	34.587	73.909	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		73.918	0.008	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-03 04:12:02	2099-12-31 00:00:00	2025-12-04 04:12:03	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022103	1ES~1927+654 is an enigmatic post-changing-look active galaxy (CL-AGN) which has shown a recent rise in the soft X-ray flux (by 10 times) and radio flux (by 60 times) in a few months, followed by detection of radio outflows (v=0.2c) with VLBA. In December 2024 for the first time a 2% linear polarization (in VLA X-band radio) was detected (priv comm.), revealing a real-time magnetic field alignment at the core of the AGN as the jet/UFO forms and evolves. Here we propose to observe the source with XRISM for a 200 ks snapshot to detect and characterize the emerging Fe K emission line and the UFOs in the 7-9 keV energy band. An affirmative detection of UFOs with XRISM will be the first ever `direct' (real-time) evidence of involvement of magnetic fields in the launching of UFOs.	NON-JET-DOMINATED AGN	2	A	SIBASISH LAHA		USA	2	NOR	AN ONGOING MAGNETIC FIELD ALIGNMENT CONTEMPORANEOUS WITH A JET/UFO LAUNCH IN THE POST-CHANGING-LOOK AGN 1ES~1927+654.	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202009010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
35	202036010	4U1957+115	299.85038	11.70867	299.25951	11.57134	304.90639	31.6019	51.30818	-9.33028	241.11244	61003.05560	2025-11-24 01:20:04	61004.36324	2025-11-25 08:43:04	62.207	50.000	62.207	55.473	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	59.336	55.473	0.000	0.000	11110	313430	11310	PROCESSED	2025-11-29 08:37:24	2026-12-03 00:00:00	2025-11-30 08:37:25	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022172	Black hole (BH) spin measurements in X-ray binaries (XBs) are crucial for understanding BH formation, but current techniques face significant limitations due to spectral complexity and the transient nature of most systems. In particular, relativistic reflection measurements suffer from uncertainties related to unresolved narrow features and continuum modeling, especially in low-mass XBs (LMXBs), which are only rarely observable, during outbursts. We propose a 50 ks XRISM observation of 4U 1957+115 - the only persistent BH LMXB - to detect and characterize narrow features in the Fe band. This will quantify their impact on spin measurements and test for a tentative ultra-fast outflow. The results will improve reflection modeling and refine spin estimates across the BH population.	BH AND NS BINARIES	2	B	PAUL DRAGHIS		USA	2	NOR	PROBING THE ONLY PERSISTENT BH LMXB: 4U1957+115	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202036010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
36	202054010	CYG_X-2	326.17165	38.3214	325.65371	38.09086	346.69932	47.95668	87.32829	-11.31646	251.76107	61002.03407	2025-11-23 00:49:04	61003.05560	2025-11-24 01:20:04	46.020	40.000	46.020	5.759	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	45.975	0.000	0.000	5.759	11110	313430	11310	PROCESSED	2025-11-28 09:02:49	2026-12-06 00:00:00	2025-11-29 09:02:49	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000021261	Cyg X-2 was observed as part of the XRISM in-flight calibration campaign for the Resolve point spread function. Although these data were not originally intended for spectroscopy---resulting in low signal-to-noise and several analytic uncertainties---we have nonetheless succeeded in resolving the complex Fe K-band emission-line components likely coming from the accretion disk corona. In this proposal, by achieving substantially higher S/N with an on-axis observation, we aim to reject models that remain viable with the current data, the disk line model. We also will compare it with other already-observed Z-track sources and establish a comprehensive picture of mass inflow and outflow in neutron star low-mass X-ray binaries, including Fe-K absorption lines by the ultrafast outflow (v/c=0.29).	BH AND NS BINARIES	2	C	MISAKI MIZUMOTO		JAP	2	NOR	CYG X-2: REVEALING ACCRETION AND OUTFLOWING IN THE Z-TRACK SOURCES	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202054010/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
37	202055010	MR2251-178	343.52431	-17.58223	342.85788	-17.84877	338.06088	-9.76485	46.19688	-61.3255	245.63524	60997.48685	2025-11-18 11:41:04	61002.03407	2025-11-23 00:49:04	230.331	200.000	230.331	201.597	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	215.637	201.597	0.000	0.000	11110	313430	11310	PROCESSED	2025-11-28 10:40:08	2026-12-03 00:00:00	2025-11-29 10:40:08	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000021275	The wind-driven feedback process by the ultra-fast outflows (UFOs) is believed to be key in the co-evolution of black holes and galaxies, transferring all their energy or momentum to the galactic outflows. However, the XRISM observation of the archetypal UFO source PDS 456 revealed the UFO's clumpy nature and its extremely large kinetic power, challenging simple feedback models. To reveal the true picture of the wind-driven feedback process, we propose a 200 ks observation of MR 2251-178, the brightest source showing both a UFO and a galactic outflow. Using Resolve's high resolution and Xtend's wide-band capabilities, we can detect the clumpy UFO feature and a broad UFO emission, allowing us to estimate the UFO's kinetic power and compare the UFO properties at different accretion rates.	NON-JET-DOMINATED AGN	2	A	KOUICHI HAGINO		JAP	2	NOR	REVEALING THE WIND-DRIVEN FEEDBACK PROCESS IN THE MODERATELY ACCRETING BLACK HOLE	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202055010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
38	202023010	GRS1915+105	288.79897	10.94603	288.20906	10.85766	292.15032	32.95104	45.36635	-0.21971	242.2429	60993.58894	2025-11-14 14:08:04	60997.48685	2025-11-18 11:41:04	166.550	150.000	166.550	146.288	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	156.477	146.288	0.000	0.000	11110	313430	11310	PROCESSED	2025-12-02 22:29:32	2026-12-06 00:00:00	2025-12-03 22:29:32	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022141	GRS 1915+105 is the stellar-mass black hole that bridges multi-wavelength phenomena observed at opposite ends of the mass scale. In addition to a highly obscured continuum and strong lines from both common and rare elements, the Resolve spectrum obtained in Cycle 1 may contain direct evidence of an extended, highly magnetized corona [priv. comm.]. If the features are not associated with a magnetic corona, they are part of a clumpy v/c = 0.33-0.36 outflow similar to that seen in SS 433. We request a 150 ks exposure in Cycle 2 in order to make a clear, 5-sigma determination of which interpretation is correct. This exposure time will also deliver abundance constraints for rare elements such as Cr and Mn that can be compared to supernova models to understand the progenitor event.	BH AND NS BINARIES	2	A	JON MILLER		USA	2	NOR	REVEALING A MAGNETIC CORONA IN THE BLACK HOLE GRS 1915+105	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202023010/	WINDOW2	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
39	202085010	CYG_X-3	308.1077	40.95778	307.65708	40.78685	328.6034	56.90655	79.84563	0.6999	247.2566	60991.29935	2025-11-12 07:11:04	60993.58894	2025-11-14 14:08:04	97.892	80.000	97.892	90.368	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	96.662	90.368	0.000	0.000	11110	313430	11310	PROCESSED	2025-11-18 10:28:11	2026-11-27 00:00:00	2025-11-19 10:28:11	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000023002	Cyg X-3 is a high-mass X-ray binary composed of a compact object and a Wolf-Rayet star, notable for wind-fed mass accretion. The PV observation of Cyg X-3 in the ultrasoft state provided us data of astonishing quality, raising strong expectations for XRISM observations in the hard state, whose X-ray spectrum is characterized by a hard continuum with a prominent Fe K alpha line at 6.4 keV. We propose an 80 ks observation of the hard state to (1) to probe the geometry and kinematics of matter around the accretion flow using the Fe K alpha line and (2) to estimate the mass transfer rate using various absorption lines. A comparative study of the mass transfer rate in the two different states is expected to provide insight into the yet unresolved mechanism behind state transitions.	BH AND NS BINARIES	2	A	DAIKI MIURA	MICHAEL MCCOLLOUGH	JUS	2	NOR-TOO	PROBING THE NATURE OF ACCRETION IN THE HARD STATE OF CYGNUS X-3	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202085010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
40	202032010	ETA_CARINAE	161.26408	-59.68551	160.77755	-59.42218	202.15592	-58.92846	287.59698	-0.63063	80.0018	60988.36949	2025-11-09 08:52:04	60991.29935	2025-11-12 07:11:04	126.085	100.000	126.085	113.795	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		113.795	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-11-18 10:21:03	2026-11-20 00:00:00	2025-11-19 10:21:04	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022154	We propose to observe the luminous colliding wind binary Eta Carinae at the start and end of XRISM AO2. This interval is important since periastron passage of the binary is late summer 2025 and during AO2 the X-ray spectrum changes rapidly. XRISM/Resolve spectra are needed to determine how the dynamics of the X-ray emitting region of the colliding wind shock change with increasing stellar separation and changing shock orientation.	STELLAR CORONAE, WINDS, AND YOUNG STARS	2	A	MICHAEL CORCORAN		USA	2	NOR	ETA CAR: SHOCK DYNAMICS AFTER PERIASTRON PASSAGE	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202032010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
41	202063010	SIGMA_GEM	115.82683	28.88398	115.04722	29.00354	112.62545	7.45076	191.18856	23.27364	100.00138	60985.92991	2025-11-06 22:19:04	60988.36949	2025-11-09 08:52:04	109.076	100.000	109.076	112.880	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		112.880	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-11-14 08:15:51	2026-11-15 00:00:00	2025-11-15 08:15:52	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000021386	Nano/micro flare heating is a promising explanation for the solar/stellar coronal heating problem. The low-ionized Fe Ka line at 6.4 keV can be a tracer of stellar nano/micro flares. High-energy-resolution spectroscopy is necessary to determine the intensity and photoionization state of the Fe Ka line accurately. The ionization parameter of the Fe Ka line depends on the flare energy scale. We propose a 100 ks Resolve observation of the RS CVn-type star Sigma Gem to reproduce the flare frequency distribution of stellar nano/micro flares and investigate whether the temperature of the Sigma Gem corona can be explained by the sum of the energies of them. We also use Xtend to determine the temperature of the quiescent corona of Sigma Gem during the Resolve observation.	STELLAR CORONAE, WINDS, AND YOUNG STARS	2	B	SHUN INOUE		JAP	2	NOR	STELLAR CORONAL HEATING PROBLEM STUDIED BY OBSERVATIONS OF THE FE KA LINE OF THE RS CVN-TYPE STAR SIGMA GEM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202063010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
42	202068010	MCG-5-23-16	146.91697	-30.94854	146.36776	-30.71597	162.6179	-41.15111	262.7437	17.23381	95.90126	60981.88616	2025-11-02 21:16:04	60985.92991	2025-11-06 22:19:04	190.196	160.000	190.196	171.734	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	183.695	171.734	0.000	0.000	11110	313430	11310	PROCESSED	2025-11-11 09:02:14	2026-11-13 00:00:00	2025-11-12 09:02:15	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000021404	MCG-5-23-16 is one of the brightest AGNs exhibiting a relativistic iron line. Unlike MCG-6-30-15, a highly significant feature of ultrafast outflow (UFO) has been reported, offering a valuable opportunity to study both the accretion disk and associated UFO. We propose a 160-ks XRISM observation of MCG-5-23-16 to resolve the Fe-K band complex, enabling a robust measurement of the inner radius. By measuring the UFO velocity (~0.1c), we will assess whether the inner radius is smaller than the launching radius of the UFO. For the first time XRISM will detect short-timescale (~20 ks) UFO variability, constraining the clumpy nature of the UFO in the sub-Eddington AGN.	NON-JET-DOMINATED AGN	2	B	SATOSHI YAMADA		JAP	2	NOR	THE LINK BETWEEN RELATIVISTIC DISK AND ULTRAFAST WIND IN MCG-5-23-16	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202068010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
43	202040010	ABELL2256_P2	255.79095	78.66095	256.50193	78.72757	102.64344	77.2623	111.04603	31.78351	229.98531	60978.58269	2025-10-30 13:59:04	60981.88616	2025-11-02 21:16:04	187.509	140.000	187.509	173.164	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		173.164	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-11-07 11:58:51	2026-11-13 00:00:00	2025-11-08 11:58:51	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022190	XRISM PV results on merging galaxy clusters show low velocity dispersion, at the lower end of cosmological simulation predictions. This raises questions on turbulence development timescales, implemented physics in the simulations, and whether the PV sample favors more relaxed clusters. To address this, we propose three Resolve pointings (510 ks total) of A2256 - a complex merger with disturbed X-ray morphology and striking radio structures. We will map gas kinematics and, supported by simulations of the A2256 analog, interpret its complexity, reconstruct merger geometry and energy partition. Correlating peculiar radio emission variations with gas motions will test cosmic ray re-acceleration models. We will constrain the velocity power spectrum, building on the first such attempt in Coma.	GROUPS AND CLUSTERS OF GALAXIES	2	B	IRINA ZHURAVLEVA		USA	2	NOR	ICM TURBULENCE IN THE MERGING CHAOS OF ABELL 2256	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202040010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
44	202039010	ABELL2256_P1	256.06685	78.63996	256.77676	78.70528	102.46376	77.30502	111.00004	31.74038	229.98506	60975.25769	2025-10-27 06:11:04	60978.58269	2025-10-30 13:59:04	181.636	150.000	181.636	167.797	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		167.797	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-11-07 11:57:44	2026-11-13 00:00:00	2025-11-08 11:57:45	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000022190	XRISM PV results on merging galaxy clusters show low velocity dispersion, at the lower end of cosmological simulation predictions. This raises questions on turbulence development timescales, implemented physics in the simulations, and whether the PV sample favors more relaxed clusters. To address this, we propose three Resolve pointings (510 ks total) of A2256 - a complex merger with disturbed X-ray morphology and striking radio structures. We will map gas kinematics and, supported by simulations of the A2256 analog, interpret its complexity, reconstruct merger geometry and energy partition. Correlating peculiar radio emission variations with gas motions will test cosmic ray re-acceleration models. We will constrain the velocity power spectrum, building on the first such attempt in Coma.	GROUPS AND CLUSTERS OF GALAXIES	2	B	IRINA ZHURAVLEVA		USA	2	NOR	ICM TURBULENCE IN THE MERGING CHAOS OF ABELL 2256	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202039010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
45	202074010	NGC7172	330.50722	-31.87049	329.7799	-32.11199	321.23337	-18.54945	15.1276	-53.06534	247.99433	60969.72991	2025-10-21 17:31:04	60975.25769	2025-10-27 06:11:04	215.347	180.000	215.347	186.177	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		186.177	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-11-03 13:23:17	2026-11-04 00:00:00	2025-11-04 13:23:18	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000021424	We propose to observe NGC 7172, the best-studied new type AGN (low scattering-fraction AGN) showing the brightest Fe K line, to unveil the nuclear structure. New type AGNs were recognized in 2007 as a putative population of deeply buried supermassive black holes. Despite their importance to understand the process of galaxy-black hole coevolution, their nature still remains unsolved. ALMA observations suggest that NGC 7172 is in the AGN feedback phase, where dense outflow in the innermost region of the torus obscures the nucleus. With XRISM we will measure the width and blue shifts of the Fe-K line with unprecedented accuracies. This is a crucial step to confirm the scenario that new type AGNs are in the outflow-dominant phase in a late stage of an AGN event.	NON-JET-DOMINATED AGN	2	B	YOSHIHIRO UEDA		JAP	2	NOR	UNVEILING NATURE OF NEW TYPE AGN: NGC 7172	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202074010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
46	202057010	IRAS_09104+4109	138.43887	40.94227	137.63622	41.14925	128.11523	23.69624	181.00472	43.62637	109.99985	60963.60491	2025-10-15 14:31:04	60969.72991	2025-10-21 17:31:04	281.189	250.000	281.189	256.930	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		256.930	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-25 16:32:09	2026-11-04 00:00:00	2025-10-26 16:32:10	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000021308	We propose a 250 ks XRISM observation of IRAS 09104+4109 one of two massive cool-core clusters hosting a type 2 QSO in the center. XRISM observations of H1821+643 underlying a quasar in Cycle 1 discovered a high-level turbulent motion of ~300km/s in its cool core. This discovery may indicate that quasar-mode feedback provides sufficient energy to drive turbulent motions of the ICM owing to its strong radiation power including ultra fast outflows (UFOs). This new hypothesis may be the first indication of resolving the cooling-flow problem with XRISM. Observing this target with XRISM is crucial for investigating this new hypothesis, i.e., not only measuring the turbulent motions but also exploring the presence of UFOs. This observation will establish a new face of quasar-mode feedback.	GROUPS AND CLUSTERS OF GALAXIES	2	B	SHUTARO UEDA		JAP	2	NOR	EXPLORING A NEW FACE OF QUASAR-MODE FEEDBACK WITH A COOL-CORE CLUSTER HOSTING AN X-RAY LUMINOUS, HEAVILY OBSCURED QUASAR	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202057010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
47	202072010	ABELL3667_CEN_N	303.10689	-56.80622	302.10655	-56.95627	291.64284	-35.82796	340.89233	-33.38079	249.99686	60961.53616	2025-10-13 12:52:04	60963.60491	2025-10-15 14:31:04	97.613	80.000	97.613	78.240	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		78.240	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-23 09:36:51	2026-10-28 00:00:00	2025-10-24 09:36:51	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000021413	XRISM AO1 observations of Abell 3667 revealed a bulk velocity difference across the cold front (CF), indicating the presence of shear flows. The sharpness and longevity of the CF suggest suppression of Kelvin Helmholtz instability, likely due to magnetic tension. To investigate this, we propose XRISM/Resolve follow-up observations targeting two key regions. A 200 ks exposure at the CF outer edge (CF_OUT) aims to measure the shear velocity, enabling a more accurate estimate of the magnetic field strength that stabilizes the CF. A complementary 80 ks observation of the downstream region (Cen_N) will map bulk velocities and turbulent broadening associated with nonlinear KHI development, targeting the same precision in four subregions across the 500 kpc-scale vortex.	GROUPS AND CLUSTERS OF GALAXIES	2	B	YUKI OMIYA		JAP	2	NOR	CONSTRAINING INTRACLUSTER MICROPHYSICS VIA SHEAR AND TURBULENCE IN ABELL 3667	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202072010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
48	102010010	RX_J1856.5-3754	284.15184	-37.91104	283.30018	-37.97711	281.52144	-15.03607	358.59877	-17.21813	269.99713	60960.40630	2025-10-12 09:45:04	60961.53616	2025-10-13 12:52:04	0.000	40.000	0.000	52.030	PX_NORMAL	N	Y	N	N	N	N	Y	DIM	OFF	OFF	OFF	1	300000A0		52.030	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-21 09:23:40	2023-09-06 00:00:00	2025-10-22 09:23:40	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	2	CAL	AO2 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102010010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
49	102006012	1E0102.2-7219	16.00923	-72.03068	15.60429	-72.29865	314.63825	-65.03604	301.55672	-45.06391	181.00528	60959.97782	2025-10-11 23:28:04	60960.40630	2025-10-12 09:45:04	0.000	30.000	0.000	11.678	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	MEDIUM	OFF	2	31100010	320000A0	12.492	11.678	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-22 08:07:59	2023-09-06 00:00:00	2025-10-23 08:07:59	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	ERIC MILLER		CAL	2	CAL	AO2 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102006012/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
50	102006011	1E0102.2-7219	16.00983	-72.03101	15.60491	-72.29898	314.63773	-65.03635	301.55649	-45.06357	181.00511	60959.72470	2025-10-11 17:23:34	60959.97782	2025-10-11 23:28:04	0.000	30.000	0.000	11.754	PX_NORMAL	N	Y	N	N	N	N	Y	MEDIUM	OFF	OFF	OFF	2	31100010	320000A0	12.573	11.754	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-22 07:52:50	2023-09-06 00:00:00	2025-10-23 07:52:50	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	ERIC MILLER		CAL	2	CAL	AO2 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102006011/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
51	102006010	1E0102.2-7219	16.01022	-72.031	15.6053	-72.29897	314.63788	-65.03646	301.55632	-45.06357	181.00499	60959.44102	2025-10-11 10:35:04	60959.72470	2025-10-11 17:23:34	0.000	30.000	0.000	11.869	PX_NORMAL	N	Y	N	N	N	N	Y	MEDIUM	OFF	OFF	OFF	2	31100010	320000A0	12.696	11.869	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-17 06:50:52	2023-09-06 00:00:00	2025-10-18 06:50:53	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	2	CAL	AO2 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102006010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
52	102005010	1E0102.2-7219	16.00933	-72.03078	15.60439	-72.29875	314.63808	-65.03611	301.55669	-45.06381	180.98873	60958.49032	2025-10-10 11:46:04	60959.44102	2025-10-11 10:35:04	0.000	30.000	0.000	35.291	PX_NORMAL	N	Y	N	N	N	N	Y	DIM	OFF	OFF	OFF	1	300000A0		35.291	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-17 07:46:06	2023-09-06 00:00:00	2025-10-18 07:46:06	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	2	CAL	AO2 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102005010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
53	102009010	Cygnus_Loop	312.8995	32.06407	312.38655	31.87549	328.14763	47.22296	75.16211	-7.78763	267.99927	60957.60352	2025-10-09 14:29:04	60958.49032	2025-10-10 11:46:04	0.000	30.000	0.000	37.877	PX_NORMAL	N	Y	N	N	N	N	Y	MEDIUM	OFF	OFF	OFF	1	300000A0		37.877	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-17 05:48:34	2023-09-06 00:00:00	2025-10-18 05:48:35	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	2	CAL	AO2 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102009010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
54	102003010	Crab_SWoffset	83.61791	22.00194	82.86572	21.96918	84.08289	-1.30636	184.56054	-5.80296	90.00139	60957.19380	2025-10-09 04:39:04	60957.60352	2025-10-09 14:29:04	14.344	8.000	14.344	0.176	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		11.516	0.000	0.176	0.000	11110	313430	11310	PROCESSED	2025-10-17 04:28:17	2023-09-06 00:00:00	2025-10-18 04:28:17	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	2	CAL	AO2 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102003010/	WINDOW1BURST		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
55	102002010	Crab_SEoffset	83.64509	22.00166	82.8929	21.96903	84.10806	-1.30775	184.57435	-5.78183	90.00052	60956.92921	2025-10-08 22:18:04	60957.19380	2025-10-09 04:39:04	10.673	8.000	10.673	0.153	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		10.010	0.000	0.153	0.000	11110	313430	11310	PROCESSED	2025-10-17 04:04:07	2023-09-06 00:00:00	2025-10-18 04:04:08	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	2	CAL	AO2 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102002010/	WINDOW1BURST		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
56	102001010	Crab_NWoffset	83.61783	22.02709	82.8655	21.99434	84.08393	-1.28123	184.53915	-5.78956	90.00108	60956.73130	2025-10-08 17:33:04	60956.92921	2025-10-08 22:18:04	9.461	8.000	9.461	0.155	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		10.127	0.000	0.155	0.000	11110	313430	11310	PROCESSED	2025-10-16 05:11:55	2023-09-06 00:00:00	2025-10-17 05:11:55	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	2	CAL	AO2 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102001010/	WINDOW1BURST		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
57	102000010	Crab_NEoffset	83.64526	22.02741	82.89292	21.99478	84.10935	-1.28204	184.55257	-5.76792	90.00153	60956.37019	2025-10-08 08:53:04	60956.73130	2025-10-08 17:33:04	10.862	8.000	10.862	0.199	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		13.019	0.000	0.199	0.000	11110	313430	11310	PROCESSED	2025-10-16 05:17:01	2023-09-06 00:00:00	2025-10-17 05:17:02	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000028001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	2	CAL	AO2 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/102000010/	WINDOW1BURST		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
58	201082010	V1223_SAGITTARII	283.75961	-31.16371	282.95481	-31.22804	281.86898	-8.2896	4.95789	-14.35497	264.60776	60952.03824	2025-10-04 00:55:04	60956.37019	2025-10-08 08:53:04	236.533	192.000	236.533	203.568	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	217.746	203.568	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-15 09:45:21	2026-10-23 00:00:00	2025-10-16 09:45:21	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000012097	We propose a model-independent mass and radius measurement of a magnetic White Dwarf (WD) by assessing its surface rotational velocity. This will be achieved with the Doppler shift of the 6.4 keV lines emitted from the WD surface. Subsequently, the WD mass will be calculated using the measured radius and the previously determined plasma maximum temperature. Our target is the magnetic cataclysmic variable V1223 Sgr, a former candidate for the PV target, as all necessary parameters have already been measured. This measurement aims to differentiate between the mass-radius relation of strongly-magnetic WDs and the standard relation. To achieve this, we estimate that a total exposure time of 192 ks is required, spread across all one-eighth WD spin phases each of which we will analyze.	ACCRETING WHITE DWARFS AND NOVAE	2	C	TAKAYUKI HAYASHI		USA	1	NOR	MODEL-INDEPENDENT MASS AND RADIUS MEASUREMENT OF A MAGNETIC WHITE DWARF	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201082010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
59	201119010	IC443	94.19906	22.54984	93.44309	22.56839	93.87792	-0.83294	189.02576	2.92892	90.00005	60946.90421	2025-09-28 21:42:04	60952.03824	2025-10-04 00:55:04	219.796	200.000	219.796	209.118	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		209.118	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-15 15:48:12	2026-10-24 00:00:00	2025-10-16 15:48:12	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000014033	The Galactic supernova remnant (SNR) IC 443 is an ideal target to study shock-cloud interaction: its evolution within a complex environment forges its peculiar X-ray emission, providing a unique clue to understand the feedback of SNRs on molecular clouds. We propose a 200 ks XRISM observation of IC 443. The Resolve pointing will focus on a region characterized by bright gamma-ray emission, where the shock impacts on a dense molecular clump. Such pointing will allow us to study the physical origin of the plasma overionization and its association with thermal conduction with the cold clump. Extend will provide a map of the hard X-ray emission of IC 443, allowing us to study both the ejecta emission and the Fe K neutral line associated with cosmic rays diffusing in the nearby clouds.	SUPERNOVA REMNANTS	2	C	MARCO MICELI		EUR	1	NOR	A THOROUGH STUDY OF THE SUPERNOVA REMNANT IC443: PROBING PLASMA CONDITIONS AND COSMIC RAY DIFFUSION IN SHOCK-CLOUD INTER	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201119010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
60	001012010	N132D	81.2564	-69.64195	81.35851	-69.68406	312.62421	-85.52108	280.30459	-32.78538	81.07023	60943.01463	2025-09-25 00:21:04	60946.90421	2025-09-28 21:42:04	174.492	160.000	174.492	155.023	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		155.023	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-15 12:35:41	2025-11-07 00:00:00	2025-10-16 12:35:41	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000010002	The XRISM project will conduct observations of specific targets following the gatevalve open operations to verify the instruments' condition.	SPECIAL OBSERVATIONS	0	A	XRISM Collaboration		JAP	1	NOR	PROJECT-DRIVEN OBSERVATIONS AFTER THE GATEVALVE OPERATIONS (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/001012010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
61	001011010	ETA_CARINAE	161.26515	-59.68505	160.77861	-59.42171	202.15598	-58.92775	287.59724	-0.62997	23.28638	60941.88755	2025-09-23 21:18:04	60943.01463	2025-09-25 00:21:04	45.933	40.000	45.933	39.390	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		39.390	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-15 08:24:10	2025-11-07 00:00:00	2025-10-16 08:24:10	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000010002	The XRISM project will conduct observations of specific targets following the gatevalve open operations to verify the instruments' condition.	SPECIAL OBSERVATIONS	0	A	XRISM Collaboration		JAP	1	NOR	PROJECT-DRIVEN OBSERVATIONS AFTER THE GATEVALVE OPERATIONS (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/001011010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
62	001010010	PSI_ORIONIS_CLUSTER	81.24898	1.7002	80.60034	1.65628	80.59597	-21.45387	201.12439	-18.30679	88.70221	60933.95421	2025-09-15 22:54:04	60941.88755	2025-09-23 21:18:04	9.079	280.000	9.079	356.962	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		356.962	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-15 15:43:04	2025-11-07 00:00:00	2025-10-16 15:43:05	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000010888	A warm-and- and/or cool-and-vibration operation will be carried out to open the gate valve. A preparatory observation and actual vibrating trials are scheduled in September, 2025. In the event of a successful opening, commissioning and calibration observations will be conducted.	SPECIAL OPERATIONS	0	A	XRISM Collaboration		JAP	1		GATEVALVE OPEN OPERATION 4 AND ASSOCIATED OBSERVATIONS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/001010010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
63	001009010	RESOLVE_THERM8_S	66.052	-59.05212	65.83642	-59.16566	23.33692	-76.85951	269.46237	-41.70373	103.60192	60932.96255	2025-09-14 23:06:04	60933.95421	2025-09-15 22:54:04	1.250	40.000	1.250	71.877	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		71.877	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-23 07:58:37	2025-11-07 00:00:00	2025-09-24 07:58:37	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000010888	A warm-and- and/or cool-and-vibration operation will be carried out to open the gate valve. A preparatory observation and actual vibrating trials are scheduled in September, 2025. In the event of a successful opening, commissioning and calibration observations will be conducted.	SPECIAL OPERATIONS	0	A	XRISM Collaboration		JAP	1		GATEVALVE OPEN OPERATION 4 AND ASSOCIATED OBSERVATIONS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/001009010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
64	001008010	RESOLVE_THERM7_S	72.45889	-59.03149	72.26124	-59.1159	35.12067	-79.07031	268.37492	-38.51576	97.0304	60931.96949	2025-09-13 23:16:04	60932.96255	2025-09-14 23:06:04	1.250	40.000	1.250	71.891	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		71.891	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-20 09:24:39	2025-11-07 00:00:00	2025-09-21 09:24:40	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000010888	A warm-and- and/or cool-and-vibration operation will be carried out to open the gate valve. A preparatory observation and actual vibrating trials are scheduled in September, 2025. In the event of a successful opening, commissioning and calibration observations will be conducted.	SPECIAL OPERATIONS	0	A	XRISM Collaboration		JAP	1		GATEVALVE OPEN OPERATION 4 AND ASSOCIATED OBSERVATIONS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/001008010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
65	001007010	RESOLVE_THERM6_S	78.41829	-59.02653	78.23253	-59.0829	49.62348	-80.82242	267.80542	-35.48395	90.93198	60930.97644	2025-09-12 23:26:04	60931.96949	2025-09-13 23:16:04	1.250	40.000	1.250	71.326	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		71.326	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-20 09:09:31	2025-11-07 00:00:00	2025-09-21 09:09:32	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000010888	A warm-and- and/or cool-and-vibration operation will be carried out to open the gate valve. A preparatory observation and actual vibrating trials are scheduled in September, 2025. In the event of a successful opening, commissioning and calibration observations will be conducted.	SPECIAL OPERATIONS	0	A	XRISM Collaboration		JAP	1		GATEVALVE OPEN OPERATION 4 AND ASSOCIATED OBSERVATIONS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/001007010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
66	001006010	RESOLVE_THERM5_S	84.81673	-59.00842	84.63802	-59.03403	70.24095	-82.09097	267.58261	-32.19659	84.49269	60929.98338	2025-09-11 23:36:04	60930.97644	2025-09-12 23:26:04	1.251	40.000	1.251	71.305	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		71.305	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-18 07:18:54	2025-11-07 00:00:00	2025-09-19 07:18:54	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000010888	A warm-and- and/or cool-and-vibration operation will be carried out to open the gate valve. A preparatory observation and actual vibrating trials are scheduled in September, 2025. In the event of a successful opening, commissioning and calibration observations will be conducted.	SPECIAL OPERATIONS	0	A	XRISM Collaboration		JAP	1		GATEVALVE OPEN OPERATION 4 AND ASSOCIATED OBSERVATIONS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/001006010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
67	001005010	RESOLVE_THERM4_S	91.20118	-58.99697	91.02385	-58.99158	94.69323	-82.41669	267.74209	-28.91271	78.09174	60929.05907	2025-09-11 01:25:04	60929.98338	2025-09-11 23:36:04	1.241	40.000	1.241	66.634	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		66.634	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-18 06:56:45	2025-11-07 00:00:00	2025-09-19 06:56:45	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000010888	A warm-and- and/or cool-and-vibration operation will be carried out to open the gate valve. A preparatory observation and actual vibrating trials are scheduled in September, 2025. In the event of a successful opening, commissioning and calibration observations will be conducted.	SPECIAL OPERATIONS	0	A	XRISM Collaboration		JAP	1		GATEVALVE OPEN OPERATION 4 AND ASSOCIATED OBSERVATIONS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/001005010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
68	001004010	RESOLVE_THERM3_S	97.59413	-58.97865	97.41231	-58.94231	118.0542	-81.67349	268.23202	-25.64904	71.62878	60928.06324	2025-09-10 01:31:04	60929.05907	2025-09-11 01:25:04	1.250	40.000	1.250	71.409	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		71.409	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-17 08:06:46	2025-11-07 00:00:00	2025-09-18 08:06:46	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000010888	A warm-and- and/or cool-and-vibration operation will be carried out to open the gate valve. A preparatory observation and actual vibrating trials are scheduled in September, 2025. In the event of a successful opening, commissioning and calibration observations will be conducted.	SPECIAL OPERATIONS	0	A	XRISM Collaboration		JAP	1		GATEVALVE OPEN OPERATION 4 AND ASSOCIATED OBSERVATIONS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/001004010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
69	001003010	RESOLVE_THERM2_S	104.10572	-58.98285	103.9139	-58.91545	136.87587	-80.09229	269.07284	-22.38385	64.92718	60927.07019	2025-09-09 01:41:04	60928.06324	2025-09-10 01:31:04	1.250	40.000	1.250	71.865	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		71.865	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-17 07:55:38	2025-11-07 00:00:00	2025-09-18 07:55:39	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000010888	A warm-and- and/or cool-and-vibration operation will be carried out to open the gate valve. A preparatory observation and actual vibrating trials are scheduled in September, 2025. In the event of a successful opening, commissioning and calibration observations will be conducted.	SPECIAL OPERATIONS	0	A	XRISM Collaboration		JAP	1		GATEVALVE OPEN OPERATION 4 AND ASSOCIATED OBSERVATIONS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/001003010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
70	001002010	RESOLVE_THERM1_S	110.16513	-58.93591	109.95796	-58.8404	149.7666	-78.11888	270.06956	-19.40203	58.50554	60926.07713	2025-09-08 01:51:04	60927.07019	2025-09-09 01:41:04	1.250	40.000	1.250	71.433	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		71.433	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-15 10:25:45	2025-11-07 00:00:00	2025-09-16 10:25:45	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000010888	A warm-and- and/or cool-and-vibration operation will be carried out to open the gate valve. A preparatory observation and actual vibrating trials are scheduled in September, 2025. In the event of a successful opening, commissioning and calibration observations will be conducted.	SPECIAL OPERATIONS	0	A	XRISM Collaboration		JAP	1		GATEVALVE OPEN OPERATION 4 AND ASSOCIATED OBSERVATIONS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/001002010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
71	001001010	ETA_CARINAE	161.26422	-59.68482	160.77769	-59.42148	202.15504	-58.92794	287.59672	-0.62998	0.00874	60918.75977	2025-08-31 18:14:04	60926.07713	2025-09-08 01:51:04	469.023	300.000	469.023	385.574	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		385.574	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-15 18:01:29	2025-11-07 00:00:00	2025-09-16 18:01:31	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000010888	A warm-and- and/or cool-and-vibration operation will be carried out to open the gate valve. A preparatory observation and actual vibrating trials are scheduled in September, 2025. In the event of a successful opening, commissioning and calibration observations will be conducted.	SPECIAL OPERATIONS	0	A	XRISM Collaboration		JAP	1		GATEVALVE OPEN OPERATION 4 AND ASSOCIATED OBSERVATIONS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/001001010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
72	201001010	GX13+1	273.62872	-17.15745	272.9021	-17.17331	273.48771	6.23792	13.51525	0.10864	271.38536	60917.54241	2025-08-30 13:01:04	60918.75977	2025-08-31 18:14:04	51.083	30.000	51.083	5.955	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	47.539	0.000	0.000	5.955	11110	313430	11310	PROCESSED	2025-09-06 11:35:37	2026-09-10 00:00:00	2025-09-07 11:35:37	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011055	GX13+1 is a low magnetic field neutron star accreting mass via a disk from its companion star. It reliably shows blueshifted absorption features, so it was chosen as an XRISM PV target to study accretion disk wind launching mechanisms. The PV observation caught the system in an unusual state, with much stronger absorption than predicted. This GO1 request is for a repeat 30ks observation of GX13+1, to compare the spectacular PV data with more normal wind absorption in this source.	BH AND NS BINARIES	2	C	RYOTA TOMARU		JAP	1	NOR	THE NORMAL ACCRETION DISK WIND IN GX13+1	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201001010/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
73	201062010	G344.7-0.1	255.95821	-41.71689	255.0774	-41.64725	258.9695	-18.81379	344.66569	-0.16375	269.99717	60914.75769	2025-08-27 18:11:04	60917.54241	2025-08-30 13:01:04	121.753	100.000	121.753	108.405	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		108.405	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-04 17:07:06	2026-09-12 00:00:00	2025-09-05 17:07:09	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011333	Although Type Ia SNe have attracted a great deal of interest, the explosion mechanism is still controversial. So far, two possible scenarios have been put forward: explosion of a white dwarf close to the Chandrasekhar limit (near-Ch) or smaller than the limit (sub-Ch). According to the latest theories, abudances and velocity structures significantly differ between the near-/sub-Ch models. Here we propose a XRISM observation of G344.7-0.1, which is one of the brightest Type Ia SNR. While previous studies suggest detections of Cr and Mn, the measurement is still uncertain and better precision measurements are required. This observation will reveal abundances of rare elements and their velocity structures, both of which are critical to elucidate the explosion mechanism of Type Ia SNe.	SUPERNOVA REMNANTS	2	C	MOE ANAZAWA		JAP	1	NOR	UNVEILING EXPLOSION MECHANISM OF TYPE IA SNR G344.7-0.1 BY MEASURING RARE ELEMENTS AND VELOCITY STRUCTURES WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201062010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
74	201038010	ETA_CARINAE	161.26375	-59.68496	160.77722	-59.42162	202.15491	-58.92821	287.59657	-0.63022	0.01118	60912.60560	2025-08-25 14:32:04	60914.75769	2025-08-27 18:11:04	144.608	80.000	144.608	115.973	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		115.973	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-04 14:54:19	2026-09-06 00:00:00	2025-09-05 14:54:19	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011206	Mass-loss is widely recognized as a key parameter to understand a stellar chemical evolution following supernova. However, a mass loss rate of Luminous Blue Variables (LBVs) are very difficult to measure due to their dense wind and understood only with digit precision of 10^-3 Mo / yr. In order to improve this accuracy, we propose to observe Eta Carinae at around the periastron passage. Eta Carinae is a long period binary of a primary LBV star and a secondary WR or O star with 5.5 yr period. During the periastron passage, the X-ray plasma heated by wind-wind collision becomes compact, the X-rays from which pierces the LBV wind with narrow beam size. Using the Fe-K absorption edge, the narrow beam enables promising us to pursue to measure the mass-loss rate of the LBV.	STELLAR CORONAE, WINDS, AND YOUNG STARS	2	A	YOSHITOMO MAEDA		JAP	1	NOR	XRISM PIERCING THE DENSE STELLAR WIND OF LUMINOUS BLUE VARIABLE IN ETA CARINAE	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201038010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
75	201029010	SAGITTARIUS_A_N2	266.32737	-28.96792	265.53293	-28.94816	266.77211	-5.56977	359.9375	0.04141	269.99711	60911.26324	2025-08-24 06:19:04	60912.60560	2025-08-25 14:32:04	58.639	50.000	58.639	56.876	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		56.876	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-04 12:56:33	2026-09-06 00:00:00	2025-09-05 12:56:34	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011149	The objective of the observation is to get the direct evidence of the past outflow of Sgr A. The key information is the bulk motions of the plasmas of not only the Sgr A bipolar but also the Galactic Center X-ray emission, which may have been created or affected by the Sgr A outflow. We propose to observe four regions (region N1,N2, S1, S2), which cover the Sgr A bipolar, with 50 ks exposure respectively (total 200 ks).	GALACTIC DIFFUSE EMISSION AND SURVEYS	2	B	HIDEKI UCHIYAMA		JAP	1	NOR	DIRECT EVIDENCE FOR A PAST OUTFLOW OF THE GALACTIC NUCLEUS SGR A*	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201029010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
76	201028010	SAGITTARIUS_A_S2	266.47754	-29.04805	265.68256	-29.02902	266.90605	-5.64659	359.93753	-0.11243	269.99714	60909.81324	2025-08-22 19:31:04	60911.26324	2025-08-24 06:19:04	60.452	50.000	60.452	59.428	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		59.428	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-04 12:59:40	2026-09-06 00:00:00	2025-09-05 12:59:41	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011149	The objective of the observation is to get the direct evidence of the past outflow of Sgr A. The key information is the bulk motions of the plasmas of not only the Sgr A bipolar but also the Galactic Center X-ray emission, which may have been created or affected by the Sgr A outflow. We propose to observe four regions (region N1,N2, S1, S2), which cover the Sgr A bipolar, with 50 ks exposure respectively (total 200 ks).	GALACTIC DIFFUSE EMISSION AND SURVEYS	2	B	HIDEKI UCHIYAMA		JAP	1	NOR	DIRECT EVIDENCE FOR A PAST OUTFLOW OF THE GALACTIC NUCLEUS SGR A*	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201028010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
77	201027010	SAGITTARIUS_A_S1	266.47137	-29.00649	265.67665	-28.98742	266.8996	-5.60517	359.97021	-0.08619	269.99748	60908.47991	2025-08-21 11:31:04	60909.81324	2025-08-22 19:31:04	60.632	50.000	60.632	60.030	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		60.030	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-01 08:06:48	2026-09-03 00:00:00	2025-09-02 08:06:48	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011149	The objective of the observation is to get the direct evidence of the past outflow of Sgr A. The key information is the bulk motions of the plasmas of not only the Sgr A bipolar but also the Galactic Center X-ray emission, which may have been created or affected by the Sgr A outflow. We propose to observe four regions (region N1,N2, S1, S2), which cover the Sgr A bipolar, with 50 ks exposure respectively (total 200 ks).	GALACTIC DIFFUSE EMISSION AND SURVEYS	2	B	HIDEKI UCHIYAMA		JAP	1	NOR	DIRECT EVIDENCE FOR A PAST OUTFLOW OF THE GALACTIC NUCLEUS SGR A*	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201027010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
78	201026010	SAGITTARIUS_A_N1	266.37148	-28.98699	265.57691	-28.96744	266.81136	-5.58786	359.94135	-0.00146	269.99813	60907.21532	2025-08-20 05:10:04	60908.47991	2025-08-21 11:31:04	62.867	50.000	62.867	56.079	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		56.079	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-09-01 07:47:38	2026-09-03 00:00:00	2025-09-02 07:47:38	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011149	The objective of the observation is to get the direct evidence of the past outflow of Sgr A. The key information is the bulk motions of the plasmas of not only the Sgr A bipolar but also the Galactic Center X-ray emission, which may have been created or affected by the Sgr A outflow. We propose to observe four regions (region N1,N2, S1, S2), which cover the Sgr A bipolar, with 50 ks exposure respectively (total 200 ks).	GALACTIC DIFFUSE EMISSION AND SURVEYS	2	B	HIDEKI UCHIYAMA		JAP	1	NOR	DIRECT EVIDENCE FOR A PAST OUTFLOW OF THE GALACTIC NUCLEUS SGR A*	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201026010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
79	201111010	V2400_OPH	258.15135	-24.2459	257.38821	-24.18691	259.20708	-1.24944	359.86634	8.73969	274.12526	60902.58963	2025-08-15 14:09:04	60907.21532	2025-08-20 05:10:04	237.744	200.000	237.744	209.635	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	224.235	209.635	0.000	0.000	11110	313430	11310	PROCESSED	2025-08-30 07:49:54	2026-09-03 00:00:00	2025-08-31 07:49:54	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012196	Masses of white dwarfs (WDs) play an important role in understanding their formation and evolution. A unique way to estimate the mass of a WD in an Intermediate Polar (IP) is to estimate the gravitational redshift of emission lines. We propose 200 kilosec XRISM observations to carry out accurate estimation of the gravitational redshift of emission lines in an IP V2400 Oph and use these measurements to accurately estimate the mass of the WD. The proposed XRISM observation would also serve as a benchmark for carrying out similar investigations for several other moderately bright IPs in future cycles and to estimate the mass of the WDs.	ACCRETING WHITE DWARFS AND NOVAE	2	B	NAZMA ISLAM		USA	1	NOR	ESTIMATING THE MASS OF THE WHITE DWARF IN THE INTERMEDIATE POLAR V2400 OPH USING XRISM OBSERVATIONS	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201111010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
80	201121010	IGR_J17062-6143	256.57054	-61.71145	255.42846	-61.64406	261.89824	-38.64933	328.72	-12.39926	257.15685	60900.84449	2025-08-13 20:16:04	60902.58963	2025-08-15 14:09:04	117.195	100.000	117.195	118.062	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	126.285	118.062	0.000	0.000	11110	313430	11310	PROCESSED	2025-08-30 04:48:22	2026-09-04 00:00:00	2025-08-31 04:48:23	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000014039	IGR J17062-6143 habors a neutron star that spins at 163~Hz and is in a 38-min orbit with a hydrogen-deficient companion star. Previous Chandra/HETG and XMM-Newton/RGS observations revealed hints of blue-shifted spectral lines at <2 keV energies that could indicate the presence of an outflowing wind. Since the commonly inferred thermal wind-launch mechanism cannot operate in such a very compact binary, the putative wind may be launched by magnetic processes. XRISM can reveal if a wind is indeed present by now allowing to search for narrow lines from a wind in the 6-7 keV Fe-K band. If confirmed, it would be the first undisputed detection of a magnetic wind in an X-ray binary and would have broad astrophysical implications.	BH AND NS BINARIES	2	C	NATHALIE DEGENAAR		EUR	1	NOR	A MAGNETICALLY-DRIVEN WIND FROM AN ACCRETING MILLISECOND PULSAR?	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201121010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
81	201047010	ELIAS29	246.78995	-24.62203	246.03256	-24.51061	248.9786	-2.86069	353.0109	16.64104	278.05521	60898.33824	2025-08-11 08:07:04	60900.84449	2025-08-13 20:16:04	115.061	100.000	115.061	36.396	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		36.396	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-08-21 11:39:27	2026-08-22 00:00:00	2025-08-22 11:39:27	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011246	Stellar X-ray activity can induce chemical reactions in the protoplanetary disk and affect planet formation. The low-ionized Fe line at ~ 6.4 keV can be a good tracer of the X-ray penetration depth toward the disk, which can reveal the ionization process of surrounding envelope and disk by coronal X-rays. We propose a 100 ks observation of the protostar Elias 29 with Resolve to estimate the X-ray penetration depth and confirm the Fe line is formed from the disk. Using the same pointing, we also use Xtend, which simultaneously observes 9 surrounding pre-main-sequence stars. From this, we can provide the constraint on the line formation region from another viewpoint, by combining the Fe line equivalent widths and the disk inclination angles from the high spatially-resolved ALMA data.	STELLAR CORONAE, WINDS, AND YOUNG STARS	2	A	SHUN INOUE		JAP	1	NOR	DISK IONIZATION AND PLANET FORMATION STUDIED BY OBSERVATIONS OF THE PROTOSTAR ELIAS 29 AND 9 PRE-MAIN-SEQUENCE STARS	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201047010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
82	201044010	IC4329A	207.33117	-30.30939	206.61702	-30.06123	216.35045	-17.77957	317.49716	30.91987	288.0001	60894.95074	2025-08-07 22:49:04	60898.33824	2025-08-11 08:07:04	146.288	130.000	146.288	99.706	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	106.650	99.706	0.000	0.000	11110	313430	11310	PROCESSED	2025-10-08 20:46:22	2026-08-26 00:00:00	2025-08-19 09:04:15	03.03.015.012	gen20241115_xtd20250915_rsl20250915	Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003	000011234	Various structures within AGNs emit Fe K lines. IC 4329A, a prominent Seyfert 1 galaxy in X-rays with minimal absorption in its spectrum, is ideal for studying Fe K emission origins. Line width analysis suggests a radius of about 60 light-days, possibly representing an outer broad line region. We propose using a 130 ks observation with XRISM to constrain the ionization degree of this Fe K reprocessor, enabling the calculation of its number density and a deeper understanding of its properties. Anticipated log ionization parameter falls between 1 and 2, with Fe Kalpha and Kbeta lines exhibiting energy shifts of several eV within this range. XRISM is uniquely equipped to detect this energy shift within a reasonable exposure time.	NON-JET-DOMINATED AGN	2	B	MISAKI MIZUMOTO		JAP	1	NOR	ORIGIN OF THE FE K REPROCESSOR IN SEYFERT 1 GALAXY, IC 4329A	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201044010/	WINDOW2	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
83	201037010	ETA_CARINAE	161.26666	-59.68522	160.7801	-59.42188	202.15723	-58.92732	287.59799	-0.62976	0.00601	60892.33824	2025-08-05 08:07:04	60894.95074	2025-08-07 22:49:04	101.432	80.000	101.432	85.979	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		85.979	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-08-15 13:52:13	2026-08-16 00:00:00	2025-08-16 13:52:14	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011206	Mass-loss is widely recognized as a key parameter to understand a stellar chemical evolution following supernova. However, a mass loss rate of Luminous Blue Variables (LBVs) are very difficult to measure due to their dense wind and understood only with digit precision of 10^-3 Mo / yr. In order to improve this accuracy, we propose to observe Eta Carinae at around the periastron passage. Eta Carinae is a long period binary of a primary LBV star and a secondary WR or O star with 5.5 yr period. During the periastron passage, the X-ray plasma heated by wind-wind collision becomes compact, the X-rays from which pierces the LBV wind with narrow beam size. Using the Fe-K absorption edge, the narrow beam enables promising us to pursue to measure the mass-loss rate of the LBV.	STELLAR CORONAE, WINDS, AND YOUNG STARS	2	A	YOSHITOMO MAEDA		JAP	1	NOR	XRISM PIERCING THE DENSE STELLAR WIND OF LUMINOUS BLUE VARIABLE IN ETA CARINAE	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201037010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
84	201123010	ABELL2142	239.57587	27.23704	239.05874	27.37907	229.18665	46.4587	44.23416	48.69612	318.00176	60889.74241	2025-08-02 17:49:04	60892.33824	2025-08-05 08:07:04	111.817	100.000	111.817	105.876	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		105.876	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-08-09 12:54:01	2026-08-15 00:00:00	2025-08-10 12:54:02	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000014047	We propose to observe the core of Abell 2142 with XRISM for 100 ks to map turbulence and bulk motions with the exquisite spectral resolution of RESOLVE. XRISM will costrain the level of turbulence in the core of the brightest and nearest clusters and it is thus important to map a variety of dynamical states. A2142 stands up for (1) its high flux in the 2-10 keV band, ideal for a gate-valve closed observation; (2) its intermediate state between a relaxed cool core and a violent merger, mirrored by an unusual radio emission; (3) its rich variety of motions suggested by its extreme sloshing and a close pair of BCGs with extreme difference in velocity along the line of sight. Therefore, A2142 is an ideal target for an AO1 XRISM observation.	GROUPS AND CLUSTERS OF GALAXIES	2	C	FABIO GASTALDELLO		EUR	1	NOR	AN ATLAS OF MOTIONS IN A2142 AT HIGH SPECTRAL RESOLUTION WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201123010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
85	201098010	ABELL2163_CENTER	243.93879	-6.14531	243.27146	-6.02155	243.12818	14.89586	6.76383	30.47109	292.00046	60884.27296	2025-07-28 06:33:04	60889.74241	2025-08-02 17:49:04	223.164	200.000	223.164	205.202	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		205.202	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-08-06 11:02:21	2026-08-09 00:00:00	2025-08-07 11:02:22	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012147	Abell 2163 is the hottest, most massive low redshift cluster in the universe. It is actively merging along the line-of-sight, with a Bullet-like cool core driving a turbulence-generating shock front ahead of it that has accelerated one of the most powerful radio halos known--a property known to correlate with higher turbulent velocity dispersion. With a single pointing of the center, we aim to measure turbulent line broadening, velocity offsets, and ion temperatures from the lines in the 6.7 keV and 7 keV Fe complexes with Resolve in two regions: one covering the reheated cool core and the other likely dominated by gas moving in the opposite direction. We will also constrain the larger-scale thermodynamic structure of the cluster with Xtend and NuSTAR.	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	2	B	DANIEL WIK		USA	1	NOR	GAS DYNAMICS IN THE LINE-OF-SIGHT MERGER ABELL 2163 WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201098010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
86	101012010	Perseus_CAL2	49.95005	41.51207	49.12258	41.33144	58.60584	22.33853	150.57521	-13.26116	84.59629	60883.33824	2025-07-27 08:07:04	60884.27296	2025-07-28 06:33:04	44.215	40.000	44.215	40.082	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	42.873	40.082	0.000	0.000	11110	313430	11310	PROCESSED	2025-08-05 07:37:53	2025-08-31 00:00:00	2025-08-06 07:37:54	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101012010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
87	101011010	Perseus_CAL1	49.95015	41.51216	49.12267	41.33153	58.60594	22.3386	150.57521	-13.26104	84.61306	60882.41046	2025-07-26 09:51:04	60883.33824	2025-07-27 08:07:04	40.000	40.000	40.000	43.140	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		43.140	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-08-05 08:01:06	2025-08-31 00:00:00	2025-08-06 08:01:07	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101011010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
88	201080010	Perseus_O3	50.03411	41.38614	49.20722	41.20582	58.63367	22.20009	150.70062	-13.33138	82.8782	60880.42366	2025-07-24 10:10:04	60882.41046	2025-07-26 09:51:04	92.411	90.000	92.411	92.536	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		92.536	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-31 12:09:49	2026-08-07 00:00:00	2025-08-01 12:09:49	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012080	Feedback from Active Galactic Nuclei (AGN) is crucial for regulating cooling and star formation in galaxy clusters. Gas motions driven by the feedback could be important in heating the gas. We propose a multi-pointing observational program for the Perseus cluster, totaling 500 ks. We will study radial and azimuthal variations of gas kinematics and metallicity within the cluster core, mapping a transition between feedback- and mergers-dominated regions, which is crucial for distinguishing various feedback scenarios and revealing the role of turbulence in AGN feedback. We will probe gas sloshing, motions driven by rising bubbles, and turbulence association with the radio mini halo. These observations will be of legacy value, complementing large multi-wavelength data sets on Perseus.	GROUPS AND CLUSTERS OF GALAXIES	2	C	IRINA ZHURAVLEVA		USA	1	NOR	MAPPING GAS KINEMATICS IN THE X-RAY BRIGHTEST GALAXY CLUSTER	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201080010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
89	201078010	Perseus_C3	49.95797	41.47393	49.13072	41.29333	58.60059	22.30024	150.6019	-13.28971	82.87786	60879.26949	2025-07-23 06:28:04	60880.42366	2025-07-24 10:10:04	54.245	50.000	54.245	51.864	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		51.864	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-31 10:48:28	2026-08-07 00:00:00	2025-08-01 10:48:28	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012080	Feedback from Active Galactic Nuclei (AGN) is crucial for regulating cooling and star formation in galaxy clusters. Gas motions driven by the feedback could be important in heating the gas. We propose a multi-pointing observational program for the Perseus cluster, totaling 500 ks. We will study radial and azimuthal variations of gas kinematics and metallicity within the cluster core, mapping a transition between feedback- and mergers-dominated regions, which is crucial for distinguishing various feedback scenarios and revealing the role of turbulence in AGN feedback. We will probe gas sloshing, motions driven by rising bubbles, and turbulence association with the radio mini halo. These observations will be of legacy value, complementing large multi-wavelength data sets on Perseus.	GROUPS AND CLUSTERS OF GALAXIES	2	C	IRINA ZHURAVLEVA		USA	1	NOR	MAPPING GAS KINEMATICS IN THE X-RAY BRIGHTEST GALAXY CLUSTER	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201078010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
90	201097010	G292_NE	171.1991	-59.22487	170.63191	-58.94989	208.09535	-55.02724	292.04023	1.80235	315.0032	60876.45213	2025-07-20 10:51:04	60879.26949	2025-07-23 06:28:04	115.473	100.000	115.473	101.307	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		101.307	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-31 12:14:57	2026-08-07 00:00:00	2025-08-01 12:14:58	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012146	The composition and dynamics of supernova remnants inform us on the explosion mechanism of the supernova and the evolution of the progenitor. The Galactic remnant G292.0+1.8 is an evolved remnant rich in emission from shocked ejecta and circumstellar material. It is also bright in [OIII] emission from shocked, fast moving ejecta which have velocities in excess of 2500 km/s. Here we propose for two 100ks observations of G292 in order to investigate the properties of the explosion and nucleosynthesis. Our proposed program will be complemented by a ground based spectroscopic survey to map the 3D structure of the ejecta in order to further understand the properties of the explosion.	SUPERNOVA REMNANTS	2	C	DANIEL PATNAUDE		USA	1	NOR	THE PROGENITOR AND EXPLOSION PROPERTIES OF G292.0+1.8	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201097010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
91	201042010	ABELL2029	227.73304	5.74453	227.11328	5.93287	223.53039	22.62623	6.47267	50.54594	284.99867	60873.53616	2025-07-17 12:52:04	60876.45213	2025-07-20 10:51:04	118.349	100.000	118.349	104.679	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		104.679	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-26 07:29:29	2026-08-01 00:00:00	2025-07-27 07:29:29	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011220	The core region of A2029 is an excellent laboratory for estimating the Ni abundance because of a relatively hot intracluster medium (ICM) at roughly 6 keV, and constraining the contribution from Type Ia supernovae that are the monopoly manufacturer of Ni. Even though the A2029 center has two XRISM performance verification (PV) datasets, the total exposure is short (only 40 ks) and not enough to provide a strong constraint on the Ni abundance, particularly in the innermost core. Here, we suggest extending the PV observation data by doing a deep 100 ks observation of the A2029 core. This observation will reveal the Type Ia characteristics in A2029 with an accurate estimation of Ni. We will also show how AGN feedback and/or sloshing impact the dynamical evolution of the ICM.	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	2	C	KOTARO FUKUSHIMA		JAP	1	NOR	ESTIMATING THE SN IA ENRICHMENT AND GAS DYNAMICS IN THE CENTRAL REGION OF THE A2029 CLUSTER WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201042010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
92	201085010	30_DORADUS	84.67107	-69.0962	84.75698	-69.12187	305.97399	-86.76614	279.4599	-31.6744	8.0135	60870.71949	2025-07-14 17:16:04	60873.53616	2025-07-17 12:52:04	184.933	100.000	184.933	100.978	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		100.978	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-22 12:50:29	2026-07-23 00:00:00	2025-07-23 12:50:29	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012115	30 Doradus represents the most intense starburst in the Local Group of galaxies and powers the spectacular Tarantula Nebula, although the underlying astrophysics remains poorly understood. We propose an XRISM observation to perform the first X-ray spectroscopic study of the starburst region. We will determine the thermal and dynamical states of the massive stellar cluster wind that shapes the nebula, the X-ray contribution from the charge exchange between hot and cool gases, and the presence of the non-thermal X-ray component and hence the cosmic ray acceleration in the region. This study will help us to understand how the starburst feedback works.	ASTROPHYSICAL PROCESSES	2	C	Q. WANG		USA	1	NOR	X-RAY SPECTROSCOPY OF 30 DORADUS	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201085010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
93	201058010	EX_HYA	193.10133	-29.24892	192.42641	-28.97736	203.85676	-21.69194	303.18533	33.62235	294.10031	60868.76741	2025-07-12 18:25:04	60870.71949	2025-07-14 17:16:04	83.009	75.000	83.009	71.624	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	76.613	71.624	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-19 06:54:06	2026-07-23 00:00:00	2025-07-20 06:54:06	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011311	The mass of white dwarfs (WDs) within binary systems is a crucial parameter for understanding their evolution into type-Ia supernovae. Among WD binary systems, we focus on the X-ray luminous object, the intermediate polars (IPs) for XRISM observations. The measurement of gravitational redshifts and the bulk Doppler shifts of atomic lines have proven to be robust tools for mass determination, as demonstrated by Hayashi et al.(2023) with Chandra HETG data. We propose a 75 ksec XRISM observation of the IP system EX Hya, to which we already applied the method for lighter elements, to ascertain the WD mass with 10% accuracy with Fe-K lines.	ACCRETING WHITE DWARFS AND NOVAE	2	C	TAICHI ICHIKAWA		JAP	1	NOR	MASS MEASUREMENT OF THE WHITE DWARF IN EX HYA WITH HIGH RESOLUTION X-RAY SPECTROSCOPY	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201058010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
94	201086010	EF_ERI	48.55438	-22.59546	48.00064	-22.78078	38.27036	-38.8878	212.9381	-57.40602	58.1426	60867.46949	2025-07-11 11:16:04	60868.76741	2025-07-12 18:25:04	54.638	50.000	54.638	47.700	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	51.023	47.700	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-18 07:21:09	2026-07-23 00:00:00	2025-07-19 07:21:09	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012119	Polars represent a distinct class of highly magnetized CVs. Measuring their white dwarf (WD) masses is crucial to understanding the origin of WD magnetic fields and the mass evolution of CVs. By fully characterizing Fe K-shell lines with Resolve, we will perform the most detailed X-ray spectroscopic study for two polars (AM Her and EF Eri): (1) robustly testing the conventional Fe line flux ratio diagnostics, (2) detecting non-equilibrium plasma with differing ion and electron temperatures near the shock region, (3) applying new methods of determining WD masses through measuring shock velocities and gravitational redshifts, and (4) constraining the accretion geometry. The proposed observations will demonstrate the unique capabilities of XRISM to probe the fundamental CV astrophysics.	ACCRETING WHITE DWARFS AND NOVAE	2	C	KAYA MORI		USA	1	NOR	COMPLETE HIGH-RESOLUTION FE LINE DIAGNOSTICS OF POLARS WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201086010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
95	201112010	ABELL2052	229.18484	7.02189	228.57028	7.20497	224.63632	24.26449	9.41736	50.12086	298.00266	60865.40352	2025-07-09 09:41:04	60867.46949	2025-07-11 11:16:04	88.472	80.000	88.472	83.604	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		83.604	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-17 08:29:47	2026-07-23 00:00:00	2025-07-18 08:29:47	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012203	The metallicity of the intracluster medium, shaped by billions of Type Ia and core-collapse supernovae explosions, reflects the complex processes from nucleosynthesis to galaxy cluster dynamics. However, determining the exact contributions of these supernovae to galaxy cluster metal enrichment especially in terms of α-capture and Fe-peak elements requires high precision, which has been a significant challenge. With its unparalleled spectral resolution, XRISM-Resolve introduces a new level of accuracy in chemical abundance measurements. To explore these fundamental questions, we propose an 80 ks Resolve observation of Abell 2052, a bright galaxy cluster with a cool core, aiming to quantify these contributions precisely.	GROUPS AND CLUSTERS OF GALAXIES	2	A	PRIYANKA CHAKRABORTY		USA	1	NOR	INVESTIGATING METAL ENRICHMENT IN THE COOL-CORE CLUSTER ABELL 2052	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201112010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
96	201081010	NGC5548	214.49837	25.13699	213.9315	25.36717	202.00151	36.41925	31.96134	70.49553	298.64004	60858.76602	2025-07-02 18:23:04	60865.40352	2025-07-09 09:41:04	301.394	270.000	301.394	271.902	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	290.839	271.902	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-17 11:47:43	2026-07-23 00:00:00	2025-07-18 11:47:43	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012087	This proposal aims to utilize the crucial new capability of XRISM/Resolve to conduct a pivotal investigation on the archetypal Seyfert-1 galaxy NGC 5548. High-resolution spectroscopy of its Fe K band with Resolve would unambiguously identify and parameterize the narrow and broad absorption and emission components. This will transform our knowledge of the highly-ionized outflows and obscuring winds in NGC 5548. By combining the XRISM results with those from an already-approved XMM+NuSTAR+HST program in Cycle 1, a comprehensive understanding of the entire AGN outflow in NGC 5548 is achieved.	NON-JET-DOMINATED AGN	2	C	MISSAGH MEHDIPOUR		USA	1	NOR	BREAKTHROUGH IN UNDERSTANDING AGN OUTFLOWS IN NGC 5548 WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201081010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
97	201031010	CENTAURUS_W	192.14886	-41.33437	191.45834	-41.0618	209.04796	-32.89462	302.3583	21.53421	286.6712	60854.12505	2025-06-28 03:00:04	60858.76602	2025-07-02 18:23:04	296.754	200.000	296.754	270.314	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		270.314	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-13 10:40:17	2026-07-17 00:00:00	2025-07-09 14:17:09	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000015002	The Centaurus cluster offers a unique opportunity to study the intricate interplay among the hot intracluster medium (ICM), the central galaxy (NGC 4696), and the central active galactic nucleus (AGN). Our initial analysis of XRISM Performance Verification (PV) data revealed tantalizing signatures of bulk motions and turbulence in the ICM, potentially driven by the central AGN and sloshing of the central galaxy. This proposal aims to expand upon these findings by observing offset regions, enabling a comprehensive study of the velocity structure, turbulence, and metal distribution across the cluster core. Specifically, we propose deep observations of the western (200 ksec: the 1st priority) and eastern (150 ksec: the 2nd priority) off-center regions, encompassing the detected cold fronts.	GROUPS AND CLUSTERS OF GALAXIES	2	C	KOSUKE SATO	EFRAIN GATUZZ	JEU	1	NOR	UNVEILING THE COMPLEX DYNAMICS OF THE INTRACLUSTER MEDIUM IN THE CENTAURUS CLUSTER WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201031010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
98	201094010	NGC4945	196.36674	-49.46863	195.63672	-49.20094	217.02798	-38.64482	305.27355	13.33933	277.70966	60849.08685	2025-06-23 02:05:04	60854.12505	2025-06-28 03:00:04	291.188	200.000	291.188	278.282	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		278.282	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-13 09:35:54	2026-07-17 00:00:00	2025-07-05 12:17:14	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012134	NGC 4945 is the brightest Seyfert 2 in hard X-rays, and the best example of only a few Compton-thick AGN known to vary strongly >10 keV. The strong hard X-ray variability implies the intrinsic flux is not smeared out by the obscurer, requiring an atypically low torus covering factor. The cause remains unknown, but may be related to outflows depleting the sub-pc reflecting gas. Chandra has also resolved part of the reflector directly on extended scales of ~30pc rather than a classical sub-pc torus. These ill-understood reflector properties make NGC 4945 an ideal target for XRISM. We propose a 200ks observation to constrain the location, density and clumpiness of the obscurer with Resolve, and understand implications for the wider population from this prototype variable Compton-thick AGN.	NON-JET-DOMINATED AGN	2	B	PETER BOORMAN		USA	1	NOR	THE NATURE OF THE CIRCUMNUCLEAR OBSCURING MEDIUM IN THE NEAREST VARIABLE COMPTON-THICK AGN NGC 4945	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201094010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
99	201067010	NGC4507	188.90389	-39.9096	188.22871	-39.63425	205.6644	-32.77975	299.63991	22.86099	283.01684	60846.38894	2025-06-20 09:20:04	60849.08685	2025-06-23 02:05:04	118.557	100.000	118.557	109.499	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		109.499	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-15 02:03:24	2026-07-10 00:00:00	2025-07-05 08:11:26	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000013013	NCG 4507 is one of the X-ray brightest, but highly obscured, Seyfert 2 galaxies. It has been observed several times in the X-ray band, and it has always shown a strong iron K emission line. NCG 4507 is one of the few Compton thin AGN with a clear detection of the Ni Ka emission line. Iron K absorption lines have also been detected, suggesting the presence of an ionized absorber, possibly outflowing. The proposed 100 ksec XRISM observation will allow us to resolve with unprecedented precision the origin of the Fe K emission and absorption lines. Thanks to the high spectral resolution offered by Resolve any contribution from a BLR-Fe Ka will be fully revealed.	NON-JET-DOMINATED AGN	2	B	VALENTINA BRAITO	YOSHIHIRO UEDA	USJ	1	NOR	THE ORIGIN OF THE FE KA LINE IN THE BRIGHT SEYFERT 2 NGC 4507	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201067010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
100	201092010	A2034	227.5489	33.51047	227.04412	33.69924	211.49775	48.69869	53.57168	59.53069	321.39531	60843.47782	2025-06-17 11:28:04	60846.38894	2025-06-20 09:20:04	126.838	120.000	126.838	129.087	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		129.087	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-15 01:43:09	2026-07-04 00:00:00	2025-06-26 07:48:18	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012133	Velocity power spectra (PS) of the ICM are necessary for testing multi-scale physics in numerical simulations and measuring turbulent dissipation/plasma properties. XRISM allows direct studies of ICM kinematics, but the large PSF makes it challenging to extract PS. However, by combining high-resolution imaging and spectroscopic missions, one can calibrate indirect methods of measuring PS. We aim to test the relation between turbulent Mach numbers measured with XRISM and ICM density fluctuations probed with Chandra by observing two clusters, A2034/A1914, with 120/100 ks exposures. These clusters have dissimilar fluctuations measured over a wide scale range, which is ideal for our goal. This calibration will provide a robust method to measure velocity PS and probe ICM transport properties.	GROUPS AND CLUSTERS OF GALAXIES	2	B	IRINA ZHURAVLEVA		USA	1	NOR	COMBINING XRISM AND CHANDRA FOR ROBUST VELOCITY POWER SPECTRA MEASUREMENTS IN THE ICM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201092010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
101	201002010	GAMMA_CASSIOPEIAE	14.17521	60.71578	13.41682	60.44549	43.92909	48.81469	123.57591	-2.14939	93.97284	60842.48130	2025-06-16 11:33:04	60843.47782	2025-06-17 11:28:04	46.521	40.000	46.521	43.504	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	46.534	43.504	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-14 23:26:36	2026-06-25 00:00:00	2025-06-24 05:48:58	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000013002	Binary evolution is one of the most fundamental ingredients in astronomy. Binaries consisting of a high-mass star and a compact object constitute an important milestone in the evolution. Gamma Cas and its analogs could be the long-sought missing population of Be/WD binaries, though an alternative scenario exists. The two scenarios (a) Be/WD binary and (b) magnetic disk-star interaction on Be star surface differ most distinctively in the production site of the hard X-rays. We propose two straightforward and fully independent tests with Resolve to distinguish (a) and (b); the test 1 is the RV change of Fe lines as a function of the orbital phase. The test 2 is the line profile of the flurescent Fe Ka lines. Based on our PV experience, the two tests are only possible with Resolve.	ACCRETING WHITE DWARFS AND NOVAE	2	A	MASAHIRO TSUJIMOTO	SEAN GUNDERSON	JUS	1	NOR	SOLVING THE LONG-STANDING MYSTERY OF GAMMA CASSIOPEIAE WITH RESOLVE	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201002010/	WINDOW2	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
102	201113010	ETA_CARINAE	161.26608	-59.68471	160.77953	-59.42137	202.15612	-58.92718	287.59749	-0.62945	285.00199	60841.73546	2025-06-15 17:39:04	60842.48130	2025-06-16 11:33:04	31.334	25.000	31.334	29.425	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		29.425	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-14 17:23:02	2026-06-25 00:00:00	2025-06-24 05:10:03	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012213	We propose two XRISM observations of Eta Carinae, the closest most massive colliding wind binary during AO1, at a time when the two stars are approaching periastron passage and the X-ray flux is increasing. Our primary goal of measuring important changes in the iron K-line region in the Resolve spectra as the companion star moves towards superior conjunction. These observations will allow us to determine how much the shocked gas cools as the colliding wind shock moves into the acceleration zone of the companion star's wind; constrain the origin of the iron fluorescence line; constrain the Si/Fe ratio as an indicator of chemical abundance; and most importantly, determine the radial velocity shift of the Fe XXV line, which will provide our best measure of the mass of the companion star.	STELLAR CORONAE, WINDS, AND YOUNG STARS	2	A	MICHAEL CORCORAN		USA	1	NOR	ETA CARINAE: MINING THE IRON RANGE WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201113010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
103	201124010	NGC7314	338.9421	-26.05023	338.25142	-26.30948	330.6811	-15.93309	27.13515	-59.74255	74.02228	60839.83824	2025-06-13 20:07:04	60841.73546	2025-06-15 17:39:04	89.616	80.000	89.616	87.110	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		87.110	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-14 17:41:17	2026-06-25 00:00:00	2025-06-24 06:13:07	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000014054	We propose to observe the bright Sy1.9 NGC 7314 as the ideal candidate to unveil the structure and physical conditions through emission lines from cold and ionized material. We will investigate the iron K alpha and K beta narrow and broad emission components and disentangle the contribution to the line of the distant reflector, disk and broad line region. This source is also ideal to study the prominent emission from ionized gas and determine its origin and geometry.	NON-JET-DOMINATED AGN	2	C	ELISA COSTANTINI		EUR	1	NOR	INVESTIGATING THE COMPLEX IRON EMISSION IN NGC7314	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201124010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
104	201090010	RT_CRU	188.7239	-64.56576	187.99863	-64.29023	224.62522	-53.38367	301.15622	-1.75106	261.57714	60835.50005	2025-06-09 12:00:04	60839.83824	2025-06-13 20:07:04	177.706	150.000	177.706	153.453	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		153.453	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-14 13:53:03	2026-06-19 00:00:00	2025-06-18 14:16:23	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012128	The goal of the proposed XRISM observation is to show that high-resolution X-ray spectroscopy can directly reveal the mass of an accreting white dwarf (WD). By measuring the centroids of Fe Ka and Kb; fluorescent lines reflected from the WD, we will determine the gravitational redshift at the WD surface and hence the WD mass in RT Cru, the most hard-X-ray luminous symbiotic binary star. The mass of this WD is thought to be above the likely upper limit for its birth mass. Confirmation of this situation would imply that the mass is almost certainly increasing, establishing a subset of symbiotic stars as viable progenitors for some Type Ia supernovae. Because this project uses emission lines in the 6-7 keV range, it is minimally impacted by the Gate Valve remaining in the closed configuration	ACCRETING WHITE DWARFS AND NOVAE	2	A	JENNIFER SOKOLOSKI		USA	1	NOR	DIRECT MEASUREMENT OF WHITE DWARF MASSES WITH XRISM: GRAVITATIONALLY REDSHIFTED 6.4 KEV LINE IN RT CRU	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201090010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
105	201100010	ABELL85_SW	10.39739	-9.36658	9.76488	-9.64072	5.80348	-12.71797	115.01108	-72.08671	78.00128	60830.70769	2025-06-04 16:59:04	60835.50005	2025-06-09 12:00:04	238.019	200.000	238.019	225.849	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		225.849	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-14 14:51:46	2026-06-19 00:00:00	2025-06-15 12:21:36	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012149	Galaxy clusters are known to grow and assemble via gas accretion and mergers. Somewhere in-between is the case of minor mergers, resulting in dynamical processes such as cold fronts, sloshing, and ram-pressure stripping, all susceptible to impact turbulence and gas (thermo-) dynamics, hence the entire evolution of large scale structures in our Universe. We propose a deep XRISM observation of the triple-merging system Abell 85, with Resolve pointings at the cluster (cool) core and in the two merging sub clusters. This study will be essential to map gas dynamics in this complex system (also with regard to its dark matter distribution), but also to understand the impact of minor mergers on the turbulent support in relaxed clusters.	GROUPS AND CLUSTERS OF GALAXIES	2	B	FRANCOIS MERNIER		USA	1	NOR	DECIPHERING THE DYNAMICS AND CHEMICAL ENRICHMENT OF THE TRIPLE-MERGING SYSTEM ABELL 85	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201100010/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
106	201099010	ABELL85_CORE	10.46043	-9.3031	9.82791	-9.57718	5.88799	-12.68476	115.23677	-72.03133	75.00138	60827.18060	2025-06-01 04:20:04	60830.70769	2025-06-04 16:59:04	172.176	150.000	172.176	162.773	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		162.773	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-14 13:07:47	2026-06-25 00:00:00	2025-06-13 13:36:32	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012149	Galaxy clusters are known to grow and assemble via gas accretion and mergers. Somewhere in-between is the case of minor mergers, resulting in dynamical processes such as cold fronts, sloshing, and ram-pressure stripping, all susceptible to impact turbulence and gas (thermo-) dynamics, hence the entire evolution of large scale structures in our Universe. We propose a deep XRISM observation of the triple-merging system Abell 85, with Resolve pointings at the cluster (cool) core and in the two merging sub clusters. This study will be essential to map gas dynamics in this complex system (also with regard to its dark matter distribution), but also to understand the impact of minor mergers on the turbulent support in relaxed clusters.	GROUPS AND CLUSTERS OF GALAXIES	2	A	FRANCOIS MERNIER		USA	1	NOR	DECIPHERING THE DYNAMICS AND CHEMICAL ENRICHMENT OF THE TRIPLE-MERGING SYSTEM ABELL 85	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201099010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
107	201005010	N63A	83.93253	-66.03614	83.91538	-66.06564	9.34879	-87.50634	275.90621	-32.27128	340.01139	60818.69935	2025-05-23 16:47:04	60827.18060	2025-06-01 04:20:04	544.407	300.000	544.407	363.005	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		363.005	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-15 16:10:43	2026-06-12 00:00:00	2025-06-11 09:41:31	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011065	We propose to observe the middle-aged supernova remnant, N63A, in the Large Magellanic Cloud with an exposure time of 300 ks. Our goals of this observation are (1) to detect signatures of charge-exchange (CX) X-ray emission, and (2) to reveal the origin of the Fe K line emission from this remnant. This observation will provide us with the second solid evidence for CX X-ray emission from SNRs after the first detection in N132D with XRISM (private communication). The line broadening of Fe K lines will clarify if the Fe emission arises from Fe-rich ejecta or swept-up interstellar medium. This study cannot be done without XRISM/Resolve having unprecedented spectral resolution above 2 keV.	SUPERNOVA REMNANTS	2	C	SATORU KATSUDA		JAP	1	NOR	DETECTING CHARGE EXCHANGE X-RAY EMISSION FROM THE N63A SUPERNOVA REMNANT	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201005010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
108	201106010	NGC4192	183.45089	14.90119	182.81433	15.17915	177.09673	15.01497	265.42921	74.96028	314.99915	60816.68269	2025-05-21 16:23:04	60818.69935	2025-05-23 16:47:04	86.710	78.000	86.710	81.204	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		81.204	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-14 04:36:57	2026-06-03 00:00:00	2025-05-31 11:00:46	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012180	The circumgalactic medium (CGM) plays a key role in the evolution and formation of galaxies. Gamma and X-ray observatories discovered spectacular structures in the emission of the tenuous gas surrounding the Milky Way: the so-called Fermi and eROSITA bubbles. Galaxy formation simulations suggest that MW-like bubbles could be ubiquitous, but so far no instrument offered the combination of a large field of view, low background, and high sensitivity required for their detection in other galaxies. We propose to search for MW-like bubbles in two nearby, edge-on, disk galaxies, analogs of the Milky Way and Andromeda. Exploiting XRISM Xtend capabilities, we will explore the presence of MW-like bubbles by characterizing the spatial and spectral properties of the large-scale CGM emission.	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	2	A	AKOS BOGDAN		USA	1	NOR	A XRISM PATHFINDER STUDY: MILKY WAY-LIKE BUBBLES IN EXTERNAL DISK GALAXIES	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201106010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
109	201105010	NGC4565	189.08636	25.98776	188.46653	26.26286	177.15845	27.28958	230.75293	86.43773	314.9991	60815.29171	2025-05-20 07:00:04	60816.68269	2025-05-21 16:23:04	61.126	56.000	61.126	60.094	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		60.094	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-14 02:17:30	2026-06-03 00:00:00	2025-05-31 09:21:43	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012180	The circumgalactic medium (CGM) plays a key role in the evolution and formation of galaxies. Gamma and X-ray observatories discovered spectacular structures in the emission of the tenuous gas surrounding the Milky Way: the so-called Fermi and eROSITA bubbles. Galaxy formation simulations suggest that MW-like bubbles could be ubiquitous, but so far no instrument offered the combination of a large field of view, low background, and high sensitivity required for their detection in other galaxies. We propose to search for MW-like bubbles in two nearby, edge-on, disk galaxies, analogs of the Milky Way and Andromeda. Exploiting XRISM Xtend capabilities, we will explore the presence of MW-like bubbles by characterizing the spatial and spectral properties of the large-scale CGM emission.	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	2	A	AKOS BOGDAN		USA	1	NOR	A XRISM PATHFINDER STUDY: MILKY WAY-LIKE BUBBLES IN EXTERNAL DISK GALAXIES	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201105010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
110	201066010	NGC4051	180.78988	44.53155	180.1515	44.80988	159.25765	40.34142	148.88299	70.08489	308.94373	60811.70074	2025-05-16 16:49:04	60815.29171	2025-05-20 07:00:04	164.356	150.000	164.356	157.244	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		157.244	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-14 06:06:22	2026-05-29 00:00:00	2025-05-27 10:56:55	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000013014	Precise profile measurements of features in the Fe K band will allow unprecedented constraints on the reprocessor, within a framework defined by the tightly-constrained black hole mass that makes NGC 4051 a compelling target for XRISM Cycle 1. We request 150 ks observation to: (i) determine the precise origin of the Fe Ka line, (ii) measure the kinematics of the ionized outflow and (iii) detect and identify lines seen red-ward of Fe Ka.	NON-JET-DOMINATED AGN	2	B	TRACEY TURNER	SHOJI OGAWA	USJ	1	NOR	FE K-BAND SIGNATURES: THE KEY TO MAPPING THE LOW MASS SYSTEM OF NGC 4051	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201066010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
111	201040010	PUPPIS_A_EJECTA	125.72733	-42.75245	125.29569	-42.59071	147.14683	-59.30901	260.27336	-3.18597	283.00242	60805.66880	2025-05-10 16:03:04	60811.70074	2025-05-16 16:49:04	364.781	250.000	364.781	338.436	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		338.436	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-16 00:41:13	2026-05-29 00:00:00	2025-05-25 06:20:13	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011210	We propose two pointings on the Galactic supernova remnant Puppis A. One is a 250 ks observation on the region where we recently found Fe-rich ejecta. The other is a 200 ks observation on the bright eastern knot. The scientific objectives of the former are (1) to measure the plasma condition, metal composition, and kinematics of the Fe-rich ejecta with Resolve, and (2) to map the spatial structure of the Fe-rich ejecta with Xtend. The scientific objective of the latter is to detect charge exchange (CX) X-ray emission from Puppis A for the first time. This observation provides us with crucial clues to understand the shock structure, the progenitor s explosion mechanism, and the basics of CX emission of this unique remnant.	SUPERNOVA REMNANTS	2	C	KOJI MORI		JAP	1	NOR	REVEALING THE NATURE OF FE-RICH EJECTA AND CHARGE EXCHANGE REACTION IN THE GALACTIC SUPERNOVA REMNANT PUPPIS A	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201040010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
112	201043010	A1060_CENTER	159.19217	-27.53045	158.60351	-27.27069	172.77024	-33.32464	269.61492	26.49194	279.99833	60803.29727	2025-05-08 07:08:04	60805.66880	2025-05-10 16:03:04	122.317	100.000	122.317	115.324	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		115.324	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-13 19:01:08	2026-05-29 00:00:00	2025-05-24 14:14:39	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011226	We propose XRISM observations of Abell 1060, the brightest and one of the nearest non-cool core/non-merging cluster, suggested by its nearly circular symmetric ICM. There is no strong AGN-jet-ICM interaction and the ICM is likely be "calm". Measuring its bulk flow and turbulence is very important for XRISM, because all cluster PV targets are either cool-core clusters or merging clusters. This observation will provide a baselines for ICM science. By a 100 ks observation at the center, and a 200 ks observation at ~4' offset to the east, we aim to observe a ~100 km/s level of bulk motion and turbulence to the accuracy of < 30 km/s (90% CL). Origin of the newly found soft-radio diffuse source "Flying Fox", and ISM stripping of the spiral galaxy NGC 3312 are also in the scope.	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	2	C	KAZUHIRO NAKAZAWA		JAP	1	NOR	HOW ``CALM'' IS THE ICM OF THE NEAREST NON COOL-CORE CLUSTER ABELL 1060?	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201043010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
113	201071010	HYDRA_A_NORTH	139.52435	-12.04629	138.92221	-11.83546	146.12505	-26.35946	242.88318	25.12372	294.48653	60798.96880	2025-05-03 23:15:04	60803.29727	2025-05-08 07:08:04	195.387	200.000	195.387	185.511	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		185.511	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-13 20:32:24	2026-05-29 00:00:00	2025-05-24 16:06:05	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012044	Hydra A is the most powerful FR I radio source in the nearby Universe. Emanating from the central galaxy in a bright X-ray cluster, its jets have inflated a system of X-ray cavities and a surrounding Mach 1.3 shock front extending several hundred kiloparsecs into the cluster atmosphere. Its proximity (z=0.054) and large angular size requires two pointings to measure the energetics of the active inner jets and a second pointing toward the enormously powerful northern cavity and surrounding shock front. The pointings will reveal the expansion speed and cluster weather due to atmospheric bulk motion on the structure of the X-ray cavities. This measurement addresses the fundamental problem of how jet energy heats cluster atmospheres and prevents catastrophic cooling.	GROUPS AND CLUSTERS OF GALAXIES	2	C	BRIAN MCNAMARA		USA	1	NOR	ATMOSPHERIC GAS MOTIONS IN THE HYDRA A GALAXY CLUSTER	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201071010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
114	201022010	SPT-CL_J2344-4243	356.18301	-42.72059	355.52363	-42.99834	336.76364	-37.08417	339.62846	-69.34119	45.00322	60792.18755	2025-04-27 04:30:04	60798.96880	2025-05-03 23:15:04	274.738	250.000	274.738	251.271	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		251.271	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-13 22:30:47	2026-06-03 00:00:00	2025-05-24 19:20:06	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011138	We propose a 250 ksec observation of the Phoenix cluster at z=0.597, the most X-ray luminous galaxy cluster as well as the only cooling flow cluster known to date. By combining Fe XXV and Fe XXVI lines, we will be able to measure velocities both inside and outside the cool core, thereby complementing the lack of spatial resolution of XRISM by its spectral capability. Our goals include testing if (i) turbulent heating can be a generic mechanism for heating the cool core, (ii) hydrostatic equilibrium is valid for this apparently quiescent system, and (iii) there are any large-scale structures associated with the most massive galaxy cluster at z~0.6. The proposed XRISM observation will provide unprecedented view of the distant diffuse Universe even with the closed Gate Valve configuration.	GROUPS AND CLUSTERS OF GALAXIES	2	A	TETSU KITAYAMA		JAP	1	NOR	DYNAMICAL STATE OF A UNIQUE COOLING-FLOW GALAXY CLUSTER AT Z~0.6	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201022010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
115	201016010	ABELL754_SUB	137.23533	-9.65558	136.62674	-9.45219	142.89743	-24.84373	239.28553	24.76553	291.63224	60787.24102	2025-04-22 05:47:04	60792.18755	2025-04-27 04:30:04	200.372	200.000	200.372	179.777	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		179.777	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-05-03 10:09:42	2026-05-08 00:00:00	2025-05-04 10:09:43	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011090	We propose two-pointing deep observations for a sloshing main gas halo (100 ksec) and a subhalo on the verge of destruction (200ksec) in a nearby violent merger, Abell 754, of which the merger axis is almost aligned on the sky plane. Edge-on observation allows us to separate hydrodynamic motion perpendicular to the merger axis from the merger-induced inflow motion. The perpendicular motion acting on disrupting gas halos is only induced in the gas by its collisional nature. Our observation will reveal mixing and incorporating processes of the gas, that is, a scene of hierarchical structure formation. Together with merger parameters derived from weak-lensing mass distribution from Subaru/HSC and galaxy dynamics, a direct measurement of the gas motion and X-ray thermodynamics give us a compr	GROUPS AND CLUSTERS OF GALAXIES	2	C	NOBUHIRO OKABE		JAP	1	NOR	ABELL 754: CAPTURING THE HYDRODYNAMIC MOTION PERPENDICULAR TO THE MERGER AXIS	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201016010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
116	201059010	N49	81.49819	-66.08287	81.47919	-66.12411	4.05822	-86.55517	276.0943	-33.24742	325.00572	60781.66324	2025-04-16 15:55:04	60787.24102	2025-04-22 05:47:04	226.446	200.000	226.446	197.923	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		197.923	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-25 18:27:53	2026-05-06 00:00:00	2025-04-26 18:27:54	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011327	We propose a 200-ks XRISM observation of the supernova remnant (SNR) N49. Our goals are to understand the evolutionary process of the over-ionized plasma, and to clarify the forming mechanism of an associated magnetar. Combining with the XRISM observation with the Reflection Grating Spectrometer on board XMM Newton, we will be able to perform unique plasma diagnostics using Fe K and L shell lines, and to establish the first robust constraint on the initial electron temperature of this peculiar over-ionized plasma. In addition to these line diagnostics, measurements of the line-of-sight expansion structure and proton cyclotron absorption features will provide insights into the explosion mechanism and nature of the progenitor of N49.	SUPERNOVA REMNANTS	2	C	YUKI AMANO		JAP	1	NOR	ORIGIN OF THE OVER-IONIZED PLASMA WITH AN EXTRAORDINARILY HIGH INITIAL TEMPERATURE IN SUPERNOVA REMNANT N49	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201059010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
117	201060010	GX5-1	270.28426	-25.07831	269.51321	-25.07781	270.25757	-1.63927	5.07797	-1.01816	90.68181	60780.57435	2025-04-15 13:47:04	60781.66324	2025-04-16 15:55:04	51.164	50.000	51.164	5.577	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	44.522	0.000	0.000	5.577	11110	313430	11310	PROCESSED	2025-04-23 11:17:41	2026-04-29 00:00:00	2025-04-24 11:17:41	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011330	Recent analyses of extraterrestrial materials returned by sample return missions have refined our understanding of solar composition. However, the elemental composition within the Milky Way, historically estimated from meteorites and the Sun's photosphere, faces scrutiny for potentially underrepresenting heavy elements compared to interstellar space. This proposal aims to utilize XRISM to accurately quantify the total abundance of heavy elements, including iron, in both gaseous and solid states in the interstellar medium towards GX~5-1, a Low-Mass X-ray Binary, overcoming limitations of traditional methods.	BH AND NS BINARIES	2	B	TASUKU HAYASHI		JAP	1	NOR	INVESTIGATING THE COMPOSITION AND STATE OF IRON IN THE INTERSTELLAR MEDIUM USING X-RAY ABSORPTION SPECTROSCOPY	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201060010/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
118	201000010	4U1822-371	276.44486	-37.10492	275.59452	-37.13412	275.28875	-13.78388	356.85039	-11.29054	92.10474	60777.72157	2025-04-12 17:19:04	60780.57435	2025-04-15 13:47:04	124.681	100.000	124.681	105.991	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	113.374	105.991	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-22 11:33:48	2026-04-25 00:00:00	2025-04-23 11:33:49	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011048	In most XRISM programs to come, spectral lines observed with Resolve are formed in the NLTE conditions. For proper interpretations of the observed spectra, spectral synthesis based on the numerical radiative transfer calculation is a requisite. Currently, however, no RT code is reliable enough to compare to the observed data in the X-rays. What we should do now is to benchmark the numerical RT calculations against the actual observations. We demonstrated that this approach is productive for the soft X-ray band using XMM-Newton grating spectra of an ADC hosting a WD. We propose to observe 4U 1822 370, an ADC hosting a NS with Resolve to extend our study to hard X-rays. The goal of this observation is to record the high-quality spectrum to be used for benchmarking RT calculations.	BH AND NS BINARIES	2	A	MASAHIRO TSUJIMOTO		JAP	1	NOR	VERIFYING THE NUMERICAL RADIATIVE TRANSFER CALCULATION USING AN ACCRETION DISK CORONA SOURCE	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201000010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
119	201046010	SAGITTARIUS_C	266.12267	-29.46089	265.32514	-29.44013	266.60563	-6.06727	359.4238	-0.06373	91.99934	60773.93407	2025-04-08 22:25:04	60777.72157	2025-04-12 17:19:04	159.880	150.000	159.880	140.561	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		140.561	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-23 08:26:11	2026-04-29 00:00:00	2025-04-24 08:26:11	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011240	The Galactic center diffuse X-rays (GCXE) has been one of interesting mysteries in X-ray astronomy for 50 years. It is still under discussion whether the origin of the GCXE is ensemble of faint point sources or truly diffuse plasma. This XRISM observation will aim to the Sagittarius B and C regions in the Galactic center to perform measurement of dynamical motion and plasma diagnostics and to derive the diffuse plasma from the GCXE for the first time. The physical information (motion, temperature, ionization degree, mass, abundances) constrain production mechanism of the diffuse plasma (stellar wind, supernova, Sgr A*, etc). Contribution to the evolution of the Galaxy will be also discussed.	GALACTIC DIFFUSE EMISSION AND SURVEYS	2	A	MASAYOSHI NOBUKAWA		JAP	1	NOR	FIRST MEASUREMENT OF DYNAMICS AND PLASMA DIAGNOSTICS OF THE GALACTIC CENTER DIFFUSE X-RAYS	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201046010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
120	101008011	1E0102.2-7219	16.00725	-72.03092	15.60228	-72.29889	314.63713	-65.03559	301.55761	-45.06372	0.71197	60773.38037	2025-04-08 09:07:44	60773.93407	2025-04-08 22:25:04	0.000	30.000	0.000	22.610	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	DIM	OFF	2	31100010	320000A0	24.185	22.610	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-18 06:54:30	2025-08-31 00:00:00	2025-04-19 06:54:31	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101008011/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
121	101008010	1E0102.2-7219	16.00814	-72.03112	15.60319	-72.29909	314.63698	-65.03592	301.55724	-45.0635	0.71075	60773.09241	2025-04-08 02:13:04	60773.38037	2025-04-08 09:07:44	0.000	30.000	0.000	7.499	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	BRIGHT	OFF	2	31100010	320000A0	8.021	7.499	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-18 06:39:20	2025-08-31 00:00:00	2025-04-19 06:39:21	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101008010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
122	101007011	1E0102.2-7219	16.00693	-72.03094	15.60196	-72.29892	314.63699	-65.03551	301.55775	-45.0637	0.69528	60772.67319	2025-04-07 16:09:24	60773.09241	2025-04-08 02:13:04	0.000	30.000	0.000	13.949	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	BRIGHT	OFF	1	300000A0		13.949	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-16 12:30:28	2025-08-31 00:00:00	2025-04-17 12:30:28	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101007011/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
123	101007010	1E0102.2-7219	16.0087	-72.03109	15.60376	-72.29906	314.63722	-65.03607	301.55699	-45.06352	0.69456	60772.23685	2025-04-07 05:41:04	60772.67319	2025-04-07 16:09:24	0.000	30.000	0.000	17.396	PX_NORMAL	N	Y	N	N	N	N	Y	DIM	OFF	OFF	OFF	1	300000A0		17.396	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-16 11:46:13	2025-08-31 00:00:00	2025-04-17 11:46:14	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101007010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
124	101014011	Cygnus_Loop	312.70519	31.89067	312.19178	31.70278	327.82371	47.12939	74.92145	-7.76821	87.99931	60772.06093	2025-04-07 01:27:44	60772.23685	2025-04-07 05:41:04	0.000	30.000	0.000	7.297	PX_NORMAL	N	Y	N	N	N	N	Y	DIM	OFF	OFF	OFF	1	300000A0		7.297	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-16 11:15:05	2025-08-31 00:00:00	2025-04-17 11:15:05	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101014011/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
125	101014010	Cygnus_Loop	312.70537	31.89032	312.19196	31.70244	327.82371	47.12902	74.92128	-7.76854	87.99861	60771.49380	2025-04-06 11:51:04	60772.06093	2025-04-07 01:27:44	0.000	30.000	0.000	24.791	PX_NORMAL	N	Y	N	N	N	N	Y	BRIGHT	OFF	OFF	OFF	1	300000A0		24.791	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-16 12:29:23	2025-08-31 00:00:00	2025-04-17 12:29:23	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101014010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
126	201006010	OPHIUCHUS_CLUSTER	258.114	-23.36865	257.35585	-23.3095	259.10124	-0.37793	0.57343	9.27166	94.84313	60765.92782	2025-03-31 22:16:04	60771.49380	2025-04-06 11:51:04	217.118	200.000	217.118	188.844	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		188.844	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-12 17:22:44	2026-04-16 00:00:00	2025-04-13 17:22:44	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011075	The Ophiuchus cluster, the second brightest X-ray source, provides a unique study of an exceptionally hot (9keV) cluster. Despite high temperatures indicating merger disruption, it has retained its cool core. Previous observations conflict on the internal gas velocity in the core, ranging from <100 to >2000km/s. We will use the spectral resolution of XRISM to precisely measure the velocity, resolve the discrepancy, and reveal the core destruction processes. The obtained velocity will allow the estimation of instability timescales that drive core evolution. We will also study elemental abundances to see if the population of supernovae differs from cooler clusters. This multi-pronged approach will provide insights into the formation and evolution of this extraordinary cluster.	GROUPS AND CLUSTERS OF GALAXIES	2	B	YUTAKA FUJITA		JAP	1	NOR	UNVEILING THE DYNAMICS AND CHEMICAL ENRICHMENT OF THE OPHIUCHUS GALAXY CLUSTER WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201006010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
127	201117010	OPHIUCHUS_CLUSTER_SE	258.12864	-23.39293	257.37035	-23.33385	259.11662	-0.40103	0.56109	9.24672	94.84379	60762.93199	2025-03-28 22:22:04	60765.92782	2025-03-31 22:16:04	116.627	100.000	116.627	103.281	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		103.281	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-16 10:39:47	2026-04-16 00:00:00	2025-04-13 14:24:01	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000014021	Radio jets are powered by gas accretion onto supermassive black holes and inflate large bubbles in galaxy and cluster atmospheres. The energy input is substantial, but must be distributed and dissipated on large scales to suppress gas cooling and slow massive galaxy growth. We propose a 100ks Resolve observation of the Ophiuchus cluster to measure turbulence and bulk motion in the wake of the largest radio bubble on the sky. The bubble's wake reveals no unrelated structure and is well-matched to Resolve's field of view. By measuring the induced gas motions, we will determine the fraction of the bubble's enthalpy that is transferred to the intracluster medium (ICM), whether turbulence or bulk motion dominates and if bubbles can lift gas flows in their wakes to sustain feedback.	GROUPS AND CLUSTERS OF GALAXIES	2	A	HELEN RUSSELL		EUR	1	NOR	GAS MOTIONS IN THE WAKE OF THE LARGEST RADIO BUBBLE IN A CLUSTER CORE	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201117010/	WINDOW1		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
128	201014010	SS433	287.95581	4.98264	287.33798	4.89823	290.19499	27.17181	39.6937	-2.24401	80.53198	60760.57644	2025-03-26 13:50:04	60762.93199	2025-03-28 22:22:04	98.374	80.000	98.374	86.729	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		86.729	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-11 13:33:03	2026-04-16 00:00:00	2025-04-12 13:33:04	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011085	We propose an 80 ks observation of the Galactic microquasar SS 433, consisting of a 50 ks exposure in the out-of-eclipse phase and 30 ks in the ingress or egress of an eclipse. The main aim is to resolve the Doppler-shifted emission lines from the bipolar jets and thereby investigate the geometry and plasma properties in the X-ray emitting region of the jets. We also determine the direction of the orbital rotation with respect to that of the jet precession, by monitoring how the approaching and receding jets are occulted by the companion star during the ingress or egress of an eclipse.	BH AND NS BINARIES	2	A	MEGUMI SHIDATSU		JAP	1	NOR	PROBING THE JET STRUCTURE IN THE MICROQUASAR SS 433	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201014010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
129	201018010	GX1+4	263.00753	-24.74524	262.23961	-24.70949	263.65029	-1.45994	1.93662	4.79626	93.08029	60759.21671	2025-03-25 05:12:04	60760.57644	2025-03-26 13:50:04	47.379	40.000	47.379	39.744	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	42.512	39.744	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-11 10:44:48	2026-04-16 00:00:00	2025-04-12 10:44:48	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011098	One of the big questions in neutron stars is how the strong magnetic field is formed and evolved. We propose a 40 ks observation of a low-mass X-ray binary pulsar GX 1+4, which has long been suspected to have a very high magnetic field strength, perhaps ~ 1e14 G. Thanks to the excellent energy resolution of the Resolve, the proposed observation enables us for the first time to resolve the profile of the Fe K alpha lines and to measure the magnetic field strength above 1e13 G, which is impossible to probe using the cyclotron resonance scattering feature (CRSF). From this observation we can determine whether or not the source is the first magnetar binary ever detected. Moreover, Resolve may provide a unique opportunity to search for the proton CRSF.	BH AND NS BINARIES	2	B	TOSHIHIRO TAKAGI		JAP	1	NOR	DETERMINING THE MAGNETIC FIELD STRENGTH OF THE LOW MASS X-RAY BINARY PULSAR GX 1+4: A UNIQUE MAGNETAR BINARY?	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201018010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
130	201122010	ABELL496_CENTER	68.40878	-13.2616	67.82932	-13.36537	64.14528	-34.78308	209.5871	-36.48691	278.262	60758.65699	2025-03-24 15:46:04	60759.21671	2025-03-25 05:12:04	26.378	20.000	26.378	24.951	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		24.951	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-10 16:01:56	2026-04-05 00:00:00	2025-03-29 19:39:35	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000014040	The bright, nearby, and hot cluster Abell 496 is a unique system. Strong gas sloshing features have been observed. Simulations of the system predict that a previous north-south minor merger induced these. eROSITA detects an emission enhancement in the north-north-west direction and XRISM is ideally suited to measure corresponding gas velocities for the first time. Combining these two datasets, we will test the merger scenario and, if confirmed, constrain its parameters.	GROUPS AND CLUSTERS OF GALAXIES	2	C	THOMAS REIPRICH		EUR	1	NOR	THE SLOSHING CORE OF ABELL 496	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201122010/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
131	201019010	3C120	68.29696	5.35417	67.63242	5.24971	67.43077	-16.40083	190.37349	-27.39635	268.4925	60753.74032	2025-03-19 17:46:04	60758.65699	2025-03-24 15:46:04	221.970	200.000	221.970	195.932	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	209.578	195.932	0.000	0.000	11110	313430	11310	PROCESSED	2025-03-28 21:45:28	2026-04-05 00:00:00	2025-03-29 21:45:28	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011124	The jet production mechanism remains one of the most important questions in astrophysics, and a key is how mass accretion and disk wind are related to a jet. Therefore, we propose a 200 ksec observation on an X-ray bright radio galaxy 3C120 with XRISM, combining observations by mm-VLBIs: EAVN, GMVA, and EHT. With Resolve, we can constrain the disk wind properties, the mass accretion structure, and the disk truncation radius by resolving Fe XXV/XXVI lines, and narrow and broad Fe-K lines, respectively. Xtend can determine the jet synchrotron in soft X-ray. These can be directly compared to the jet activity and structure, spatially resolved by mm-VLBIs. By this powerful method, we constrain the relation of the jet production to mass accretion/disk wind most strongly so far.	BLAZARS AND OTHER JET-DOMINATED AGN	2	A	HIROFUMI NODA		JAP	1	NOR	RESOLVING THE MASS ACCRETION AND JET EJECTION IN 3C120 WITH XRISM & MM-VLBIS (EAVN, GMVA, AND EHT)	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201019010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
132	201052010	RADIO_ARC	266.59627	-28.89568	265.80224	-28.87722	267.00669	-5.49175	0.1217	-0.12191	80.0005	60750.66741	2025-03-16 16:01:04	60753.74032	2025-03-19 17:46:04	119.813	100.000	119.813	116.670	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		116.670	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-03-29 05:44:19	2026-04-05 00:00:00	2025-03-30 05:44:20	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013003	The most characteristic spectral features of the Galactic center are bright fluorescence X-rays at 6.4 keV emitted from neutral Fe atoms in molecular clouds. Photoionization by X-rays from Sagittarius A* has been considered as its origin (the XRNe scenario). On the other hand, the Galactic center should have a high density of low-energy cosmic rays (CRs), and thus there is still a strong possibility that the neutral Fe line is due to CR bombardment. In this observation, we will explore new spectral features that could never be observed by X-ray CCD energy resolutions, and measure neutral emission lines from other elements so that we will quantitatively clarify the ratio of the XRNe and CR origins.	GALACTIC DIFFUSE EMISSION AND SURVEYS	2	A	KUMIKO NOBUKAWA	SHUO ZHANG	JUS	1	NOR	THE ORIGIN OF THE NEUTRAL FE LINE IN THE GALACTIC CENTER EXPLORED BY NEW SPECTRAL FEATURES	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201052010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
133	201054010	RCW86_SW	220.22387	-62.67192	219.2403	-62.45774	240.72966	-44.19932	315.12495	-2.42043	114.99726	60743.60838	2025-03-09 14:36:04	60750.66741	2025-03-16 16:01:04	431.262	280.000	431.262	409.239	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		409.239	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-03-29 23:39:38	2026-04-05 00:00:00	2025-03-30 23:39:38	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000015001	Collisionless shocks are one of the most attracting phenomena in the universe, as the sites where the shock kinetic energy is transformed into thermal and non-thermal energies. They are important research targets in both physical and astronomical aspects. One of the ideal and most well-studied collisionless shocks are seen in supernova remnants. We propose a 280 ks XRISM observation of the southwestern region of RCW 86, where the Fe-K emission is brightest over the remnant. We will 1) determine Fe-Ka and Kb centroids, flux ratio and broadening, and robustly estimating the efficiency of the collisionless electron heating and reverse shock velocity, and 2) locating the reverse shock surface based on the spatial distribution of the Fe-Kb flux.	SUPERNOVA REMNANTS	2	A	HIROMASA SUZUKI	JACCO VINK	JEU	1	NOR	COLLISIONLESS ELECTRON HEATING AT A REVERSE SHOCK IN THE SUPERNOVA REMNANT RCW 86	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201054010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
134	201045030	SAGITTARIUS_B	266.82504	-28.37967	266.03421	-28.36233	267.19638	-4.97127	0.667	-0.02582	88.70295	60742.45352	2025-03-08 10:53:04	60743.60838	2025-03-09 14:36:04	51.166	150.000	51.166	47.948	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		47.948	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-03-28 11:24:52	2026-04-05 00:00:00	2025-03-29 11:24:53	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011240	The Galactic center diffuse X-rays (GCXE) has been one of interesting mysteries in X-ray astronomy for 50 years. It is still under discussion whether the origin of the GCXE is ensemble of faint point sources or truly diffuse plasma. This XRISM observation will aim to the Sagittarius B and C regions in the Galactic center to perform measurement of dynamical motion and plasma diagnostics and to derive the diffuse plasma from the GCXE for the first time. The physical information (motion, temperature, ionization degree, mass, abundances) constrain production mechanism of the diffuse plasma (stellar wind, supernova, Sgr A*, etc). Contribution to the evolution of the Galaxy will be also discussed.	GALACTIC DIFFUSE EMISSION AND SURVEYS	2	A	MASAYOSHI NOBUKAWA		JAP	1	NOR	FIRST MEASUREMENT OF DYNAMICS AND PLASMA DIAGNOSTICS OF THE GALACTIC CENTER DIFFUSE X-RAYS	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201045030/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
135	201041020	G349.7+0.2	259.50088	-37.43905	258.65101	-37.38628	261.41263	-14.31222	349.72856	0.17051	90.00166	60739.01463	2025-03-05 00:21:04	60742.45352	2025-03-08 10:53:04	173.517	150.000	173.517	169.573	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		169.622	0.000	0.000	0.006	11110	313430	11310	PROCESSED	2025-03-28 13:07:04	2026-04-05 00:00:00	2025-03-29 13:07:04	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011218	Although a textbook explanation says that stars with a mass between 8-30M_sun explodes as a standard core-collapse supernova (SN), the true mass range is still unknown: stars with masses at the lower limit of this range are believed to experience electron capture SN and such SNe is thought to eject large amount of nickel (Ni) during the explosion. Here we propose an observation of G349.7+0.2, whose Ni abundance is highest among all the SNRs. While our previous analysis has large uncertainties, XRISM has the capability to accurately determine the yields of Fe-group elements and their velocity structures, providing valuable insights into the lower mass limit for standard SNe and potentially offer the first robust evidence of electron capture SN in our Galaxy.	SUPERNOVA REMNANTS	2	B	HIROYUKI UCHIDA		JAP	1	NOR	INVESTIGATING THE NATURE OF NI-RICH SNR G349.7+0.2: SEARCHING FOR FIRST ROBUST EVIDENCE OF ELECTRON-CAPTURE EXPLOSION	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201041020/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
136	901002010	MAXI_J1744-294	266.42427	-29.00914	265.62955	-28.98985	266.8583	-5.60884	359.9465	-0.05241	90.00252	60737.47921	2025-03-03 11:30:04	60739.01463	2025-03-05 00:21:04	71.481	60.000	71.481	9.286	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	74.134	0.000	0.000	9.286	11110	313430	11310	PROCESSED	2025-03-11 07:16:26	2023-09-06 00:00:00	2025-03-12 07:16:27	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000019008	MAXI J1744-294 is a newly discovered X-ray transient located just 25" from Sgr A, confirmed by NinjaSAT and Swift-BAT/XRT. Recent observations with NuSTAR indicate it is a black hole (BH) transient in a soft state. In the central parsec region near Sgr A, known BH transients may exhibit outbursts with a several-decades recurrent time, with the last occurrence being in 2016. This suggests that MAXI J1744-294 may not erupt again for decades, potentially making it the only BH outburst in the Galactic Center during the XRISM operation. Given the rarity of such events, we propose a joint XRISM observation alongside scheduled ones with NuSTAR, XMM, and Chandra to capitalize on this unique opportunity to study the transient.	BH AND NS BINARIES	9	A	XRISM Collaboration		DDT	1	DDT-TOO	DDT TOO REQUEST OF MAXI J1744-294	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/901002010/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
137	201041010	G349.7+0.2	259.50074	-37.43846	258.65087	-37.38568	261.41246	-14.31163	349.72898	0.17094	90.00147	60733.96949	2025-02-27 23:16:04	60737.47921	2025-03-03 11:30:04	206.068	300.000	206.068	185.727	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		185.776	0.046	0.000	0.000	11110	313430	11310	PROCESSED	2025-03-07 14:52:36	2026-04-05 00:00:00	2025-03-08 14:52:37	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011218	Although a textbook explanation says that stars with a mass between 8-30M_sun explodes as a standard core-collapse supernova (SN), the true mass range is still unknown: stars with masses at the lower limit of this range are believed to experience electron capture SN and such SNe is thought to eject large amount of nickel (Ni) during the explosion. Here we propose an observation of G349.7+0.2, whose Ni abundance is highest among all the SNRs. While our previous analysis has large uncertainties, XRISM has the capability to accurately determine the yields of Fe-group elements and their velocity structures, providing valuable insights into the lower mass limit for standard SNe and potentially offer the first robust evidence of electron capture SN in our Galaxy.	SUPERNOVA REMNANTS	2	B	HIROYUKI UCHIDA		JAP	1	NOR	INVESTIGATING THE NATURE OF NI-RICH SNR G349.7+0.2: SEARCHING FOR FIRST ROBUST EVIDENCE OF ELECTRON-CAPTURE EXPLOSION	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201041010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
138	201057010	1E1740.7-2942	265.97795	-29.74458	265.17863	-29.72311	266.48697	-6.35433	359.11622	-0.10507	89.76059	60731.55282	2025-02-25 13:16:04	60733.96949	2025-02-27 23:16:04	129.446	100.000	129.446	108.986	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	116.577	108.986	0.000	0.000	11110	313430	11310	PROCESSED	2025-03-06 13:24:05	2026-03-11 00:00:00	2025-03-07 13:24:05	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011310	We propose 100 ksec observation of the microquasar 1E 1740.7--2942 to reveal an existence of Doppler-shifted emission lines originating from ionized heavy elements in relativistic jets with XRISM/Resolve. This microquasar is persistent X-ray source with steady bipolar radio jets in the Galaxy Centre region. Previous Chandra/HETGS observation in 1999 suggested a possible narrow Doppler-shifted emission lines originating from jets. Through high resolution X-ray spectroscopy with XRISM, we will clarify whether the jet plasma is really hadronic origin and could make 1E 1740.7--2942 the second jet source which shows a direct evidence for hadron acceleration in jets after SS433.	BH AND NS BINARIES	2	B	KAZUTAKA YAMAOKA		JAP	1	NOR	DIRECT EVIDENCE FOR HADRON ACCELERATION IN PERSISTENT JETS OF THE MICROQUASAR 1E 1740.7--2942 WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201057010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
139	201032010	TOOTHBRUSH_S	90.83052	42.20197	89.93751	42.20385	90.64976	18.76455	170.24565	9.72421	278.86915	60728.54102	2025-02-22 12:59:04	60731.55282	2025-02-25 13:16:04	166.747	100.000	166.747	137.308	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		137.308	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-03-06 14:16:20	2026-03-11 00:00:00	2025-03-07 14:16:20	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011171	At radio frequencies, the Toothbrush Cluster is a spectacular source that has been essential in revealing details of the particle acceleration generated during mergers. We propose to map the velocity field of the intracluster medium in this remarkable target with two Resolve pointings. One will probe the radio halo, where particle acceleration is driven by developed turbulence. The second will probe the region between the halo and the 2~Mpc-long radio shock, where strong gradients in the radio spectral index map indicate a transition between turbulence-driven and shock-driven acceleration. Determining and comparing the line broadening and shifts between these regions will provide key information needed to complete physical picture of cosmic ray electron acceleration on the largest scales.	GROUPS AND CLUSTERS OF GALAXIES	2	A	HIROKI AKAMATSU		JAP	1	NOR	PROBING THE PHYSICS OF TURBULENT PARTICLE ACCELERATION IN ``THE TOOTHBRUSH''	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201032010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
140	201007010	MRK0003	93.90645	71.03635	92.45674	71.05182	91.88234	47.62259	143.29776	22.71986	293.92946	60727.59796	2025-02-21 14:21:04	60728.54102	2025-02-22 12:59:04	61.747	40.000	61.747	61.342	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	65.615	61.342	0.000	0.000	11110	313430	11310	PROCESSED	2025-03-05 08:04:57	2026-03-07 00:00:00	2025-03-06 08:04:58	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011077	We propose a 40 ksec observation of a radio-quiet luminous Seyfert 2 galaxy, Mrk 0003. To estimate the mass of a Supermassive Black Hole (SMBH), a high-potential method is to measure the velocity dispersion of neutral iron fluorescence. Although the X-ray spectra of the Seyfert 2 galaxies exhibit neutral iron fluorescence, the origin of neutral iron fluorescence remains unclear for 30 years after its discovery. One of the best targets is Seyfert 2 galaxy, Mrk 0003. This is because Mrk 0003 had the highest flux of neutral iron fluorescence after the performance verification targets. This observation will enable us to understand the origin of neutral iron fluorescence and investigate the relationship between the origin and X-ray luminosity.	NON-JET-DOMINATED AGN	2	C	ATSUSHI TANIMOTO		JAP	1	NOR	THE ORIGIN OF NEUTRAL IRON FLUORESCENCE IN THE RADIO-QUIET LUMINOUS SEYFERT 2 GALAXY MRK 0003	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201007010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
141	201079020	Perseus_M3	49.99973	41.42994	49.17266	41.24949	58.61997	22.24931	150.65367	-13.30911	262.87555	60726.20352	2025-02-20 04:53:04	60727.59796	2025-02-21 14:21:04	62.128	110.000	62.128	60.392	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		60.392	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-03-05 08:08:05	2026-03-07 00:00:00	2025-03-06 08:08:06	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012080	Feedback from Active Galactic Nuclei (AGN) is crucial for regulating cooling and star formation in galaxy clusters. Gas motions driven by the feedback could be important in heating the gas. We propose a multi-pointing observational program for the Perseus cluster, totaling 500 ks. We will study radial and azimuthal variations of gas kinematics and metallicity within the cluster core, mapping a transition between feedback- and mergers-dominated regions, which is crucial for distinguishing various feedback scenarios and revealing the role of turbulence in AGN feedback. We will probe gas sloshing, motions driven by rising bubbles, and turbulence association with the radio mini halo. These observations will be of legacy value, complementing large multi-wavelength data sets on Perseus.	GROUPS AND CLUSTERS OF GALAXIES	2	C	IRINA ZHURAVLEVA		USA	1	NOR	MAPPING GAS KINEMATICS IN THE X-RAY BRIGHTEST GALAXY CLUSTER	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201079020/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
142	201045020	SAGITTARIUS_B	266.8256	-28.37832	266.03477	-28.36098	267.19684	-4.96991	0.6684	-0.02554	88.70604	60725.28755	2025-02-19 06:54:04	60726.20352	2025-02-20 04:53:04	41.971	150.000	41.971	39.173	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		39.173	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-03-05 05:53:39	2026-04-05 00:00:00	2025-03-06 05:53:40	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011240	The Galactic center diffuse X-rays (GCXE) has been one of interesting mysteries in X-ray astronomy for 50 years. It is still under discussion whether the origin of the GCXE is ensemble of faint point sources or truly diffuse plasma. This XRISM observation will aim to the Sagittarius B and C regions in the Galactic center to perform measurement of dynamical motion and plasma diagnostics and to derive the diffuse plasma from the GCXE for the first time. The physical information (motion, temperature, ionization degree, mass, abundances) constrain production mechanism of the diffuse plasma (stellar wind, supernova, Sgr A*, etc). Contribution to the evolution of the Galaxy will be also discussed.	GALACTIC DIFFUSE EMISSION AND SURVEYS	2	A	MASAYOSHI NOBUKAWA		JAP	1	NOR	FIRST MEASUREMENT OF DYNAMICS AND PLASMA DIAGNOSTICS OF THE GALACTIC CENTER DIFFUSE X-RAYS	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201045020/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
143	201011010	IGR_J17091-3624	257.28158	-36.40766	256.4411	-36.34436	259.50383	-13.43064	349.52432	2.21243	91.34595	60724.19866	2025-02-18 04:46:04	60725.28755	2025-02-19 06:54:04	45.803	40.000	45.803	5.129	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	40.948	0.000	0.000	5.129	11110	313430	11310	PROCESSED	2025-02-27 04:43:01	2026-03-04 00:00:00	2025-02-28 04:43:01	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011083	We propose ToO observations of a Galactic transient black hole X-ray binary with a high inclination angle, during the state transition. Resolve high-resolution spectroscopy in the state where wind absorption lines have been observed enables us to obtain essential wind parameters (such as density, velocity, and the ionization stage) to determine the wind structure and launching mechanism. We also search for weak absorption and emission lines from the wind (and also jets) in the states where significant lines have rarely been observed in X-rays. Moreover, we have organized a multi-wavelength monitoring campaign simultaneously with the XRISM observations, from which we can achieve the whole picture of the evolution of the accretion disk, disk wind, and jets.	BH AND NS BINARIES	2	A	MEGUMI SHIDATSU		JAP	1	NOR-TOO	UNDERSTANDING EVOLUTION OF DISK WIND IN BLACK HOLE X-RAY BINARIES	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201011010/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
144	201045010	SAGITTARIUS_B	266.8258	-28.37853	266.03497	-28.36119	267.19703	-4.97011	0.66832	-0.0258	88.70603	60722.46185	2025-02-16 11:05:04	60724.19866	2025-02-18 04:46:04	76.132	150.000	76.132	69.613	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		69.613	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-02-22 14:19:13	2026-04-05 00:00:00	2025-02-23 14:19:14	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011240	The Galactic center diffuse X-rays (GCXE) has been one of interesting mysteries in X-ray astronomy for 50 years. It is still under discussion whether the origin of the GCXE is ensemble of faint point sources or truly diffuse plasma. This XRISM observation will aim to the Sagittarius B and C regions in the Galactic center to perform measurement of dynamical motion and plasma diagnostics and to derive the diffuse plasma from the GCXE for the first time. The physical information (motion, temperature, ionization degree, mass, abundances) constrain production mechanism of the diffuse plasma (stellar wind, supernova, Sgr A*, etc). Contribution to the evolution of the Galaxy will be also discussed.	GALACTIC DIFFUSE EMISSION AND SURVEYS	2	A	MASAYOSHI NOBUKAWA		JAP	1	NOR	FIRST MEASUREMENT OF DYNAMICS AND PLASMA DIAGNOSTICS OF THE GALACTIC CENTER DIFFUSE X-RAYS	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201045010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
145	201004010	GAMMA_CASSIOPEIAE	14.1806	60.71741	13.42216	60.44712	43.93378	48.81447	123.57851	-2.14771	223.95285	60721.16741	2025-02-15 04:01:04	60722.46185	2025-02-16 11:05:04	59.292	40.000	59.292	55.337	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	59.191	55.337	0.000	0.000	11110	313430	11310	PROCESSED	2025-03-20 15:58:57	2026-02-26 00:00:00	2025-02-23 12:27:17	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013002	Binary evolution is one of the most fundamental ingredients in astronomy. Binaries consisting of a high-mass star and a compact object constitute an important milestone in the evolution. Gamma Cas and its analogs could be the long-sought missing population of Be/WD binaries, though an alternative scenario exists. The two scenarios (a) Be/WD binary and (b) magnetic disk-star interaction on Be star surface differ most distinctively in the production site of the hard X-rays. We propose two straightforward and fully independent tests with Resolve to distinguish (a) and (b); the test 1 is the RV change of Fe lines as a function of the orbital phase. The test 2 is the line profile of the flurescent Fe Ka lines. Based on our PV experience, the two tests are only possible with Resolve.	ACCRETING WHITE DWARFS AND NOVAE	2	A	MASAHIRO TSUJIMOTO	SEAN GUNDERSON	JUS	1	NOR	SOLVING THE LONG-STANDING MYSTERY OF GAMMA CASSIOPEIAE WITH RESOLVE	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201004010/	WINDOW2	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
146	201036010	CIR_X-1	230.1686	-57.16715	229.19997	-56.98696	244.13233	-37.25036	322.11754	0.03783	103.57368	60719.27157	2025-02-13 06:31:04	60721.16741	2025-02-15 04:01:04	76.429	60.000	76.429	8.461	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	67.548	0.000	0.000	8.461	11110	313430	11310	PROCESSED	2025-02-19 12:37:56	2026-02-20 00:00:00	2025-02-20 12:37:57	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011196	In X-ray binaries, the presence of the excretion (outward) flow is theoretically envisioned as inevitable. The excretion flow has been entirely ignored despite its firm theoretical ground, but recent observations point toward the presence of it. Convincing evidence was obtained with the NICER observations of the neutron star binary Cir X-1. Physical properties of the excretion flow can be constrained with two high-resolution X-ray spectra taken at different orbital phases. The diagnostic requires a spectral resolution of R = E/DE ~ 10^3 in 2-8 keV band, which can only be achieved with Resolve. One of the two observations was already executed in the PV phase, and we propose the other one in the AO1 cycle, to verify the presence of the excretion flow.	BH AND NS BINARIES	2	A	NAGI ATSUCHI		JAP	1	NOR	ESTABLISHING THE PRESENCE OF EXCRETION FLOW IN X-RAY BINARIES WITH RESOLVE SPECTROSCOPY OF CIRCINUS X-1	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201036010/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
147	201079010	Perseus_M3	49.99998	41.43004	49.1729	41.24959	58.62019	22.24936	150.65377	-13.30893	262.8768	60717.92296	2025-02-11 22:09:04	60719.27157	2025-02-13 06:31:04	60.046	110.000	60.046	57.764	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		57.764	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-02-18 13:26:31	2026-03-07 00:00:00	2025-02-19 13:26:32	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012080	Feedback from Active Galactic Nuclei (AGN) is crucial for regulating cooling and star formation in galaxy clusters. Gas motions driven by the feedback could be important in heating the gas. We propose a multi-pointing observational program for the Perseus cluster, totaling 500 ks. We will study radial and azimuthal variations of gas kinematics and metallicity within the cluster core, mapping a transition between feedback- and mergers-dominated regions, which is crucial for distinguishing various feedback scenarios and revealing the role of turbulence in AGN feedback. We will probe gas sloshing, motions driven by rising bubbles, and turbulence association with the radio mini halo. These observations will be of legacy value, complementing large multi-wavelength data sets on Perseus.	GROUPS AND CLUSTERS OF GALAXIES	2	C	IRINA ZHURAVLEVA		USA	1	NOR	MAPPING GAS KINEMATICS IN THE X-RAY BRIGHTEST GALAXY CLUSTER	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201079010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
148	201064010	4U1700-37	255.98714	-37.84365	255.13716	-37.77422	258.58457	-14.95803	347.75509	2.17342	88.58698	60716.49032	2025-02-10 11:46:04	60717.92296	2025-02-11 22:09:04	58.720	50.000	58.720	49.984	PX_NORMAL	N	N	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	53.466	49.984	0.000	0.000	11110	313430	11310	PROCESSED	2025-02-18 11:33:13	2026-02-19 00:00:00	2025-02-19 11:33:14	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011343	We aim to study 4U 1700-377, a high-mass X-ray binary system, to better understand how matter behaves around its bright companion star and address the ``mass-gap'' mystery. Depending on its true nature, 4U 1700-377 could either be the heaviest neutron star without detected pulsations or the smallest black hole ever found. Using XRISM's detailed spectral analysis, we plan to measure the central energies and the profiles of the neutral and ionized iron lines with unprecedented accuracy.	BH AND NS BINARIES	2	B	SHINYA YAMADA		JAP	1	NOR	TOWARD IDENTIFYING 4U~1700-377 AS NEUTRON STAR OR BLACK HOLE	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201064010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
149	201116010	NGC1068	40.66964	-0.01351	40.02939	-0.2257	38.24482	-15.03722	172.10397	-51.93394	255.08992	60714.04241	2025-02-08 01:01:04	60716.49032	2025-02-10 11:46:04	114.990	100.000	114.990	112.816	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		112.816	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-02-17 07:57:01	2026-02-19 00:00:00	2025-02-18 07:57:02	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000014019	We propose a 100 ks XRISM observation of the Compton-thick AGN NGC1068, to serve as a benchmark for advancing the study of circumnuclear matter via high-resolution X-ray spectroscopy. The combination of XRISM and the already available broad-band (spectro-polarimetric) X-ray dataset, along with the possibility to extend the self-consistent modelling down to the sub-mm band, will offer an unprecedented view of the geometrical and physical properties of the torus. Moreover, the XRISM spectrum will allow us to measure the properties of the ionized gas and, together with existing soft X-ray high-resolution spectra, understand its origin. State-of-the-art models, developed or specifically adapted by members of the proposing team, will be crucial to leverage the potential of the XRISM spectrum.	NON-JET-DOMINATED AGN	2	A	STEFANO BIANCHI		EUR	1	NOR	NGC 1068: A XRISM BENCHMARK FOR COMPTON-THICK SEYFERT 2S	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201116010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
150	201020010	ABELL3395_SOUTH	96.70153	-54.54647	96.4492	-54.5146	108.31294	-77.5593	263.31153	-25.26554	221.74343	60709.15838	2025-02-03 03:48:04	60714.04241	2025-02-08 01:01:04	266.408	190.000	266.408	202.825	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		202.825	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-02-13 11:49:00	2026-02-14 00:00:00	2025-02-14 11:49:00	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011129	We propose conducting high-resolution spectroscopic observations of A3391/95, the unique triple galaxy cluster at z=0.05. Despite sharing a common large-scale structure, these clusters exhibit distinct merger stages and radio emissions, as revealed by eROSITA. Utilizing XRISM, we aim to accurately constrain bulk and turbulent motions at 150 and 200 km/s levels, respectively, and distinguish between the generation processes of gas motions attributed to AGN feedback and merger activity. Comparative analysis with multi-wavelength data and simulations will provide insights into the origins of gas motion and feedback processes within the cluster cores.	GROUPS AND CLUSTERS OF GALAXIES	2	C	NAOMI OTA		JAP	1	NOR	AGN-ICM INTERACTION IN THE INTERACTING CLUSTER SYSTEM A3391/95	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201020010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
151	201072010	GX301-2	186.65543	-62.76985	185.95571	-62.49304	221.51815	-52.62771	300.09754	-0.03475	132.46403	60707.79519	2025-02-01 19:05:04	60709.15838	2025-02-03 03:48:04	59.161	50.000	59.161	6.833	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	54.554	0.000	0.000	6.833	11110	313430	11310	PROCESSED	2025-02-07 08:00:25	2026-02-08 00:00:00	2025-02-08 08:00:25	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013008	We propose a 50 ks observation of the Compton-thick hypergiant X-ray Binary GX 301-2 during its regular pre-periastron flares. We will study the exact shape of the strong Fe K fluorescence line complex, the Fe K absorption edge, and the Compton shoulder profile. All these provide information on the ionization structure, temperature, column density and geometry of the absorbing material. We will also study the temporal variability of the Fe K lines and edge in 500s steps to probe the inhomogeneity of the stellar wind of the donor. This observation will therefore contribute to the construction of a self-consistent picture of the geometry and distribution of the reprocessing material in GX 301-2 and the interaction of the strong X-ray radiation with the dense wind of the stellar companion.	BH AND NS BINARIES	2	A	RALF BALLHAUSEN	YUTARO NAGAI	USJ	1	NOR	RESOLVING THE FE K FLUORESCENCE COMPLEX AND COMPTON SHOULDER IN GX 301-2 WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201072010/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
152	101019010	Perseus_CCD4_SPRING	49.82439	41.67507	48.99619	41.49397	58.55705	22.52119	150.40244	-13.17683	264.61163	60706.72088	2025-01-31 17:18:04	60707.79519	2025-02-01 19:05:04	50.195	40.000	50.195	48.392	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		48.392	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-02-04 12:33:34	2025-08-31 00:00:00	2025-02-05 12:33:34	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018002	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (2)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101019010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
153	101018010	Perseus_CCD3_SPRING	50.26381	41.70264	49.4342	41.52316	58.90661	22.45697	150.66766	-12.97264	264.61248	60705.79727	2025-01-30 19:08:04	60706.72088	2025-01-31 17:18:04	43.007	40.000	43.007	42.651	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		42.651	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-02-04 12:10:10	2025-08-31 00:00:00	2025-02-05 12:10:10	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018002	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (2)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101018010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
154	101017010	Perseus_CCD1_SPRING	50.2814	41.53168	49.45287	41.35227	58.86945	22.28898	150.77629	-13.10755	264.61234	60704.79241	2025-01-29 19:01:04	60705.79727	2025-01-30 19:08:04	44.975	40.000	44.975	44.907	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		44.907	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-02-04 11:59:02	2025-08-31 00:00:00	2025-02-05 11:59:02	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018002	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (2)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101017010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
155	101010010	Perseus_CAL2	49.95035	41.51181	49.12287	41.33118	58.60599	22.33822	150.57554	-13.26126	264.59656	60703.87574	2025-01-28 21:01:04	60704.79241	2025-01-29 19:01:04	42.808	40.000	42.808	39.260	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	41.994	39.260	0.000	0.000	11110	313430	11310	PROCESSED	2025-02-04 11:26:51	2025-08-31 00:00:00	2025-02-05 11:26:51	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101010010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
156	101009010	Perseus_CAL1	49.95037	41.51185	49.12289	41.33122	58.60602	22.33825	150.57554	-13.26122	264.61333	60702.79657	2025-01-27 19:07:04	60703.87574	2025-01-28 21:01:04	46.783	40.000	46.783	46.620	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		46.620	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-02-04 12:28:23	2025-08-31 00:00:00	2025-02-05 12:28:23	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101009010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
157	201087010	ABELL1795_CENTER	207.21837	26.59235	206.64113	26.84052	193.9269	34.98707	33.80627	77.18603	90.00215	60697.78685	2025-01-22 18:53:04	60702.79657	2025-01-27 19:07:04	225.682	200.000	225.682	217.485	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		217.485	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-31 13:54:29	2026-02-01 00:00:00	2025-02-01 13:54:29	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013010	We propose two XRISM Resolve pointings toward the bright cool-core cluster Abell 1795, one centered on the cluster and one offset 3 arcmin (220 kpc) to the north, with a primary goal of measuring the line-of-sight bulk motion and velocity broadening inside the disturbed central region and in a more relaxed region outside the core. These observations will also provide an initial baseline for future long observations to measure turbulence out to larger radius; probe the effects of gas dynamics on the distribution of metals in the ICM; and provide a deep Xtend observation to measure thermodynamic profiles out to R200.	GROUPS AND CLUSTERS OF GALAXIES	2	A	ERIC MILLER	YUTAKA FUJITA	USJ	1	NOR	RESOLVING THE ICM VELOCITY STRUCTURE OF ABELL 1795 WITH XRISM	processed	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201087010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
158	201088010	ABELL1795_NORTH	207.21804	26.64328	206.64094	26.89144	193.89973	35.03288	34.03473	77.19123	90.00117	60695.18963	2025-01-20 04:33:04	60697.78685	2025-01-22 18:53:04	113.363	100.000	113.363	114.904	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		114.904	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-28 11:49:49	2026-01-30 00:00:00	2025-01-29 11:49:50	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013010	We propose two XRISM Resolve pointings toward the bright cool-core cluster Abell 1795, one centered on the cluster and one offset 3 arcmin (220 kpc) to the north, with a primary goal of measuring the line-of-sight bulk motion and velocity broadening inside the disturbed central region and in a more relaxed region outside the core. These observations will also provide an initial baseline for future long observations to measure turbulence out to larger radius; probe the effects of gas dynamics on the distribution of metals in the ICM; and provide a deep Xtend observation to measure thermodynamic profiles out to R200.	GROUPS AND CLUSTERS OF GALAXIES	2	A	ERIC MILLER	YUTAKA FUJITA	USJ	1	NOR	RESOLVING THE ICM VELOCITY STRUCTURE OF ABELL 1795 WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201088010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
159	201093010	A1914	216.50033	37.82636	215.98792	38.05083	196.42071	48.55189	67.20656	67.46162	109.33804	60692.67019	2025-01-17 16:05:04	60695.18963	2025-01-20 04:33:04	111.751	100.000	111.751	116.493	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		116.493	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-24 10:38:22	2026-01-29 00:00:00	2025-01-25 10:38:23	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012133	Velocity power spectra (PS) of the ICM are necessary for testing multi-scale physics in numerical simulations and measuring turbulent dissipation/plasma properties. XRISM allows direct studies of ICM kinematics, but the large PSF makes it challenging to extract PS. However, by combining high-resolution imaging and spectroscopic missions, one can calibrate indirect methods of measuring PS. We aim to test the relation between turbulent Mach numbers measured with XRISM and ICM density fluctuations probed with Chandra by observing two clusters, A2034/A1914, with 120/100 ks exposures. These clusters have dissimilar fluctuations measured over a wide scale range, which is ideal for our goal. This calibration will provide a robust method to measure velocity PS and probe ICM transport properties.	GROUPS AND CLUSTERS OF GALAXIES	2	B	IRINA ZHURAVLEVA		USA	1	NOR	COMBINING XRISM AND CHANDRA FOR ROBUST VELOCITY POWER SPECTRA MEASUREMENTS IN THE ICM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201093010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
160	201114010	COMA_OFFSET_N	194.94136	28.04897	194.33839	28.31829	181.45946	31.46227	59.93018	87.93793	105.84454	60689.45560	2025-01-14 10:56:04	60692.67019	2025-01-17 16:05:04	144.847	135.000	144.847	148.103	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		148.103	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-21 15:49:25	2026-01-23 00:00:00	2025-01-22 15:49:26	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000014004	Though crucial for cluster physics, direct measurements of the intracluster medium (ICM) velocity structure are scarce. Recent advancements have enabled ICM velocity measurements in various clusters using the XMM-Newton EPIC-pn instrument. This employs Cu Ka line for recalibration. In the Coma cluster, distinct velocities, likely linked to subgroup mergers, have been identified. To explore further, the exceptional capabilities of the XRISM instruments are vital. Hence, we propose a 135 ks observation of the Coma cluster to map its ICM velocity structure and investigate potential merging scenarios.	GROUPS AND CLUSTERS OF GALAXIES	2	B	EFRAIN GATUZZ		EUR	1	NOR	ICM VELOCITY STRUCTURE UNVEILED: THE COMA CLUSTER MERGING NATURE	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201114010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
161	201109010	WR140	305.11785	43.85413	304.69581	43.69484	327.37156	60.49126	80.93046	4.17613	189.85852	60687.62921	2025-01-12 15:06:04	60689.45560	2025-01-14 10:56:04	80.792	65.000	80.792	75.260	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	80.501	75.260	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-21 12:02:55	2026-01-22 00:00:00	2025-01-22 12:02:55	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012182	Cosmic dust is a primary building block of the Earth, and its formation is a fundamental question. The massive colliding wind binary system, WR140, produces massive dust near periastron of its 7.9-year-long orbit. During the dust emission rise in previous binary cycles, the CIII line excess enhanced, and the X-ray emission declined oppositely, suggesting strong cooling of the WWC plasma produced a condition for dust formation. The star experiences another periastron passage on November 22nd, 2024. We propose 3 XRISM observations around that time to study the location and motion of the WWC plasma using the Fe XXV emission line. We also expect to detect the fluorescent Fe line, which strongly constrains the distance of the WWC apex from the stellar surface.	STELLAR CORONAE, WINDS, AND YOUNG STARS	2	A	KENJI HAMAGUCHI		USA	1	NOR	DYNAMICS OF THE EXPLOSIVE DUST FORMATION NEAR PERIASTRON IN WR140	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201109010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
162	201023010	ABELL3571_S	206.86602	-32.8884	206.14536	-32.63922	216.98423	-20.31914	316.30675	28.52409	90.00222	60684.51394	2025-01-09 12:20:04	60687.62921	2025-01-12 15:06:04	174.630	130.000	174.630	155.655	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		155.655	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-20 11:33:49	2026-01-22 00:00:00	2025-01-21 11:33:50	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013005	We propose three pointing observations of A3571: a south-pointing (S, 130 ks) to cover the southern cold front, a north-pointing (N, 110 ks) to include the northern jump in the surface brightness, and east pointing (E, 40 ks). This cluster does not exhibit signs of a cool core, presenting a unique opportunity to explore the influence of sloshing motions, avoiding the complexities associated with active galactic nuclei. We aim to investigate the thermodynamic properties of A3571's core regions by analyzing gas motions, temperature, and metal abundance distributions. Additionally, we plan to measure the Ni/Fe ratio to study the progenitor population of SN Ia.	GROUPS AND CLUSTERS OF GALAXIES	2	B	KYOKO MATSUSHITA	IRINA ZHURAVLEVA	JUS	1	NOR	EXPLORING THE EFFECTS OF SLOSHING MOTIONS ON ICM DYNAMICS IN ABELL 3571	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201023010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
163	201024010	ABELL3571_N	206.86576	-32.83701	206.14526	-32.58783	216.96328	-20.27165	316.32085	28.57396	90.00337	60681.77991	2025-01-06 18:43:04	60684.51394	2025-01-09 12:20:04	137.428	110.000	137.428	122.808	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		122.808	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-15 14:44:14	2026-01-22 00:00:00	2025-01-16 14:44:14	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013005	We propose three pointing observations of A3571: a south-pointing (S, 130 ks) to cover the southern cold front, a north-pointing (N, 110 ks) to include the northern jump in the surface brightness, and east pointing (E, 40 ks). This cluster does not exhibit signs of a cool core, presenting a unique opportunity to explore the influence of sloshing motions, avoiding the complexities associated with active galactic nuclei. We aim to investigate the thermodynamic properties of A3571's core regions by analyzing gas motions, temperature, and metal abundance distributions. Additionally, we plan to measure the Ni/Fe ratio to study the progenitor population of SN Ia.	GROUPS AND CLUSTERS OF GALAXIES	2	B	KYOKO MATSUSHITA	IRINA ZHURAVLEVA	JUS	1	NOR	EXPLORING THE EFFECTS OF SLOSHING MOTIONS ON ICM DYNAMICS IN ABELL 3571	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201024010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
164	101004010	3C273	187.27808	2.05348	186.63871	2.32982	185.86922	4.77457	289.95074	64.36108	112.45128	60680.93824	2025-01-05 22:31:04	60681.77991	2025-01-06 18:43:04	35.437	30.000	35.437	32.295	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	31100010	320000A0	34.591	32.295	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-15 11:22:52	2025-08-31 00:00:00	2025-01-16 11:22:53	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101004010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
165	201025010	ABELL3571_E	206.92752	-32.85464	206.20679	-32.60559	217.02159	-20.26835	316.37318	28.54412	90.00216	60679.39935	2025-01-04 09:35:04	60680.93824	2025-01-05 22:31:04	72.368	60.000	72.368	68.631	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		68.631	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-16 19:40:09	2026-01-22 00:00:00	2025-01-17 19:40:09	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013005	We propose three pointing observations of A3571: a south-pointing (S, 130 ks) to cover the southern cold front, a north-pointing (N, 110 ks) to include the northern jump in the surface brightness, and east pointing (E, 40 ks). This cluster does not exhibit signs of a cool core, presenting a unique opportunity to explore the influence of sloshing motions, avoiding the complexities associated with active galactic nuclei. We aim to investigate the thermodynamic properties of A3571's core regions by analyzing gas motions, temperature, and metal abundance distributions. Additionally, we plan to measure the Ni/Fe ratio to study the progenitor population of SN Ia.	GROUPS AND CLUSTERS OF GALAXIES	2	B	KYOKO MATSUSHITA	IRINA ZHURAVLEVA	JUS	1	NOR	EXPLORING THE EFFECTS OF SLOSHING MOTIONS ON ICM DYNAMICS IN ABELL 3571	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201025010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
166	201095010	ABELL3571	206.86605	-32.85329	206.14549	-32.6041	216.97008	-20.28663	316.31658	28.55812	90.00424	60674.96463	2024-12-30 23:09:04	60679.39935	2025-01-04 09:35:04	192.136	165.000	192.136	173.606	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		173.650	0.042	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-08 15:38:59	2026-01-11 00:00:00	2025-01-09 15:39:00	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013005	We propose three pointing observations of A3571: a south-pointing (S, 130 ks) to cover the southern cold front, a north-pointing (N, 110 ks) to include the northern jump in the surface brightness, and east pointing (E, 40 ks). This cluster does not exhibit signs of a cool core, presenting a unique opportunity to explore the influence of sloshing motions, avoiding the complexities associated with active galactic nuclei. We aim to investigate the thermodynamic properties of A3571's core regions by analyzing gas motions, temperature, and metal abundance distributions. Additionally, we plan to measure the Ni/Fe ratio to study the progenitor population of SN Ia.	GROUPS AND CLUSTERS OF GALAXIES	2	B	KYOKO MATSUSHITA	IRINA ZHURAVLEVA	JUS	1	NOR	EXPLORING THE EFFECTS OF SLOSHING MOTIONS ON ICM DYNAMICS IN ABELL 3571	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201095010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
167	201076090	NGC4151	182.63393	39.40703	182.00258	39.68514	164.09467	36.62426	155.07852	75.06128	109.5996	60674.00838	2024-12-30 00:12:04	60674.96463	2024-12-30 23:09:04	43.618	40.000	43.618	35.097	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	37.542	35.097	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-04 10:35:13	2026-01-09 00:00:00	2025-01-05 10:35:13	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012061	Optical broad line reverberation mapping of Seyferts has helped the field to understand the geometry of accretion onto massive black holes, and to measure black hole masses. Now, XRISM observations of NGC 4151 during the PV phase have resolved specific line components that may reveal even more. We request a total of 360 ks in 9 exposures in XRISM Cycle 1 to undertake a pioneering simultaneous X-ray and optical reverberation lag study of NGC 4151. Building on key prior results, we demonstrate that modest observations will achieve the sensitivity needed to detect a reverberation lag in X-rays. This is the first step to understanding the relative geometry of the X-ray and optical components of the broad line region, and weighing massive black holes in X-rays.	NON-JET-DOMINATED AGN	2	A	JON MILLER		USA	1	NOR	REVERBERATION IN NGC 4151 WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201076090/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
168	201003010	GAMMA_CASSIOPEIAE	14.17804	60.71654	13.41962	60.44625	43.93146	48.8145	123.57728	-2.1486	272.49417	60673.18407	2024-12-29 04:25:04	60674.00838	2024-12-30 00:12:04	34.392	40.000	34.392	35.037	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	37.477	35.037	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-04 09:27:51	2026-01-09 00:00:00	2025-01-05 09:27:51	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013002	Binary evolution is one of the most fundamental ingredients in astronomy. Binaries consisting of a high-mass star and a compact object constitute an important milestone in the evolution. Gamma Cas and its analogs could be the long-sought missing population of Be/WD binaries, though an alternative scenario exists. The two scenarios (a) Be/WD binary and (b) magnetic disk-star interaction on Be star surface differ most distinctively in the production site of the hard X-rays. We propose two straightforward and fully independent tests with Resolve to distinguish (a) and (b); the test 1 is the RV change of Fe lines as a function of the orbital phase. The test 2 is the line profile of the flurescent Fe Ka lines. Based on our PV experience, the two tests are only possible with Resolve.	ACCRETING WHITE DWARFS AND NOVAE	2	A	MASAHIRO TSUJIMOTO	SEAN GUNDERSON	JUS	1	NOR	SOLVING THE LONG-STANDING MYSTERY OF GAMMA CASSIOPEIAE WITH RESOLVE	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201003010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
169	201076080	NGC4151	182.63364	39.40708	182.00229	39.68519	164.0944	36.62419	155.0791	75.0611	109.59922	60672.28269	2024-12-28 06:47:04	60673.18407	2024-12-29 04:25:04	42.447	40.000	42.447	33.718	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	36.067	33.718	0.000	0.000	11110	313430	11310	PROCESSED	2025-01-04 09:42:02	2026-01-09 00:00:00	2025-01-05 09:42:02	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012061	Optical broad line reverberation mapping of Seyferts has helped the field to understand the geometry of accretion onto massive black holes, and to measure black hole masses. Now, XRISM observations of NGC 4151 during the PV phase have resolved specific line components that may reveal even more. We request a total of 360 ks in 9 exposures in XRISM Cycle 1 to undertake a pioneering simultaneous X-ray and optical reverberation lag study of NGC 4151. Building on key prior results, we demonstrate that modest observations will achieve the sensitivity needed to detect a reverberation lag in X-rays. This is the first step to understanding the relative geometry of the X-ray and optical components of the broad line region, and weighing massive black holes in X-rays.	NON-JET-DOMINATED AGN	2	A	JON MILLER		USA	1	NOR	REVERBERATION IN NGC 4151 WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201076080/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
170	201110050	NGC7212	331.7557	10.23123	331.13869	9.98669	337.63947	20.37798	70.41919	-35.37798	240.16341	60671.50769	2024-12-27 12:11:04	60672.28269	2024-12-28 06:47:04	32.699	220.000	32.699	32.898	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		32.898	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-31 10:41:53	2026-01-03 00:00:00	2025-01-01 10:41:54	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012190	The nearby (z~0.0266) Compton thick AGN NGC 7212 is, to our knowledge, the first AGN with a detection of vanadium via X-ray spectroscopy. Vanadium is a short-lived intermediate product of the spallation of iron by cosmic rays. Its presence in the narrow line region suggests ongoing strong cosmic ray feedback, and the likelihood that the energy range between 4.5 keV and iron K-alpha is likely to be dominated by more stable He-like and H-like products of spallation (such as titanium, chromium and manganese). Only XRISM has the sensitivity and resolution to measure these lines. This would have deep and consequential implications for the "hard continuum" between 2-6 keV. We will also model extended hot feedback in conjunction with archival Chandra data.	NON-JET-DOMINATED AGN	2	B	WALTER MAKSYM		USA	1	NOR	COSMIC RAY SPALLATION AND THE ENIGMATIC EXTENDED NARROW LINE REGION OF NGC 7212	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201110050/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
171	201076070	NGC4151	182.6337	39.40694	182.00235	39.68506	164.09453	36.6241	155.07927	75.06124	109.59897	60670.42505	2024-12-26 10:12:04	60671.50769	2024-12-27 12:11:04	46.888	40.000	46.888	39.128	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	41.853	39.128	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-31 10:20:36	2026-01-03 00:00:00	2025-01-01 10:20:36	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012061	Optical broad line reverberation mapping of Seyferts has helped the field to understand the geometry of accretion onto massive black holes, and to measure black hole masses. Now, XRISM observations of NGC 4151 during the PV phase have resolved specific line components that may reveal even more. We request a total of 360 ks in 9 exposures in XRISM Cycle 1 to undertake a pioneering simultaneous X-ray and optical reverberation lag study of NGC 4151. Building on key prior results, we demonstrate that modest observations will achieve the sensitivity needed to detect a reverberation lag in X-rays. This is the first step to understanding the relative geometry of the X-ray and optical components of the broad line region, and weighing massive black holes in X-rays.	NON-JET-DOMINATED AGN	2	A	JON MILLER		USA	1	NOR	REVERBERATION IN NGC 4151 WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201076070/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
172	201110040	NGC7212	331.75588	10.23129	331.13887	9.98675	337.63966	20.37797	70.41939	-35.37806	240.16352	60669.06116	2024-12-25 01:28:04	60670.42505	2024-12-26 10:12:04	62.005	220.000	62.005	61.383	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		61.383	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-31 10:51:05	2026-01-03 00:00:00	2025-01-01 10:51:05	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012190	The nearby (z~0.0266) Compton thick AGN NGC 7212 is, to our knowledge, the first AGN with a detection of vanadium via X-ray spectroscopy. Vanadium is a short-lived intermediate product of the spallation of iron by cosmic rays. Its presence in the narrow line region suggests ongoing strong cosmic ray feedback, and the likelihood that the energy range between 4.5 keV and iron K-alpha is likely to be dominated by more stable He-like and H-like products of spallation (such as titanium, chromium and manganese). Only XRISM has the sensitivity and resolution to measure these lines. This would have deep and consequential implications for the "hard continuum" between 2-6 keV. We will also model extended hot feedback in conjunction with archival Chandra data.	NON-JET-DOMINATED AGN	2	B	WALTER MAKSYM		USA	1	NOR	COSMIC RAY SPALLATION AND THE ENIGMATIC EXTENDED NARROW LINE REGION OF NGC 7212	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201110040/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
173	201076060	NGC4151	182.63421	39.4068	182.00286	39.68491	164.09504	36.62417	155.0784	75.06159	109.59883	60667.96602	2024-12-23 23:11:04	60669.06116	2024-12-25 01:28:04	51.645	40.000	51.645	40.435	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	43.251	40.435	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-31 09:55:20	2026-01-03 00:00:00	2025-01-01 09:55:20	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012061	Optical broad line reverberation mapping of Seyferts has helped the field to understand the geometry of accretion onto massive black holes, and to measure black hole masses. Now, XRISM observations of NGC 4151 during the PV phase have resolved specific line components that may reveal even more. We request a total of 360 ks in 9 exposures in XRISM Cycle 1 to undertake a pioneering simultaneous X-ray and optical reverberation lag study of NGC 4151. Building on key prior results, we demonstrate that modest observations will achieve the sensitivity needed to detect a reverberation lag in X-rays. This is the first step to understanding the relative geometry of the X-ray and optical components of the broad line region, and weighing massive black holes in X-rays.	NON-JET-DOMINATED AGN	2	A	JON MILLER		USA	1	NOR	REVERBERATION IN NGC 4151 WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201076060/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
174	201110030	NGC7212	331.7558	10.23123	331.13879	9.98669	337.63957	20.37795	70.41928	-35.37805	240.16327	60666.99727	2024-12-22 23:56:04	60667.96602	2024-12-23 23:11:04	41.742	220.000	41.742	43.380	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		43.380	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-28 11:51:37	2026-01-03 00:00:00	2024-12-29 11:51:37	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012190	The nearby (z~0.0266) Compton thick AGN NGC 7212 is, to our knowledge, the first AGN with a detection of vanadium via X-ray spectroscopy. Vanadium is a short-lived intermediate product of the spallation of iron by cosmic rays. Its presence in the narrow line region suggests ongoing strong cosmic ray feedback, and the likelihood that the energy range between 4.5 keV and iron K-alpha is likely to be dominated by more stable He-like and H-like products of spallation (such as titanium, chromium and manganese). Only XRISM has the sensitivity and resolution to measure these lines. This would have deep and consequential implications for the "hard continuum" between 2-6 keV. We will also model extended hot feedback in conjunction with archival Chandra data.	NON-JET-DOMINATED AGN	2	B	WALTER MAKSYM		USA	1	NOR	COSMIC RAY SPALLATION AND THE ENIGMATIC EXTENDED NARROW LINE REGION OF NGC 7212	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201110030/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
175	201076050	NGC4151	182.6348	39.4066	182.00346	39.68471	164.09566	36.62422	155.07749	75.06203	109.59865	60665.77574	2024-12-21 18:37:04	60666.99727	2024-12-22 23:56:04	59.582	40.000	59.582	49.878	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	53.348	49.878	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-28 11:37:24	2026-01-01 00:00:00	2024-12-29 11:37:25	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012061	Optical broad line reverberation mapping of Seyferts has helped the field to understand the geometry of accretion onto massive black holes, and to measure black hole masses. Now, XRISM observations of NGC 4151 during the PV phase have resolved specific line components that may reveal even more. We request a total of 360 ks in 9 exposures in XRISM Cycle 1 to undertake a pioneering simultaneous X-ray and optical reverberation lag study of NGC 4151. Building on key prior results, we demonstrate that modest observations will achieve the sensitivity needed to detect a reverberation lag in X-rays. This is the first step to understanding the relative geometry of the X-ray and optical components of the broad line region, and weighing massive black holes in X-rays.	NON-JET-DOMINATED AGN	2	A	JON MILLER		USA	1	NOR	REVERBERATION IN NGC 4151 WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201076050/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
176	201096030	G292_NW	171.09097	-59.22481	170.52464	-58.94991	208.02501	-55.06515	291.98795	1.78418	90.00035	60664.77435	2024-12-20 18:35:04	60665.77574	2024-12-21 18:37:04	38.609	100.000	38.609	34.330	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		34.330	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-24 09:38:34	2025-12-27 00:00:00	2024-12-25 09:38:35	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012146	The composition and dynamics of supernova remnants inform us on the explosion mechanism of the supernova and the evolution of the progenitor. The Galactic remnant G292.0+1.8 is an evolved remnant rich in emission from shocked ejecta and circumstellar material. It is also bright in [OIII] emission from shocked, fast moving ejecta which have velocities in excess of 2500 km/s. Here we propose for two 100ks observations of G292 in order to investigate the properties of the explosion and nucleosynthesis. Our proposed program will be complemented by a ground based spectroscopic survey to map the 3D structure of the ejecta in order to further understand the properties of the explosion.	SUPERNOVA REMNANTS	2	B	DANIEL PATNAUDE		USA	1	NOR	THE PROGENITOR AND EXPLOSION PROPERTIES OF G292.0+1.8	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201096030/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
177	201076040	NGC4151	182.63459	39.40638	182.00324	39.68449	164.09562	36.62394	155.07852	75.0621	109.59909	60663.44935	2024-12-19 10:47:04	60664.77435	2024-12-20 18:35:04	69.862	40.000	69.862	55.750	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	59.632	55.750	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-24 09:03:43	2025-12-27 00:00:00	2024-12-25 09:03:43	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012061	Optical broad line reverberation mapping of Seyferts has helped the field to understand the geometry of accretion onto massive black holes, and to measure black hole masses. Now, XRISM observations of NGC 4151 during the PV phase have resolved specific line components that may reveal even more. We request a total of 360 ks in 9 exposures in XRISM Cycle 1 to undertake a pioneering simultaneous X-ray and optical reverberation lag study of NGC 4151. Building on key prior results, we demonstrate that modest observations will achieve the sensitivity needed to detect a reverberation lag in X-rays. This is the first step to understanding the relative geometry of the X-ray and optical components of the broad line region, and weighing massive black holes in X-rays.	NON-JET-DOMINATED AGN	2	A	JON MILLER		USA	1	NOR	REVERBERATION IN NGC 4151 WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201076040/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
178	201110020	NGC7212	331.75557	10.23122	331.13856	9.98668	337.63933	20.37802	70.41907	-35.37789	240.16308	60662.47921	2024-12-18 11:30:04	60663.44935	2024-12-19 10:47:04	43.805	220.000	43.805	42.353	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		42.353	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-24 09:17:03	2026-01-03 00:00:00	2024-12-25 09:17:04	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012190	The nearby (z~0.0266) Compton thick AGN NGC 7212 is, to our knowledge, the first AGN with a detection of vanadium via X-ray spectroscopy. Vanadium is a short-lived intermediate product of the spallation of iron by cosmic rays. Its presence in the narrow line region suggests ongoing strong cosmic ray feedback, and the likelihood that the energy range between 4.5 keV and iron K-alpha is likely to be dominated by more stable He-like and H-like products of spallation (such as titanium, chromium and manganese). Only XRISM has the sensitivity and resolution to measure these lines. This would have deep and consequential implications for the "hard continuum" between 2-6 keV. We will also model extended hot feedback in conjunction with archival Chandra data.	NON-JET-DOMINATED AGN	2	B	WALTER MAKSYM		USA	1	NOR	COSMIC RAY SPALLATION AND THE ENIGMATIC EXTENDED NARROW LINE REGION OF NGC 7212	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201110020/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
179	201076030	NGC4151	182.63453	39.40632	182.00318	39.68444	164.0956	36.62387	155.07879	75.06212	109.59853	60661.12574	2024-12-17 03:01:04	60662.47921	2024-12-18 11:30:04	68.700	40.000	68.700	53.599	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	57.332	53.599	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-24 08:53:32	2025-12-27 00:00:00	2024-12-25 08:53:32	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012061	Optical broad line reverberation mapping of Seyferts has helped the field to understand the geometry of accretion onto massive black holes, and to measure black hole masses. Now, XRISM observations of NGC 4151 during the PV phase have resolved specific line components that may reveal even more. We request a total of 360 ks in 9 exposures in XRISM Cycle 1 to undertake a pioneering simultaneous X-ray and optical reverberation lag study of NGC 4151. Building on key prior results, we demonstrate that modest observations will achieve the sensitivity needed to detect a reverberation lag in X-rays. This is the first step to understanding the relative geometry of the X-ray and optical components of the broad line region, and weighing massive black holes in X-rays.	NON-JET-DOMINATED AGN	2	A	JON MILLER		USA	1	NOR	REVERBERATION IN NGC 4151 WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201076030/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
180	201096020	G292_NW	171.09117	-59.22475	170.52484	-58.94985	208.02507	-55.06503	291.98802	1.78427	90.00092	60660.06255	2024-12-16 01:30:04	60661.12574	2024-12-17 03:01:04	40.152	100.000	40.152	38.104	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		38.104	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-23 09:39:33	2025-12-27 00:00:00	2024-12-24 09:39:33	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012146	The composition and dynamics of supernova remnants inform us on the explosion mechanism of the supernova and the evolution of the progenitor. The Galactic remnant G292.0+1.8 is an evolved remnant rich in emission from shocked ejecta and circumstellar material. It is also bright in [OIII] emission from shocked, fast moving ejecta which have velocities in excess of 2500 km/s. Here we propose for two 100ks observations of G292 in order to investigate the properties of the explosion and nucleosynthesis. Our proposed program will be complemented by a ground based spectroscopic survey to map the 3D structure of the ejecta in order to further understand the properties of the explosion.	SUPERNOVA REMNANTS	2	B	DANIEL PATNAUDE		USA	1	NOR	THE PROGENITOR AND EXPLOSION PROPERTIES OF G292.0+1.8	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201096020/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
181	201076020	NGC4151	182.63456	39.40659	182.00321	39.6847	164.09546	36.62412	155.07808	75.06192	109.59849	60658.99657	2024-12-14 23:55:04	60660.06255	2024-12-16 01:30:04	55.921	40.000	55.921	45.360	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	48.520	45.360	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-23 08:37:00	2025-12-27 00:00:00	2024-12-24 08:37:00	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012061	Optical broad line reverberation mapping of Seyferts has helped the field to understand the geometry of accretion onto massive black holes, and to measure black hole masses. Now, XRISM observations of NGC 4151 during the PV phase have resolved specific line components that may reveal even more. We request a total of 360 ks in 9 exposures in XRISM Cycle 1 to undertake a pioneering simultaneous X-ray and optical reverberation lag study of NGC 4151. Building on key prior results, we demonstrate that modest observations will achieve the sensitivity needed to detect a reverberation lag in X-rays. This is the first step to understanding the relative geometry of the X-ray and optical components of the broad line region, and weighing massive black holes in X-rays.	NON-JET-DOMINATED AGN	2	A	JON MILLER		USA	1	NOR	REVERBERATION IN NGC 4151 WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201076020/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
182	201096010	G292_NW	171.09108	-59.22479	170.52475	-58.94989	208.02507	-55.0651	291.988	1.78422	90.00138	60657.93824	2024-12-13 22:31:04	60658.99657	2024-12-14 23:55:04	40.600	100.000	40.600	38.711	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		38.711	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-23 09:10:14	2025-12-27 00:00:00	2024-12-24 09:10:14	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012146	The composition and dynamics of supernova remnants inform us on the explosion mechanism of the supernova and the evolution of the progenitor. The Galactic remnant G292.0+1.8 is an evolved remnant rich in emission from shocked ejecta and circumstellar material. It is also bright in [OIII] emission from shocked, fast moving ejecta which have velocities in excess of 2500 km/s. Here we propose for two 100ks observations of G292 in order to investigate the properties of the explosion and nucleosynthesis. Our proposed program will be complemented by a ground based spectroscopic survey to map the 3D structure of the ejecta in order to further understand the properties of the explosion.	SUPERNOVA REMNANTS	2	B	DANIEL PATNAUDE		USA	1	NOR	THE PROGENITOR AND EXPLOSION PROPERTIES OF G292.0+1.8	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201096010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
183	201076010	NGC4151	182.63471	39.40655	182.00337	39.68466	164.09562	36.62414	155.0778	75.06203	109.59817	60656.80560	2024-12-12 19:20:04	60657.93824	2024-12-13 22:31:04	55.393	40.000	55.393	47.193	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	50.477	47.193	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-21 07:00:24	2025-12-27 00:00:00	2024-12-22 07:00:24	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012061	Optical broad line reverberation mapping of Seyferts has helped the field to understand the geometry of accretion onto massive black holes, and to measure black hole masses. Now, XRISM observations of NGC 4151 during the PV phase have resolved specific line components that may reveal even more. We request a total of 360 ks in 9 exposures in XRISM Cycle 1 to undertake a pioneering simultaneous X-ray and optical reverberation lag study of NGC 4151. Building on key prior results, we demonstrate that modest observations will achieve the sensitivity needed to detect a reverberation lag in X-rays. This is the first step to understanding the relative geometry of the X-ray and optical components of the broad line region, and weighing massive black holes in X-rays.	NON-JET-DOMINATED AGN	2	A	JON MILLER		USA	1	NOR	REVERBERATION IN NGC 4151 WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201076010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
184	201110010	NGC7212	331.75588	10.23109	331.13888	9.98655	337.63959	20.37779	70.41922	-35.37821	240.16305	60655.10838	2024-12-11 02:36:04	60656.80560	2024-12-12 19:20:04	71.075	220.000	71.075	67.269	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		67.269	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-21 08:50:44	2026-01-03 00:00:00	2024-12-22 08:50:44	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012190	The nearby (z~0.0266) Compton thick AGN NGC 7212 is, to our knowledge, the first AGN with a detection of vanadium via X-ray spectroscopy. Vanadium is a short-lived intermediate product of the spallation of iron by cosmic rays. Its presence in the narrow line region suggests ongoing strong cosmic ray feedback, and the likelihood that the energy range between 4.5 keV and iron K-alpha is likely to be dominated by more stable He-like and H-like products of spallation (such as titanium, chromium and manganese). Only XRISM has the sensitivity and resolution to measure these lines. This would have deep and consequential implications for the "hard continuum" between 2-6 keV. We will also model extended hot feedback in conjunction with archival Chandra data.	NON-JET-DOMINATED AGN	2	B	WALTER MAKSYM		USA	1	NOR	COSMIC RAY SPALLATION AND THE ENIGMATIC EXTENDED NARROW LINE REGION OF NGC 7212	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201110010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
185	300017020	M87_SW_ARM	187.66044	12.35797	187.02767	12.63407	182.03129	14.36832	283.65656	74.44621	120.27824	60653.09866	2024-12-09 02:22:04	60655.10838	2024-12-11 02:36:04	82.049	72.000	82.049	79.890	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		79.890	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-21 09:12:59	2025-12-27 00:00:00	2024-12-22 09:12:59	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000035	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.	GROUPS AND CLUSTERS OF GALAXIES	3	A	XRISM Collaboration		JAP	0	NOR	SUPERMASSIVE BLACK HOLE FEEDBACK IN M87	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300017020/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
186	201063010	NGC4388	186.44428	12.6629	185.81037	12.93968	180.7843	14.1632	279.11812	74.336	103.00075	60648.78477	2024-12-04 18:50:04	60653.09866	2024-12-09 02:22:04	182.548	160.000	182.548	168.404	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	180.133	168.404	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-16 07:29:18	2025-12-24 00:00:00	2024-12-17 07:29:19	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011336	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-K 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.	NON-JET-DOMINATED AGN	2	A	YOSHIHIRO UEDA		JAP	1	NOR	RESOLVING CIRCUMNUCLEAR STRUCTURE IN SEYFERT 2 GALAXY NGC 4388	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201063010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
187	201065010	PG1211+143	183.57325	14.05474	182.9366	14.33266	177.56745	14.29169	267.54869	74.31575	118.51646	60643.66046	2024-11-29 15:51:04	60648.78477	2024-12-04 18:50:04	226.822	200.000	226.822	221.382	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		221.382	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-13 13:50:58	2025-12-17 00:00:00	2024-12-14 13:50:59	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013012	The nearby QSO, PG 1211+143, is one of the first known prototypes of the ultra fast outflows (UFOs). It has a deep, blue-shifted Fe K absorption trough, which can be modeled by a fast wind with an outflow velocity of 0.1c. It has an extensive soft X-ray UFO, as revealed by multiple absorption lines measured by XMM/RGS and Chandra/HETG and hosts a UV UFO counterpart via HST/COS. Here, a 200 ks XRISM observation of PG 1211+143 is proposed. This will provide the first precision, high resolution measurement of the Fe K band UFO, at a resolution surpassing the soft X-ray measurements. XRISM will resolve the individual Fe K band absorption profiles, allowing the line widths and velocities to be measured at high precision in order to infer the wind structure and geometry.	NON-JET-DOMINATED AGN	2	A	JAMES REEVES	MISAKI MIZUMOTO	USJ	1	NOR	REVEALING THE ULTRA FAST OUTFLOW IN PG 1211+143	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201065010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
188	201070010	HYDRA_A_CENTRAL	139.52264	-12.09511	138.92067	-11.88429	146.14171	-26.40598	242.92456	25.09237	114.48767	60641.19241	2024-11-27 04:37:04	60643.66046	2024-11-29 15:51:04	124.901	100.000	124.901	116.996	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		116.996	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-04 12:42:50	2025-12-11 00:00:00	2024-12-05 12:42:50	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012044	Hydra A is the most powerful FR I radio source in the nearby Universe. Emanating from the central galaxy in a bright X-ray cluster, its jets have inflated a system of X-ray cavities and a surrounding Mach 1.3 shock front extending several hundred kiloparsecs into the cluster atmosphere. Its proximity (z=0.054) and large angular size requires two pointings to measure the energetics of the active inner jets and a second pointing toward the enormously powerful northern cavity and surrounding shock front. The pointings will reveal the expansion speed and cluster weather due to atmospheric bulk motion on the structure of the X-ray cavities. This measurement addresses the fundamental problem of how jet energy heats cluster atmospheres and prevents catastrophic cooling.	GROUPS AND CLUSTERS OF GALAXIES	2	B	BRIAN MCNAMARA		USA	1	NOR	ATMOSPHERIC GAS MOTIONS IN THE HYDRA A GALAXY CLUSTER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201070010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
189	201107010	WR140	305.1173	43.85438	304.69527	43.69509	327.37108	60.49166	80.93044	4.17659	237.18784	60636.83060	2024-11-22 19:56:04	60641.19241	2024-11-27 04:37:04	232.152	160.000	232.152	168.319	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		168.319	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-17 08:13:29	2025-12-11 00:00:00	2024-12-11 19:17:05	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000012182	Cosmic dust is a primary building block of the Earth, and its formation is a fundamental question. The massive colliding wind binary system, WR140, produces massive dust near periastron of its 7.9-year-long orbit. During the dust emission rise in previous binary cycles, the CIII line excess enhanced, and the X-ray emission declined oppositely, suggesting strong cooling of the WWC plasma produced a condition for dust formation. The star experiences another periastron passage on November 22nd, 2024. We propose 3 XRISM observations around that time to study the location and motion of the WWC plasma using the Fe XXV emission line. We also expect to detect the fluorescent Fe line, which strongly constrains the distance of the WWC apex from the stellar surface.	STELLAR CORONAE, WINDS, AND YOUNG STARS	2	A	KENJI HAMAGUCHI		USA	1	NOR	DYNAMICS OF THE EXPLOSIVE DUST FORMATION NEAR PERIASTRON IN WR140	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201107010/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
190	201015010	ABELL754_MAIN	137.3318	-9.68789	136.72326	-9.48418	143.00811	-24.8437	239.37594	24.82343	111.63276	60634.31741	2024-11-20 07:37:04	60636.83060	2024-11-22 19:56:04	119.725	100.000	119.725	0.000	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	310000A0		0.000	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-02 08:51:59	2025-12-11 00:00:00	2024-12-03 08:51:59	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011090	We propose two-pointing deep observations for a sloshing main gas halo (100 ksec) and a subhalo on the verge of destruction (200ksec) in a nearby violent merger, Abell 754, of which the merger axis is almost aligned on the sky plane. Edge-on observation allows us to separate hydrodynamic motion perpendicular to the merger axis from the merger-induced inflow motion. The perpendicular motion acting on disrupting gas halos is only induced in the gas by its collisional nature. Our observation will reveal mixing and incorporating processes of the gas, that is, a scene of hierarchical structure formation. Together with merger parameters derived from weak-lensing mass distribution from Subaru/HSC and galaxy dynamics, a direct measurement of the gas motion and X-ray thermodynamics give us a compr	GROUPS AND CLUSTERS OF GALAXIES	2	A	NOBUHIRO OKABE		JAP	1	NOR	ABELL 754: CAPTURING THE HYDRODYNAMIC MOTION PERPENDICULAR TO THE MERGER AXIS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201015010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
191	201131010	VELA_X-1	135.52796	-40.55428	135.05441	-40.35639	157.03646	-53.92494	263.05766	3.92977	111.3438	60633.01741	2024-11-19 00:25:04	60634.31741	2024-11-20 07:37:04	61.313	40.000	61.313	5.992	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	0.000	0.000	0.000	5.992	11110	313430	11310	PROCESSED	2024-12-02 09:05:19	2025-12-11 00:00:00	2024-12-03 09:05:20	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000014062	We propose a 40-ks XRISM observation of the wind-fed High-Mass X-ray Binary (HMXB) Vela X-1 at orbital phase 0.43-0.53 where we expect the largest changes in absorption as the accretion structure crosses and obstructs our line of sight. By tracing the onset of this structure, we obtain an in-depth view of the stellar wind complexity in this source. In particular, the moderate absorption combined with strong continuum emission happening at these orbital phases will reveal emission lines below 12 keV, even with the gate valve closed. We will follow absorption variability and iron line energy shifts down to the pulse period of the neutron star to probe the onset of the accretion wake on our line of sight and radial velocities of the wind.	BH AND NS BINARIES	2	A	CAMILLE DIEZ		EUR	1	NOR	ON THE ONSET OF THE ACCRETION WAKE IN THE HIGH-MASS X-RAY BINARY VELA X-1	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201131010/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
192	201103010	PI_AQR	336.31988	1.37735	335.68163	1.123	338.59862	10.47267	66.00724	-44.73993	250.49686	60631.53060	2024-11-17 12:44:04	60633.01741	2024-11-19 00:25:04	57.604	50.000	57.604	51.798	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	1	300000A0		51.798	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-12-02 04:57:52	2025-12-11 00:00:00	2024-12-03 04:57:52	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012162	We propose to observe the two brightest gamma Cas-type stars: gamma Cas and pi Aqr for 30 and 50 ks, respectively. The X-ray generating mechanism in these stars is unknown, but recent work has attributed it to accretion onto unseen White Dwarf companions. If accretion is the source, then the X-ray spectra can be used to estimate masses and radii of the White Dwarfs from the plasma's maximum temperature, Fe K line shape quantities, and the mass-accretion rate from a cooling flow model; all of which should be self-consistent. Our plan is to use the high resolution and high energy sensitivity of XRISM to resolve both line emission and thermal continuum turn-over to constrain these quantities and calculate masses and radii as a method testing the self-consistency of the White Dwarf hypothesis.	STELLAR CORONAE, WINDS, AND YOUNG STARS	2	C	SEAN GUNDERSON		USA	1	NOR	TESTING THE WHITE DWARF HYPOTHESIS FOR GAMMA CAS COMPANIONS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201103010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
193	201049010	ABELL1413	178.82728	23.4104	178.18347	23.68867	169.18471	20.91963	226.17287	76.78624	124.50341	60629.24727	2024-11-15 05:56:04	60631.53060	2024-11-17 12:44:04	107.815	100.000	107.815	98.223	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		98.223	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-11-26 05:39:31	2025-12-11 00:00:00	2024-11-27 05:39:31	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011253	To investigate the relationship between the thermal and non-thermal processes in the ICM, we propose a total of 430 ks of on-source XRISM time to observe two intriguing relaxed galaxy clusters. With this data, we will probe the effects of gas sloshing on the non-thermal emission by directly measuring the line-of-sight velocity dispersions within a 15% uncertainty to validate the tentative correlation found for the first time here in relaxed clusters, where the intensity of the non-thermal emission follows the strength of the velocity dispersion in the thermal plasma, a new result for radio mini-halos. Combining this data with the PV relaxed galaxy cluster targets of Perseus and A2029 will allow us to explore the role of gas sloshing as a function of host environment.	GROUPS AND CLUSTERS OF GALAXIES	2	A	HIROKI AKAMATSU		JAP	1	NOR	MINING MEERKAT MINI-HALOS WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201049010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
194	201132010	MRK509	311.04123	-10.72363	310.36016	-10.90519	310.55351	7.12655	35.97129	-29.85588	253.31417	60626.29241	2024-11-12 07:01:04	60629.24727	2024-11-15 05:56:04	128.381	100.000	128.381	4.832	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	31100010	320000A0	105.545	4.832	0.000	0.000	11110	313430	11310	PROCESSED	2024-11-21 20:56:52	2025-12-11 00:00:00	2024-11-22 20:56:53	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000014064	We propose a 100 ks XRISM observation of Mrk509 to assess the origin of its accretion (in)flow and ejection (out)flow. Mrk509 is an ideal target because i) it is very bright in X-rays (<F(2-10)> ~4x10^-11 cgs), providing high enough S/N in the FeK band; ii) it shows a persistent wealth of FeK features, including iii) a strong and multi-component FeK emission line, with a narrow constant component plus a broader one possibly reverberated from a reflector at a few 100s Rg, and iv) two variable narrow absorption lines at ~5.4 keV and ~8.2 keV which could be direct probes of free-falling material. The proposed XRISM high-res observation will allow with a single observation to probe the accretion and ejection processes at once, giving a direct view on the central engine and its energetics.	NON-JET-DOMINATED AGN	2	B	MASSIMO CAPPI		EUR	1	NOR	PROBING THE ACCRETION (IN)FLOW AND WIND (OUT)FLOW IN THE LUMINOUS SEYFERT 1 GALAXY MRK 509	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201132010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
195	201048010	NGC4395	186.45451	33.54741	185.83371	33.82416	170.81796	32.97634	162.08845	81.533	137.52587	60621.16949	2024-11-07 04:04:04	60626.29241	2024-11-12 07:01:04	237.325	200.000	237.325	166.519	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		166.573	0.050	0.000	0.000	11110	313430	11310	PROCESSED	2024-11-21 18:23:08	2025-12-11 00:00:00	2024-11-22 18:23:08	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011251	In understanding the mass accretion onto the BH in all mass range from stellar-mass to supermassive BHs, obscuring structures are crucial, but particularly those of low-mass AGNs are poorly understood. Thus, this proposal aims to study obscuring matter of the nearby low-mass AGN NGC 4395 by 200-ks observation. Our objectives are as follows. (1) Assess the geometrical thickness of the torus by focusing on iron emission originating at radii larger than a dust-sublimation radius. (2) Constrain the inner radius of an iron broad-line region (BLR) by reverberation mapping between the iron-line and continuum emission, and derive a virial factor. Then, assuming a disk model, we will constrain the geometric structure of the BLR, and will conclude the main obscuring structure of the low-mass AGN.	NON-JET-DOMINATED AGN	2	A	TAIKI KAWAMURO		JAP	1	NOR	REVEALING THE NUCLEAR OBSCURING STRUCTURES IN LOW-MASS AGN	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201048010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
196	201115010	NGC7213	332.31743	-47.16715	331.53474	-47.41286	315.9949	-33.17448	349.58782	-52.57983	244.06175	60618.79241	2024-11-04 19:01:04	60621.16949	2024-11-07 04:04:04	118.506	80.000	118.506	83.201	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	88.997	83.201	0.000	0.000	11110	313430	11310	PROCESSED	2024-11-15 11:31:57	2025-11-19 00:00:00	2024-11-16 11:31:57	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000015003	For a long period, research on the broad line region (BLR) in active galactic nuclei (AGN) has predominantly relied on UV/optical spectroscopy. The XRISM/Resolve X-ray spectrometer offers an unprecedented opportunity to explore the X-ray BLR. This proposal aims at utilising the high spectral resolution of Resolve to probe the BLR in NGC 7213, a nearby, bright, and unabsorbed AGN where the low-ionisation Fe Ka is broadly consistent with being produced by the BLR. The proposed XRISM observation will unambiguously establish the origin of the low-ionization Fe K emission line in this target. This will provide a novel perspective, unveiling the hot phases of BLR and its overall ionisation structure.	NON-JET-DOMINATED AGN	2	A	ELIAS KAMMOUN	TAIKI KAWAMURO	EUJ	1	NOR	THE FIRST UNAMBIGUOUS DETECTION OF THE X-RAY BROAD-LINE REGION	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201115010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
197	201050010	ABELL3667_CF_IN	303.26525	-56.88616	302.26445	-57.03687	291.71928	-35.92823	340.79538	-33.46648	250.00111	60614.74588	2024-10-31 17:54:04	60618.79241	2024-11-04 19:01:04	298.903	180.000	298.903	243.336	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		243.336	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-11-08 15:32:02	2025-11-13 00:00:00	2024-11-09 15:32:02	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011257	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 Abell 3667, a striking phenomenon caused by a merger. Resolve observations of this cold front would yield the bulk and turbulent velocities as a function of the distance from the interface, 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.	GROUPS AND CLUSTERS OF GALAXIES	2	C	YUTO ICHINOHE		JAP	1	NOR	GAS DYNAMICS IN THE MOST STRIKING CLUSTER COLD FRONT	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201050010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
198	201051010	ABELL3667_CENTER	303.17404	-56.84815	302.1734	-56.99848	291.67263	-35.87821	340.84164	-33.41709	250.00106	60613.07713	2024-10-30 01:51:04	60614.74588	2024-10-31 17:54:04	116.575	60.000	116.575	108.613	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		108.613	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-11-06 07:48:25	2025-11-07 00:00:00	2024-11-07 07:48:25	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011257	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 Abell 3667, a striking phenomenon caused by a merger. Resolve observations of this cold front would yield the bulk and turbulent velocities as a function of the distance from the interface, 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.	GROUPS AND CLUSTERS OF GALAXIES	2	C	YUTO ICHINOHE		JAP	1	NOR	GAS DYNAMICS IN THE MOST STRIKING CLUSTER COLD FRONT	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201051010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
199	101023010	NGC3516_CAL	166.69742	72.5685	165.8447	72.83887	123.36281	57.98717	133.23589	42.40281	134.41414	60612.70213	2024-10-29 16:51:04	60613.07713	2024-10-30 01:51:04	0.000	30.000	0.000	23.142	PX_NORMAL	N	Y	N	N	N	N	Y	MEDIUM	OFF	OFF	OFF	2	31100010	320000A0	24.750	23.142	0.000	0.000	11110	313430	11310	PROCESSED	2024-11-06 04:02:03	2025-11-07 00:00:00	2024-11-07 04:02:03	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018002	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (2)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101023010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: A WRONG EXPOSURE LONGER THAN A DURATION MAY BE RECORDED DUE TO THE DATA INCLUSION OF BOTH DATAMODE=PX_NORMAL AND PX_MIDRES.
200	201034010	NGC3516	166.6981	72.56833	165.8454	72.8387	123.36331	57.9872	133.23578	42.40307	134.43026	60609.02157	2024-10-26 00:31:04	60612.70213	2024-10-29 16:51:04	268.589	160.000	268.589	184.981	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	197.865	184.981	0.000	0.000	11110	313430	11310	PROCESSED	2024-11-05 13:25:05	2025-11-07 00:00:00	2024-11-06 13:25:06	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013004	In an AGN, a Broad-Line Region (BLR) is one of the most important structures deeply related to the evolution of black holes and feedback to galaxies. However, its formation mechanism is still unclear. Therefore, we propose a 160 ksec XRISM observation on a changing-state AGN NGC 3516, in which a BLR is likely being formed by an outflow in addition to an inflow. With Resolve, we can decompose Fe-K lines from a BLR and a torus, and compare the flux and profile of the BLR line to those in our prior study (Noda+23). We also aim to detect weak Fe XXV/XXVI absorption lines by the outflow. Xtend enables us to identify a soft X-ray continuum that produces the outflow via radiation pressure. By these, we constrain the contributions of inflow and outflow to the BLR formation for the first time.	NON-JET-DOMINATED AGN	2	C	HIROFUMI NODA	EHUD BEHAR	JUS	1	NOR	PROBING FORMATION MECHANISM OF BROAD-LINE REGION IN CHANGING-STATE AGN NGC 3516 WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201034010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
201	201035010	AM_HER	274.05585	49.86801	273.7444	49.84906	279.06429	73.17969	77.86492	25.87586	243.25009	60604.98060	2024-10-21 23:32:04	60609.02157	2024-10-26 00:31:04	198.631	160.000	198.631	165.346	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	176.862	165.346	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-31 14:24:14	2025-11-02 00:00:00	2024-11-01 14:24:15	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013001	The accretion columns in magnetic cataclysmic variables (MCVs) serve as prime laboratories for examining cooling-flow collisional-ionization-equilibrium (CIE) plasma. Fe-K lines, originating from the hot top region of the column, are essential for the diagnostics. We propose a 160 ksec observation of AM Her to achieve the following science goals: 1) Benchmarking the cooling-flow CIE plasma through temperature and density diagnostics, 2) Analyzing shock heating via Doppler velocity measurements of pre/post-shock materials, 3) Determining plasma shape through optically-thick resonance lines within optically-thin plasma, 4) Inferring white dwarf composition from the Compton hump.	ACCRETING WHITE DWARFS AND NOVAE	2	A	YUKIKATSU TERADA	KAYA MORI	JUS	1	NOR-TOO	DIAGNOSTICS OF COOLING-FLOW COLLISIONAL-IONIZATION EQUILIBRIUM PLASMA IN MAGNETIC CATACLYSMIC VARIABLES	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201035010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
202	201073010	SERPENS_X-1	279.99033	5.03594	279.37364	4.9891	281.29588	28.08433	36.11839	4.8417	257.94823	60600.90074	2024-10-17 21:37:04	60604.98060	2024-10-21 23:32:04	172.513	150.000	172.513	19.212	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	153.375	0.000	0.000	19.212	11110	313430	11310	PROCESSED	2024-10-26 11:43:52	2025-10-31 00:00:00	2024-10-27 11:43:53	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012057	Serpens X-1 is a persistently accreting neutron star (NS) with the first confirmed relativistically broadened Fe line for such systems. However, there remains conflicting reports of key parameters, such as the position of the inner accretion disk and inclination. These quantities can be determined from resolving the red- and blue-wings of the Fe line profile, which are most sensitive to the gravitational redshift and Doppler effects, respectively. Further, the Fe line has a unique double-peaked profile which can be due to high disk density effects causing the Fe XXV and XXVI lines to be produced at a similar strength. We request a 300 ks observation of the source to reveal the Doppler and relativistic effects that shape the line profile and further our understanding of the accretion flow.	BH AND NS BINARIES	2	A	RENEE LUDLAM		USA	1	NOR	RESOLVING RELATIVISTIC EFFECTS IN THE ACCRETION DISK OF SERPENS X-1	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201073010/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
203	201068010	GRS1915+105	288.79871	10.94557	288.2088	10.85721	292.14994	32.95063	45.36583	-0.2197	259.88992	60600.03963	2024-10-17 00:57:04	60600.90074	2024-10-17 21:37:04	37.517	30.000	37.517	3.966	PX_NORMAL	N	Y	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	31.661	0.000	0.000	3.966	11110	313430	11310	PROCESSED	2024-10-26 06:25:46	2025-10-31 00:00:00	2024-10-27 06:25:46	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013007	After a long period wherein it was the archetype micro-quasar, GRS 1915+105 has spent the last several years in a highly obscured state that evokes Compton- thick AGN like NGC 1068. However, even in its most obscured phases it is an order of magitude brighter than NGC 1068, and it can deliver even deeper insights into accretion and outflows in this universally important mode. We request a 30 ks observation with XRISM to perform line diagnostics that will reveal the relative radial positioning of cold and hot gas components components, whether or not they are bound to the system or escaping, how much mechanical power is being channeled into the flows, and how the flows relate to the large obscuring column density.	BH AND NS BINARIES	2	A	JON MILLER	SHOGO KOBAYASHI	USJ	1	NOR	GRS 1915+105: FROM MICRO-QUASAR TO MICRO-COMPTON-THICK AGN?	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201068010/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
204	201061010	3C397	286.88076	7.14565	286.27326	7.06622	289.32409	29.45953	41.12086	-0.29832	282.99838	60595.50907	2024-10-12 12:13:04	60600.03963	2024-10-17 00:57:04	186.504	150.000	186.504	157.670	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		157.670	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-26 13:15:39	2025-10-31 00:00:00	2024-10-27 13:15:40	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011331	Thermonuclear explosions of carbon-oxygen white dwarfs (WDs), or Type Ia supernovae (SNe Ia), are important astrophysical phenomena but their exact nature still remains uncertain. Here we propose an XRISM observation of 3C 397, an ``outlier'' of Type Ia supernova remnant likely originating from a near-Chandrasekhar mass WD with an exceptionally high central density (Ohshiro et al. 2021). Thanks to the high spectral resolution of Resolve, we can measure the abundance ratios of Fe-peak elements with unprecedented accuracy. In combination with the performance verification phase observation, this SNR is fully covered by Resolve FoV, enabling us to investigate the spatial distribution of heavy elements.	SUPERNOVA REMNANTS	2	B	YUKEN OHSHIRO		JAP	1	NOR	THE SUPERNOVA REMNANT 3C 397: A PROBE FOR TYPE IA SUPERNOVAE ORIGINATING FROM EXCEPTIONALLY HIGH-DENSITY WHITE DWARFS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201061010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
205	101006010	1E0102.2-7219	16.0096	-72.03182	15.60468	-72.29979	314.63593	-65.03663	301.55667	-45.06277	181.00282	60594.68616	2024-10-11 16:28:04	60595.50907	2024-10-12 12:13:04	43.245	30.000	43.245	31.529	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	MEDIUM	OFF	1	31100010	320000A0	33.771	31.529	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-23 05:52:28	2025-08-31 00:00:00	2024-10-24 05:52:29	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101006010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
206	101005011	1E0102.2-7219	16.0104	-72.03165	15.60549	-72.29962	314.63653	-65.03678	301.55631	-45.06292	180.98521	60594.28755	2024-10-11 06:54:04	60594.68616	2024-10-11 16:28:04	22.356	30.000	22.356	18.184	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	MEDIUM	OFF	1	300000A0		18.184	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-18 07:09:00	2025-08-31 00:00:00	2024-10-19 07:09:00	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101005011/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
207	101005010	1E0102.2-7219	16.01007	-72.03186	15.60516	-72.29983	314.63599	-65.03678	301.55647	-45.06272	180.98576	60593.87574	2024-10-10 21:01:04	60594.28755	2024-10-11 06:54:04	0.000	30.000	0.000	15.971	PX_NORMAL	N	Y	N	N	N	N	Y	MEDIUM	OFF	OFF	OFF	1	300000A0		15.971	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-18 06:40:47	2025-08-31 00:00:00	2024-10-19 06:40:47	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101005010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
208	101013010	Cygnus_Loop	312.89891	32.06389	312.38596	31.87531	328.14684	47.223	75.16165	-7.78736	267.99861	60593.02852	2024-10-10 00:41:04	60593.87574	2024-10-10 21:01:04	39.304	30.000	39.304	35.662	PX_NORMAL	N	Y	N	N	N	N	Y	MEDIUM	OFF	OFF	OFF	1	300000A0		35.662	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-17 05:23:27	2025-08-31 00:00:00	2024-10-18 05:23:27	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101013010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
209	201120010	CYGNUS_A	299.86695	40.73369	299.43401	40.59597	317.70361	59.32564	76.1892	5.75605	275.39115	60589.92991	2024-10-06 22:19:04	60593.02852	2024-10-10 00:41:04	179.372	100.000	179.372	132.243	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		132.243	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-17 10:24:59	2025-10-19 00:00:00	2024-10-18 10:25:00	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000016001	The core region of Cygnus A hosts a remarkably powerful, high-Mach number cocoon shock with an energy up to 10^61 erg. This is clearly a very dynamical example of interaction between the central SMBH and the surrounding gas that should leave unique imprints on the velocity of the ICM. Owing to the high X-ray temperature and brightness of this source, a relatively short 45 ks XRISM observation is sufficient to provide a wealth of velocity diagnostics, including line shifts, widths, shapes, and line strengths which will constrain the resonant scattering effect. These complementary probes of the gas kinematics, sensitive to motions on different scales and their anisotropy, will allow us to study both the small-scale turbulence, and the large-scale motions due to the cocoon shock's expansion.	GROUPS AND CLUSTERS OF GALAXIES	2	A	ANWESH MAJUMDER	TIMOTHY HECKMAN	EUS	1	NOR	EXPLORING THE NATURE OF AGN FEEDBACK NEAR THE COCOON OF CYGNUS A	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201120010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
210	101003010	Crab_SWoffset	83.61798	22.0021	82.86579	21.96935	84.08296	-1.3062	184.56044	-5.80282	90.0007	60589.58130	2024-10-06 13:57:04	60589.92991	2024-10-06 22:19:04	17.244	8.000	17.244	0.236	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		15.440	0.000	0.236	0.000	11110	313430	11310	PROCESSED	2024-10-16 23:09:51	2025-08-31 00:00:00	2024-10-17 23:09:52	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101003010/	WINDOW1BURST		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
211	101002010	Crab_SEoffset	83.64521	22.00183	82.89301	21.96921	84.10818	-1.30758	184.57426	-5.78164	90.00034	60589.38199	2024-10-06 09:10:04	60589.58130	2024-10-06 13:57:04	10.356	8.000	10.356	0.146	PX_NORMAL	N	N	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		9.547	0.000	0.146	0.000	11110	313430	11310	PROCESSED	2024-10-17 23:11:34	2025-08-31 00:00:00	2024-10-16 04:59:44	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101002010/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
212	101001010	Crab_NWoffset	83.61772	22.02725	82.86539	21.99449	84.08384	-1.28107	184.53897	-5.78956	90.0003	60589.18269	2024-10-06 04:23:04	60589.38199	2024-10-06 09:10:04	9.805	8.000	9.805	0.132	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31200010		8.608	0.000	0.132	0.000	11110	313430	11310	PROCESSED	2024-10-17 22:51:19	2025-08-31 00:00:00	2024-10-16 04:27:43	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101001010/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
213	101000010	Crab_NEoffset	83.64751	22.02716	82.89517	21.99454	84.11142	-1.28238	184.5539	-5.76629	90.00348	60588.95560	2024-10-05 22:56:04	60589.18269	2024-10-06 04:23:04	8.629	8.000	8.629	0.103	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31200010		6.758	0.000	0.103	0.000	11110	313430	11310	PROCESSED	2024-10-17 22:55:25	2025-08-31 00:00:00	2024-10-15 16:11:22	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000018001	None	CALIBRATION	1	A	XRISM Collaboration		CAL	1	CAL	AO1 Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/101000010/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
214	201108010	WR140	305.11507	43.85461	304.69305	43.69532	327.36841	60.49261	80.92972	4.17805	283.34756	60587.46255	2024-10-04 11:06:04	60588.95560	2024-10-05 22:56:04	104.066	45.000	104.066	59.588	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	63.738	59.588	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-18 00:19:49	2025-10-19 00:00:00	2024-10-15 16:28:10	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012182	Cosmic dust is a primary building block of the Earth, and its formation is a fundamental question. The massive colliding wind binary system, WR140, produces massive dust near periastron of its 7.9-year-long orbit. During the dust emission rise in previous binary cycles, the CIII line excess enhanced, and the X-ray emission declined oppositely, suggesting strong cooling of the WWC plasma produced a condition for dust formation. The star experiences another periastron passage on November 22nd, 2024. We propose 3 XRISM observations around that time to study the location and motion of the WWC plasma using the Fe XXV emission line. We also expect to detect the fluorescent Fe line, which strongly constrains the distance of the WWC apex from the stellar surface.	STELLAR CORONAE, WINDS, AND YOUNG STARS	2	A	KENJI HAMAGUCHI		USA	1	NOR	DYNAMICS OF THE EXPLOSIVE DUST FORMATION NEAR PERIASTRON IN WR140	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201108010/	WINDOW2	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
215	201104010	SNR0509-68.7	77.24902	-68.72666	77.30721	-68.78801	330.12374	-84.70105	279.58108	-34.36676	89.99442	60583.71046	2024-09-30 17:03:04	60587.46255	2024-10-04 11:06:04	189.817	125.000	189.817	122.864	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		122.864	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-11 12:39:03	2025-10-16 00:00:00	2024-10-12 12:39:04	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012172	We propose for observations of the two brightest Type Ia supernova remnants in the LMC. Both of these objects, 0509-68.7 (N103B) and 0519-69.0 are young (<1000 yrs). These remnants are very well-studied with other observatories, but XRISM observations will allow us to directly measure the ion temperature of various species, determine the bulk velocity of the ejecta products, measure elemental abundances of both ejecta and the surrounding medium, and search for new spectral features. We request 125 ks for N103B and 300 ks for 0519-69.0.	SUPERNOVA REMNANTS	2	B	BRIAN WILLIAMS		USA	1	NOR	RESOLVING THE TWO BRIGHTEST YOUNG TYPE IA SNRS IN THE LMC	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201104010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
216	901001010	V4641_Sgr	274.84045	-25.40719	274.06778	-25.42882	274.37411	-2.04137	6.77407	-4.78933	268.19773	60583.40421	2024-09-30 09:42:04	60583.71046	2024-09-30 17:03:04	13.361	10.000	13.361	12.172	PX_NORMAL	N	N	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		12.172	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-04 09:36:02	2023-09-07 00:00:00	2024-10-05 09:36:02	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000019006	V4641 Sgr is a transient Galactic black hole X-ray binary (BHXB) with unique spectral properties. It shows a disk blackbody spectrum at unusually low luminosities, which suggests that the inner region of the disk is obscured and only the scattered emission can be observed (Shaw et al. 2022). In addition, narrow emission lines, including Fe XXVI Lya and Fe XXV Hea, were detected with Chandra/HETG in 2020 (Shaw et al. 2022). In the Chandra observations, some of the low-energy lines such as Mg XII and Si XVI were found to have potential blueshifted absorption lines (i.e., p-Cygni profiles), suggesting that their origin is a disk wind with a large solid angle, perhaps a spherical geometry.	BH AND NS BINARIES	9	A	XRISM Collaboration		DDT	1	DDT-TOO	DDT TOO REQUEST OF V4641	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/901001010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
217	201021010	3C111	64.5868	38.02637	63.75068	37.9051	69.36787	16.38982	161.67465	-8.82099	71.87593	60578.52644	2024-09-25 12:38:04	60583.40421	2024-09-30 09:42:04	224.068	200.000	224.068	178.856	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	191.313	178.856	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-04 14:09:02	2025-10-05 00:00:00	2024-10-05 14:09:03	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000011132	One of the most important questions of the active galactic nucleus (AGN) is the origin of the dichotomy of radio-quiet and radio-loud AGN. This is tightly related to the formation of the relativistic jets from black holes. The key to solving it is fast accretion disk winds, so-called ultra-fast outflows (UFOs). Observational facts indicate that the UFO is launched from the vicinity of the black hole. Thus, the UFO is the best probe for the innermost region of radio-loud AGN. To tackle the radio-quiet/loud dichotomy with the UFOs, we propose a 200 ks observation of 3C 111, which most probably harbors the UFO. With high resolution of Resolve, we will detect the UFO at 6 sigma level. Resolve will also allow us to estimate the kinetic power of the UFO and magnetization of the disk and UFO.	BLAZARS AND OTHER JET-DOMINATED AGN	2	B	KOUICHI HAGINO		JAP	1	NOR	PROBING THE INNERMOST REGION OF A JETTED ACTIVE GALACTIC NUCLEUS 3C 111	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201021010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
218	201118010	TYCHO_NE	6.40798	64.17041	5.70697	63.89364	42.92178	53.75317	120.12496	1.43939	4.89326	60576.38130	2024-09-23 09:09:04	60578.52644	2024-09-25 12:38:04	159.515	100.000	159.515	148.211	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		148.211	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-02 13:51:02	2025-10-05 00:00:00	2024-10-03 13:51:02	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000014029	We propose a 100 ks observation to study the unique northeast region with complementary goals: understand the origin of the large-scale velocity asymmetry in the line-of-sight, where the northeast region is observed to be predominantly blue-shifted, constrain the explosion mechanism and environment of a Type Ia progenitor, constrain the ion temperatures, and probe the interaction with the neutral ambient medium in this region observed in Halpha optical emission. For that, we will resolve the line complex, measure temperatures, non-equilibrium ionization times and abundances, determine line shifts and broadenings of individual element from Si to the iron K line, search for rare element lines and charge exchange lines due to interaction with the neutral ambient medium.	SUPERNOVA REMNANTS	2	B	ANNE DECOURCHELLE		EUR	1	NOR	UNVEILING THE ASYMMETRIC EJECTA ORIGIN AND AMBIENT MEDIUM INTERACTION IN TYCHO'S SNR	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201118010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
219	201083010	MRK279	208.2657	69.30836	207.97464	69.55382	144.91488	67.64716	115.04092	46.86442	210.81787	60572.83199	2024-09-19 19:58:04	60576.38130	2024-09-23 09:09:04	181.110	150.000	181.110	154.689	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	165.463	154.689	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-28 11:50:06	2025-10-03 00:00:00	2024-09-29 11:50:07	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000012098	Observations of extreme variability in the narrow Fe K-alpha emission line - independent of a moderately broad line component - demonstrate that multiple geometries can be explored in the Sy-1.5 AGN Mrk 279. This makes it an optimal target for XRISM Cycle 1. Variability in the narrow line component suggests a modest radius and extent, consistent with the optical broad line region. The "broad" Fe Ka component is not extreme and suggests a truncated inner disk and/or one with a warp. We request a 150 ks obs. of Mrk 279 in XRISM Cycle 1 to (1) precisely locate the Fe Ka emission components within the accretion flow, (2) compare the radii and geometries to optical line constraints, (3) test models of warped and/or truncated disks, (4) study ionized winds in emission.	NON-JET-DOMINATED AGN	2	A	JON MILLER		USA	1	NOR	IRONING-OUT THE ACCRETION FLOW IN SEYFERT AGN WITH MRK 279	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201083010/	WINDOW2	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
220	201089010	ABELL_2199	247.15924	39.55073	246.73043	39.65972	233.10266	60.09778	62.93361	43.69359	259.92583	60567.47157	2024-09-14 11:19:04	60572.83199	2024-09-19 19:58:04	262.636	220.000	262.636	245.687	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		245.738	0.000	0.000	0.006	11110	313430	11310	PROCESSED	2024-09-25 14:36:16	2025-10-03 00:00:00	2024-09-26 14:36:17	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013011	As clusters are ultimate depositories of billions of core-collapse and Type Ia supernovae, measuring accurate abundances in the intracluster medium (ICM) provides unique constraints on the nature and physics of supernovae progenitors. While Resolve (in its GVC status) constrains the abundance of heavier elements (S, Ar, Ca, Cr, Mn, Fe, Ni), lighter elements (O, Ne, Mg, Si) can be constrained with XMM-Newton RGS and EPIC. Unlike other "abundance-friendly" clusters, Abell 2199 exhibits very weak EPIC-RGS abundance discrepancies. Our proposal takes advantage of this and aims for a 220 ks XRISM exposure of the core of A2199. Unleashing the full potential of join RGS-Resolve spectroscopy will boost our understanding of the nature of Type Ia supernovae progenitors and ICM enrichment.	GROUPS AND CLUSTERS OF GALAXIES	2	A	FRANCOIS MERNIER	KOSUKE SATO	USJ	1	NOR	THE CHEMICAL COMPOSITION OF THE COOL-CORE CLUSTER ABELL 2199	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201089010/	WINDOW1		1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
221	201074010	HERCULES_X-1	254.45767	35.3426	254.00717	35.41823	246.00071	57.49404	58.14936	37.52297	269.57223	60563.06602	2024-09-10 01:35:04	60567.47157	2024-09-14 11:19:04	215.178	180.000	215.178	25.190	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	201.102	0.000	0.000	25.190	11110	313430	11310	PROCESSED	2024-09-19 08:46:56	2025-09-27 00:00:00	2024-09-20 08:46:57	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000013009	Her X-1 is an X-ray binary with a warped, precessing disk, uniquely allowing us to sample the vertical structure of its disk wind, and measure the wind number density from its time-dependent ionization response to the X-ray pulsations of the neutron star. We request 180 ks of XRISM exposure to perform a deep analysis of the wind of Her X-1. Pulse-resolved analysis of these exposures will result in 3 to 5 constraints on the wind number density over a range of heights above disk, allowing us to fit for density evolution with height. The measured density evolution will strongly constrain the wind launching mechanism. These observations will give us the best 3D understanding of an accretion disk wind in an XRB, and result in the most precise total mass outflow rate and energetics measurements.	BH AND NS BINARIES	2	A	PETER KOSEC	TERUAKI ENOTO	USJ	1	NOR-TOO	MAPPING THE 3D GEOMETRY OF THE DISK WIND OF HERCULES X-1	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201074010/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
222	201030010	H1821+643	275.48893	64.34386	275.4247	64.31737	318.33027	86.82175	94.00305	27.41687	289.99964	60557.10074	2024-09-04 02:25:04	60563.06602	2024-09-10 01:35:04	283.716	250.000	283.716	278.888	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		278.888	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-16 21:23:52	2025-09-19 00:00:00	2024-09-17 21:33:04	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000011159	We propose a 250 ks XRISM observation of H1821+643, a recoiling and extremely accreting supermassive black hole (SMBH) in a cooling flow cluster. Cooling flows are expected to have a huge impact on the active galactic nuclei (AGNs), yet they are scarcely observed in the local Universe, known as the cooling flow problem. H1821+643 is an irreplaceable target hosting cooling flows and a radio-quiet quasar. We will measure the turbulent motions within the cooling core to understand quasar-mode feedback. To comprehend how the SMBH acquires its large mass, we will also examine the AGN structure (torus, broad-line region, and accretion disk) by resolving the complex Fe lines. This observation will reveal new frontiers on the long-standing cooling flow problem and SMBH formation in cooling cores.	NON-JET-DOMINATED AGN	2	B	SATOSHI YAMADA		JAP	1	NOR	A RECOILING AND EXTREMELY ACCRETING SUPERMASSIVE BLACK HOLE IN A COOLING FLOW CLUSTER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201030010/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
223	300002020	GX340+00	251.44989	-45.61103	250.54062	-45.52034	256.00213	-23.06907	339.58871	-0.07996	263.99948	60553.67852	2024-08-31 16:17:04	60557.10074	2024-09-04 02:25:04	153.887	150.000	153.887	16.454	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	131.361	0.000	0.000	16.454	11110	313430	11310	PROCESSED	2024-09-11 11:13:17	2025-09-12 00:00:00	2024-09-12 11:13:18	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000009	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.	GALACTIC DIFFUSE EMISSION AND SURVEYS	3	A	XRISM Collaboration		JAP	0	NOR	THE X-RAY VIEW OF INTERSTELLAR DUST FROM SILICON TO IRON	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300002020/	WINDOW2BURST	WINDOW1	1	Observation Log: No remarks ; Pre-pipeline Log: No remarks
224	300046010	Galactic_Center_3	266.28059	-29.1153	265.48522	-29.09531	266.73484	-5.71815	359.79043	-0.00059	271.49941	60550.75074	2024-08-28 18:01:04	60553.67852	2024-08-31 16:17:04	125.832	100.000	125.832	111.831	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		111.831	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 02:44:42	2025-08-31 00:00:00	2024-09-07 23:52:10	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000072	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.	GALACTIC DIFFUSE EMISSION AND SURVEYS	3	C	XRISM Collaboration		JAP	0	NOR	INVESTIGATION OF THE ACTIVITIES IN THE GALACTIC CENTER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300046010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
225	300008020	T_CORONA_BOREALIS	239.87595	25.92048	239.35229	26.06127	230.10034	45.27522	42.37434	48.16451	276.31359	60547.16255	2024-08-25 03:54:04	60550.75074	2024-08-28 18:01:04	158.881	150.000	158.881	137.919	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		137.919	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 16:02:54	2025-08-31 00:00:00	2024-09-08 02:40:04	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000020	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.	ACCRETING WHITE DWARFS AND NOVAE	3	A	XRISM Collaboration		JAP	0	NOR-TOO	GRAVITATIONALLY REDSHIFTED 6.4 KEV LINE IN T CORONAE BOREALIS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300008020/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
226	300045020	Galactic_Center_2	266.55772	-28.88932	265.76373	-28.87068	266.97264	-5.4862	0.10959	-0.08977	256.99689	60545.50421	2024-08-23 12:06:04	60547.16255	2024-08-25 03:54:04	67.066	100.000	67.066	53.752	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		53.752	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-20 20:36:36	2025-08-31 00:00:00	2024-09-07 19:18:20	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000072	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.	GALACTIC DIFFUSE EMISSION AND SURVEYS	3	A	XRISM Collaboration		JAP	0	NOR	INVESTIGATION OF THE ACTIVITIES IN THE GALACTIC CENTER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300045020/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
227	300005020	Kepler_SNR	262.66482	-21.48226	261.91559	-21.44491	263.17358	1.78338	4.52204	6.82879	269.99719	60543.26880	2024-08-21 06:27:04	60545.50421	2024-08-23 12:06:04	91.627	50.000	91.627	80.110	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		80.110	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 08:46:02	2025-08-31 00:00:00	2024-09-07 21:16:15	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000016	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.	SUPERNOVA REMNANTS	3	C	XRISM Collaboration		JAP	0	NOR	THE PROGENITOR SYSTEM AND EXPLOSION PHYSICS FOR KEPLER'S SNR	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300005020/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
228	300002010	GX340+00	251.44838	-45.61112	250.53912	-45.52042	256.00101	-23.06931	339.58796	-0.07922	263.99691	60539.44796	2024-08-17 10:45:04	60543.26880	2024-08-21 06:27:04	152.637	150.000	152.637	15.203	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	121.372	0.000	0.000	15.203	11110	313430	11310	PROCESSED	2024-09-22 02:40:16	2025-09-12 00:00:00	2024-09-08 02:01:46	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000009	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.	GALACTIC DIFFUSE EMISSION AND SURVEYS	3	A	XRISM Collaboration		JAP	0	NOR	THE X-RAY VIEW OF INTERSTELLAR DUST FROM SILICON TO IRON	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300002010/	WINDOW2BURST	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
229	300000010	GT_MUS	174.873	-65.39784	174.28945	-65.1206	218.30538	-58.10221	295.53142	-3.56504	331.16729	60535.05213	2024-08-13 01:15:04	60539.44796	2024-08-17 10:45:04	204.679	90.000	204.679	165.142	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		165.142	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-10-08 10:04:05	2025-08-31 00:00:00	2024-08-21 14:23:07	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000004	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.	STELLAR CORONAE, WINDS, AND YOUNG STARS	3	A	XRISM Collaboration		JAP	0	NOR-TOO	NON-THERMAL SIGNATURES DURING STELLAR FLARES	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300000010/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
230	300020010	IRAS_F05189-2524	80.25513	-25.36227	79.74466	-25.41064	76.69392	-48.35243	227.88845	-30.29328	63.0007	60531.68338	2024-08-09 16:24:04	60535.05213	2024-08-13 01:15:04	169.164	100.000	169.164	145.414	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		145.414	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 11:36:52	2025-08-31 00:00:00	2024-08-20 09:43:57	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000038	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.	NON-JET-DOMINATED AGN	3	C	XRISM Collaboration		JAP	0	NOR	XRISM STUDIES OF ULTRA LUMINOUS IR GALAXY IRAS F05189-2524	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300020010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
231	300019010	CENTAURUS_A	201.36512	-43.019	200.63176	-42.75903	217.14334	-31.33179	309.51595	19.41737	299.9728	60526.80352	2024-08-04 19:17:04	60531.68338	2024-08-09 16:24:04	227.986	100.000	227.986	182.753	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	195.482	182.753	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 01:27:32	2025-08-31 00:00:00	2024-08-17 13:31:24	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000037	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=3.8 Mpc) with dramatic bipolar jets; it is the brightest such galaxy in the 4-10~keV band, and its spectra show the strongest narrow Fe~Ka emission line among radio-loud AGN. It is possible to associate the narrow Fe line with the elusive optical BLR, and some spectra hint at ultra-fast, v~0.1c winds. Resolve spectroscopy of Cen A will reveal the inner and intermediate disk in the jet mode, and reveal the properties of slow and ultra-fast disk winds.	BLAZARS AND OTHER JET-DOMINATED AGN	3	A	XRISM Collaboration		JAP	0	NOR	THE JET-LAUNCHING DISK AND ACCRETION FLOW IN CENTAURUS A	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300019010/	WINDOW2	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
232	300053010	Abell2029_N2	227.79431	5.82455	227.17486	6.01267	223.56849	22.72049	6.63097	50.54494	284.99919	60518.67782	2024-07-27 16:16:04	60526.80352	2024-08-04 19:17:04	383.186	50.000	383.186	350.240	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		350.240	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-25 12:02:50	2025-08-31 00:00:00	2024-08-14 02:36:32	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000080	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.	GROUPS AND CLUSTERS OF GALAXIES	3	A	XRISM Collaboration		JAP	0	NOR	NON-THERMAL PRESSURE SUPPORT IN RELAXED GALAXY CLUSTERS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300053010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
233	300050010	NGC3783	174.75746	-37.73904	174.13758	-37.46189	192.67926	-36.17844	287.45639	22.94711	310.19096	60509.20699	2024-07-18 04:58:04	60518.67782	2024-07-27 16:16:04	451.210	200.000	451.210	371.912	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	397.815	371.912	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 04:01:49	2025-08-31 00:00:00	2024-08-06 14:06:36	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000078	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.	NON-JET-DOMINATED AGN	3	A	XRISM Collaboration		JAP	0	NOR	THROUGH DARKNESS AND LIGHT: THE MANY FACES OF THE OUTFLOWS IN NGC 3783	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300050010/	WINDOW2	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
234	300073010	COMA_CENTER	194.94363	27.94653	194.3405	28.21584	181.51561	31.37171	57.29432	87.97895	285.8439	60500.30352	2024-07-09 07:17:04	60509.20699	2024-07-18 04:58:04	402.101	200.000	402.101	356.832	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		356.832	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 10:35:08	2025-08-31 00:00:00	2024-07-28 19:44:44	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000102	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.	GROUPS AND CLUSTERS OF GALAXIES	3	A	XRISM Collaboration		JAP	0	NOR	FIRST DIRECT MEASUREMENT OF THE POWER SPECTRUM OF INTERGALACTIC TURBULENCE	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300073010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
235	300075020	NGC1365	53.40093	-36.14094	52.92357	-36.30791	36.80348	-53.03479	237.95708	-54.59856	48.90066	60494.49171	2024-07-03 11:48:04	60500.30352	2024-07-09 07:17:04	261.763	125.000	261.763	238.773	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		238.773	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 19:45:06	2025-08-31 00:00:00	2024-07-25 15:15:44	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000103	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.	NON-JET-DOMINATED AGN	3	A	XRISM Collaboration		JAP	0	NOR	STUDYING PHOTOIONISED OUTFLOWS IN A LUMINOUS STAR-FORMING AGN	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300075020/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
236	300008010	T_CORONA_BOREALIS	239.87456	25.92151	239.35091	26.0623	230.09823	45.27585	42.37544	48.16595	321.17066	60488.00282	2024-06-27 00:04:04	60494.49171	2024-07-03 11:48:04	294.093	150.000	294.093	230.377	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		230.377	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 10:43:37	2025-08-31 00:00:00	2024-07-11 19:38:13	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000020	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.	ACCRETING WHITE DWARFS AND NOVAE	3	A	XRISM Collaboration		JAP	0	NOR-TOO	GRAVITATIONALLY REDSHIFTED 6.4 KEV LINE IN T CORONAE BOREALIS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300008010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
237	300007010	MRK766	184.61068	29.81311	183.98205	30.09068	171.20723	28.93979	190.67877	82.27022	290.32471	60485.55491	2024-06-24 13:19:04	60488.00282	2024-06-27 00:04:04	111.753	80.000	111.753	85.231	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	91.167	85.231	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-20 21:10:06	2025-08-31 00:00:00	2024-07-09 06:57:13	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000018	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.	NON-JET-DOMINATED AGN	3	C	XRISM Collaboration		JAP	0	NOR	ABSORPTION AND EMISSION UNDER EXTREME CONDITIONS: THE CASE OF MRK766	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300007010/	WINDOW2	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
238	300047040	NGC4151	182.63562	39.40586	182.00428	39.68397	164.0968	36.62389	155.0773	75.063	292.34797	60483.58407	2024-06-22 14:01:04	60485.55491	2024-06-24 13:19:04	90.109	45.000	90.109	72.990	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	78.074	72.990	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 12:34:07	2025-08-31 00:00:00	2024-07-02 07:37:09	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000073	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.	NON-JET-DOMINATED AGN	3	A	XRISM Collaboration		JAP	0	NOR	SHAPING NEW AGN HORIZONS WITH NGC 4151	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300047040/	WINDOW2	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
239	300021010	SN1987A	83.86674	-69.26864	83.95832	-69.29819	307.604	-86.44652	279.70213	-31.93721	31.01293	60478.76394	2024-06-17 18:20:04	60483.58407	2024-06-22 14:01:04	348.866	100.000	348.866	176.284	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		176.284	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 13:48:18	2025-08-31 00:00:00	2024-06-28 18:46:15	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000040	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.	SUPERNOVA REMNANTS	3	A	XRISM Collaboration		JAP	0	NOR	TIME EVOLUTION OF YOUNG NEI PLASMA IN SN 1987A	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300021010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
240	300047030	NGC4151	182.63587	39.40583	182.00453	39.68394	164.09703	36.62396	155.07679	75.06314	292.34868	60476.93755	2024-06-15 22:30:04	60478.76394	2024-06-17 18:20:04	85.154	45.000	85.154	72.719	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	77.784	72.719	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 08:44:12	2025-08-31 00:00:00	2024-06-23 10:12:59	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000073	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.	NON-JET-DOMINATED AGN	3	A	XRISM Collaboration		JAP	0	NOR	SHAPING NEW AGN HORIZONS WITH NGC 4151	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300047030/	WINDOW2	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
241	300014010	M87	187.70449	12.38992	187.07178	12.66598	182.05844	14.41501	283.77406	74.48959	300.27887	60474.34310	2024-06-13 08:14:04	60476.93755	2024-06-15 22:30:04	121.725	100.000	121.725	109.030	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		109.030	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 15:32:33	2025-08-31 00:00:00	2024-06-23 12:55:16	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000035	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.	GROUPS AND CLUSTERS OF GALAXIES	3	A	XRISM Collaboration		JAP	0	NOR	SUPERMASSIVE BLACK HOLE FEEDBACK IN M87	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300014010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
242	300067010	Eta_Carinae	161.26326	-59.68439	160.77673	-59.42105	202.15378	-58.928	287.59609	-0.62983	267.00212	60470.01185	2024-06-09 00:17:04	60474.34310	2024-06-13 08:14:04	316.703	100.000	316.703	183.448	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		183.448	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 13:08:40	2025-08-31 00:00:00	2024-06-22 12:32:36	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000092	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.	STELLAR CORONAE, WINDS, AND YOUNG STARS	3	A	XRISM Collaboration		JAP	0	NOR	DYNAMICS OF THE COLLISIONAL SHOCKS DRIVEN BY THE MASSIVE BINARY ETA CARINAE	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300067010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
243	300042010	SS_CYGNI	325.67804	43.58574	325.18703	43.35652	350.4662	52.65588	90.55877	-7.1107	60.43878	60465.44310	2024-06-04 10:38:04	60470.01185	2024-06-09 00:17:04	281.346	100.000	281.346	169.270	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	181.059	169.270	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 18:32:17	2025-08-31 00:00:00	2024-06-15 14:25:49	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000067	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.	ACCRETING WHITE DWARFS AND NOVAE	3	A	XRISM Collaboration		JAP	0	NOR-TOO	OBSERVATIONS OF SS CYGNI IN QUIESCENCE AND OUTBURST	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300042010/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
244	300017010	M87_SW_ARM	187.66104	12.35739	187.02826	12.63349	182.03208	14.36803	283.65928	74.44583	300.27703	60463.83407	2024-06-02 20:01:04	60465.44310	2024-06-04 10:38:04	78.289	150.000	78.289	73.914	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		73.914	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 12:02:23	2025-12-27 00:00:00	2024-06-11 15:28:16	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000035	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.	GROUPS AND CLUSTERS OF GALAXIES	3	A	XRISM Collaboration		JAP	0	NOR	SUPERMASSIVE BLACK HOLE FEEDBACK IN M87	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300017010/	WINDOW1		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
245	300015010	M87_E_ARM	187.75884	12.39092	187.12619	12.66695	182.10809	14.43753	283.96256	74.50634	300.28031	60460.37574	2024-05-30 09:01:04	60463.83407	2024-06-02 20:01:04	168.098	150.000	168.098	157.201	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		157.201	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 04:48:43	2025-08-31 00:00:00	2024-06-11 17:19:55	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000035	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.	GROUPS AND CLUSTERS OF GALAXIES	3	A	XRISM Collaboration		JAP	0	NOR	SUPERMASSIVE BLACK HOLE FEEDBACK IN M87	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300015010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
246	300016020	M87_NW	187.67858	12.43514	187.04587	12.71122	182.01556	14.44602	283.63288	74.52513	300.28125	60457.24380	2024-05-27 05:51:04	60460.37574	2024-05-30 09:01:04	151.639	100.000	151.639	137.800	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		137.800	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 21:45:41	2025-08-31 00:00:00	2024-06-07 12:30:47	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000035	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.	GROUPS AND CLUSTERS OF GALAXIES	3	A	XRISM Collaboration		JAP	0	NOR	SUPERMASSIVE BLACK HOLE FEEDBACK IN M87	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300016020/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
247	100017010	M87_NW_CAL	187.67863	12.43497	187.04592	12.71106	182.01568	14.44589	283.63324	74.52498	300.2972	60456.87921	2024-05-26 21:06:04	60457.24380	2024-05-27 05:51:04	0.000	17.000	0.000	17.845	PX_NORMAL	N	Y	N	N	N	N	Y	MEDIUM	OFF	OFF	OFF	1	300000A0		17.845	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 05:07:31	2025-08-31 00:00:00	2024-06-06 08:40:59	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100017010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: A WRONG EXPOSURE LONGER THAN A DURATION MAY BE RECORDED DUE TO THE DATA INCLUSION OF BOTH DATAMODE=PX_NORMAL AND PX_MIDRES.
248	300016010	M87_NW	187.67835	12.43539	187.04565	12.71147	182.01526	14.44615	283.63182	74.5253	300.28114	60456.18685	2024-05-26 04:29:04	60456.87921	2024-05-26 21:06:04	29.138	100.000	29.138	28.052	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		28.052	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 03:30:58	2025-08-31 00:00:00	2024-06-05 00:26:12	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000035	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.	GROUPS AND CLUSTERS OF GALAXIES	3	A	XRISM Collaboration		JAP	0	NOR	SUPERMASSIVE BLACK HOLE FEEDBACK IN M87	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300016010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
249	900002010	SN2024iss	194.77515	28.81104	194.17297	29.08056	180.90076	32.07586	78.22256	87.61381	313.82588	60454.64171	2024-05-24 15:24:04	60456.18685	2024-05-26 04:29:04	71.287	60.000	71.287	65.037	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		65.037	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 22:48:48	2025-08-31 00:00:00	2024-06-05 01:32:39	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000009002	We propose a ToO observation of supernovae (SN) in nearby galaxies. Goal is to detect emission lines including Fe-K lines and measure their center energy and width (minimum case). In addition, when the flux is higher, we could measure metal abundance pattern and ionization state of CSM. From these measurements, we can obtain information on physical properties of circumstellar (CSM) medium around SN. If the SN is enough bright to monitor a long time trend, we propose one more observation after one month or later to probe a mass loss history of progenitor (ideal case).	EXTRAGALACTIC TRANSIENTS: SNE, GRBS, GW EVENTS, AND TDES	9	A	XRISM Collaboration		DDT	0	DDT-TOO	HIGH RESOLUTION X-RAY PROBING OF CIRCUMSTELLAR MEDIUM AROUND SUPERNOVAE IN THE EARLY PHASE	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/900002010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
250	300074020	COMA_OFFSET	194.94154	27.84697	194.33825	28.11629	181.56612	31.28196	54.67252	88.01812	313.82618	60452.99796	2024-05-22 23:57:04	60454.64171	2024-05-24 15:24:04	81.201	100.000	81.201	72.760	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		72.760	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 23:15:14	2025-08-31 00:00:00	2024-05-30 12:32:18	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000102	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.	GROUPS AND CLUSTERS OF GALAXIES	3	C	XRISM Collaboration		JAP	0	NOR	FIRST DIRECT MEASUREMENT OF THE POWER SPECTRUM OF INTERGALACTIC TURBULENCE	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300074020/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
251	300057020	VELA_X-1	135.52863	-40.55475	135.05508	-40.35686	157.0376	-53.92511	263.05836	3.92984	294.84764	60452.49032	2024-05-22 11:46:04	60452.99796	2024-05-22 23:57:04	13.088	10.000	13.088	1.390	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	320000A0	11.096	0.000	0.000	1.390	11110	313430	11310	PROCESSED	2024-09-24 20:26:40	2025-08-31 00:00:00	2024-05-30 10:23:21	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000087	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	BH AND NS BINARIES	3	C	XRISM Collaboration		JAP	0	NOR	PROBING THE WIND-COMPACT OBJECT INTERACTION IN VELA X-1	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300057020/	WINDOW2BURST	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
252	300074010	COMA_OFFSET	194.94118	27.84693	194.33789	28.11625	181.56581	31.28179	54.67472	88.01842	313.82617	60450.50352	2024-05-20 12:05:04	60452.49032	2024-05-22 11:46:04	89.819	100.000	89.819	81.044	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		81.044	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 23:04:38	2025-08-31 00:00:00	2024-05-30 12:12:20	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000102	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.	GROUPS AND CLUSTERS OF GALAXIES	3	C	XRISM Collaboration		JAP	0	NOR	FIRST DIRECT MEASUREMENT OF THE POWER SPECTRUM OF INTERGALACTIC TURBULENCE	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300074010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
253	300047020	NGC4151	182.63516	39.40629	182.00382	39.6844	164.09615	36.62409	155.07736	75.06244	308.87155	60448.29866	2024-05-18 07:10:04	60450.50352	2024-05-20 12:05:04	103.714	45.000	103.714	80.437	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	86.040	80.437	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 03:18:56	2025-08-31 00:00:00	2024-05-26 14:22:01	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000073	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.	NON-JET-DOMINATED AGN	3	A	XRISM Collaboration		JAP	0	NOR	SHAPING NEW AGN HORIZONS WITH NGC 4151	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300047020/	WINDOW2	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
254	300042020	SS_CYGNI	325.67751	43.58596	325.1865	43.35675	350.46587	52.65628	90.55863	-7.11027	76.86924	60444.99866	2024-05-14 23:58:04	60448.29866	2024-05-18 07:10:04	158.798	100.000	158.798	140.806	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	320000A0	150.613	140.806	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 22:18:20	2025-08-31 00:00:00	2024-05-23 10:39:58	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000067	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.	ACCRETING WHITE DWARFS AND NOVAE	3	C	XRISM Collaboration		JAP	0	NOR-TOO	OBSERVATIONS OF SS CYGNI IN QUIESCENCE AND OUTBURST	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300042020/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
255	300068010	M82	148.96941	69.67956	147.93305	69.91675	118.98057	52.10839	141.40936	40.56731	286.83353	60442.00352	2024-05-12 00:05:04	60444.99866	2024-05-14 23:58:04	223.180	50.000	223.180	168.887	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		168.887	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 17:48:10	2025-08-31 00:00:00	2024-05-23 10:03:08	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000093	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.	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	3	A	XRISM Collaboration		JAP	0	NOR	DIRECT VELOCITY MEASUREMENT OF X-RAY EMITTING HOT GAS IN STARBURST-DRIVEN OUTFLOWS IN M82 AND NGC 253 WITH XRISM/RESOLVE	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300068010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
256	300018010	M81	148.89023	69.06487	147.86581	69.30187	119.49165	51.58025	142.09173	40.90089	286.83671	60438.36324	2024-05-08 08:43:04	60442.00352	2024-05-12 00:05:04	268.779	100.000	268.779	239.300	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		239.300	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 20:18:39	2025-08-31 00:00:00	2024-05-19 12:44:22	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000036	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.	NON-JET-DOMINATED AGN	3	C	XRISM Collaboration		JAP	0	NOR	A RADIATIVELY INEFFICIENT ACCRETION FLOW IN THE LINER M81*	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300018010/	WINDOW1		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
257	300056010	W49B_West	287.77938	9.11004	287.18099	9.02641	290.65822	31.2831	43.27412	-0.18156	67.99979	60430.95699	2024-04-30 22:58:04	60438.36324	2024-05-08 08:43:04	323.191	100.000	323.191	274.973	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		274.973	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-27 05:26:49	2025-08-31 00:00:00	2024-05-18 20:14:38	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000084	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.	SUPERNOVA REMNANTS	3	A	XRISM Collaboration		JAP	0	NOR	TRACING A MISSING BRANCH IN THE SNR EVOLUTION: RECOMBINING PLASMA IN W49B	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300056010/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
258	300055010	W49B_East	287.79356	9.09746	287.19512	9.01376	290.67235	31.26866	43.26944	-0.19979	67.99998	60423.07088	2024-04-23 01:42:04	60430.95699	2024-04-30 22:58:04	332.527	100.000	332.527	272.655	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		272.655	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 05:59:21	2025-08-31 00:00:00	2024-05-15 06:53:31	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000084	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.	SUPERNOVA REMNANTS	3	A	XRISM Collaboration		JAP	0	NOR	TRACING A MISSING BRANCH IN THE SNR EVOLUTION: RECOMBINING PLASMA IN W49B	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300055010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
259	100009140	Cyg_X-2_6p0_270	326.19015	38.42065	325.67259	38.19006	346.79142	48.03582	87.40622	-11.25149	97.99888	60422.86046	2024-04-22 20:39:04	60423.07088	2024-04-23 01:42:04	11.454	-999.000	11.454	0.149	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		9.751	0.000	0.149	0.000	11110	313430	11310	PROCESSED	2024-09-25 20:33:26	2025-08-31 00:00:00	2024-05-04 03:22:05	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009140/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
260	100009130	Cyg_X-2_4p5_270	326.18557	38.39637	325.66791	38.16579	346.76881	48.01649	87.38712	-11.26736	97.99948	60422.72713	2024-04-22 17:27:04	60422.86046	2024-04-22 20:39:04	7.696	-999.000	7.696	0.104	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		6.829	0.000	0.104	0.000	11110	313430	11310	PROCESSED	2024-09-26 04:04:57	2025-08-31 00:00:00	2024-05-04 03:24:49	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009130/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
261	100009120	Cyg_X-2_3p0_270	326.18113	38.37132	325.66338	38.14076	346.7458	47.99643	87.3676	-11.28388	98.00004	60422.59380	2024-04-22 14:15:04	60422.72713	2024-04-22 17:27:04	7.614	-999.000	7.614	0.095	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		6.245	0.000	0.095	0.000	11110	313430	11310	PROCESSED	2024-09-26 03:20:24	2025-08-31 00:00:00	2024-05-02 08:08:51	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009120/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
262	100009110	Cyg_X-2_1p8_270	326.17789	38.35167	325.66007	38.12112	346.728	47.98059	87.35243	-11.29696	97.99977	60422.26880	2024-04-22 06:27:04	60422.59380	2024-04-22 14:15:04	13.598	-999.000	13.598	0.138	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		9.030	0.000	0.138	0.000	11110	313430	11310	PROCESSED	2024-09-26 03:26:32	2025-08-31 00:00:00	2024-05-02 08:41:04	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009110/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
263	100009100	Cyg_X-2_6p0_315	326.27453	38.38189	325.75652	38.15108	346.8487	47.96945	87.43082	-11.32424	97.99907	60422.06394	2024-04-22 01:32:04	60422.26880	2024-04-22 06:27:04	9.290	-999.000	9.290	0.101	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		6.613	0.000	0.101	0.000	11110	313430	11310	PROCESSED	2024-09-25 18:58:06	2025-08-31 00:00:00	2024-05-02 07:44:39	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009100/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
264	100009090	Cyg_X-2_4p5_315	326.24898	38.36689	325.731	38.13614	346.81163	47.9663	87.40538	-11.32232	97.999	60421.92852	2024-04-21 22:17:04	60422.06394	2024-04-22 01:32:04	7.812	-999.000	7.812	0.098	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		6.399	0.000	0.098	0.000	11110	313430	11310	PROCESSED	2024-09-22 19:56:28	2025-08-31 00:00:00	2024-05-02 07:09:44	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009090/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
265	100009080	Cyg_X-2_3p0_315	326.22317	38.35188	325.7052	38.1212	346.77427	47.96325	87.37976	-11.32024	97.99954	60421.79519	2024-04-21 19:05:04	60421.92852	2024-04-21 22:17:04	7.854	5.000	7.854	0.106	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		6.921	0.000	0.106	0.000	11110	313430	11310	PROCESSED	2024-09-22 19:55:20	2025-08-31 00:00:00	2024-05-01 11:01:45	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009080/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
266	100009070	Cyg_X-2_3p0_225	326.13407	38.36187	325.61643	38.13144	346.69087	48.00643	87.33299	-11.2666	98.0002	60421.66185	2024-04-21 15:53:04	60421.79519	2024-04-21 19:05:04	7.873	2.000	7.873	0.106	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		6.935	0.000	0.106	0.000	11110	313430	11310	PROCESSED	2024-09-22 16:27:43	2025-08-31 00:00:00	2024-05-01 11:37:10	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009070/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
267	100009060	Cyg_X-2_3p0_135	326.12183	38.29173	325.60391	38.06133	346.62669	47.95016	87.27837	-11.3129	97.99965	60421.34102	2024-04-21 08:11:04	60421.66185	2024-04-21 15:53:04	12.976	21.000	12.976	0.150	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		9.790	0.000	0.150	0.000	11110	313430	11310	PROCESSED	2024-09-22 13:57:38	2025-08-31 00:00:00	2024-05-01 11:50:56	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009060/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
268	100009050	Cyg_X-2_3p0_45	326.21123	38.28186	325.69298	38.05122	346.71054	47.90697	87.32545	-11.36666	97.99915	60421.13755	2024-04-21 03:18:04	60421.34102	2024-04-21 08:11:04	8.328	4.000	8.328	0.087	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		5.703	0.000	0.087	0.000	11110	313430	11310	PROCESSED	2024-09-26 07:52:48	2025-08-31 00:00:00	2024-05-01 11:30:24	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009050/	WINDOW1BURST		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
269	100009040	Cyg_X-2_1p8_315	326.20292	38.33973	325.68496	38.10911	346.74469	47.96052	87.35942	-11.31889	97.99946	60420.99588	2024-04-20 23:54:04	60421.13755	2024-04-21 03:18:04	7.505	2.000	7.505	0.085	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		5.545	0.000	0.085	0.000	11110	313430	11310	PROCESSED	2024-09-22 08:25:52	2025-08-31 00:00:00	2024-05-01 06:41:06	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009040/	WINDOW1BURST		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
270	100009030	Cyg_X-2_1p8_225	326.1495	38.34599	325.63173	38.11551	346.69487	47.98665	87.33155	-11.28652	97.99972	60420.86255	2024-04-20 20:42:04	60420.99588	2024-04-20 23:54:04	8.038	2.000	8.038	0.108	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		7.032	0.000	0.108	0.000	11110	313430	11310	PROCESSED	2024-09-22 05:37:33	2025-08-31 00:00:00	2024-05-01 06:43:38	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009030/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
271	100009020	Cyg_X-2_1p8_135	326.14225	38.30401	325.62432	38.07355	346.65655	47.95294	87.29891	-11.31428	97.99947	60420.72852	2024-04-20 17:29:04	60420.86255	2024-04-20 20:42:04	8.072	2.000	8.072	0.108	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		7.045	0.000	0.108	0.000	11110	313430	11310	PROCESSED	2024-09-22 04:46:07	2025-08-31 00:00:00	2024-04-30 05:58:03	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009020/	WINDOW1BURST		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
272	100009010	Cyg_X-2_1p8_45	326.19472	38.29745	325.6766	38.06685	346.70519	47.92692	87.32602	-11.3464	97.99885	60420.37782	2024-04-20 09:04:04	60420.72852	2024-04-20 17:29:04	16.524	2.000	16.524	0.181	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31200010		11.835	0.000	0.181	0.000	11110	313430	11310	PROCESSED	2024-09-26 07:54:59	2025-08-31 00:00:00	2024-04-30 06:12:19	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100009010/	WINDOW1BURST		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
273	100008020	Cygnus_Loop	312.70478	31.89017	312.19138	31.70229	327.82296	47.12908	74.92085	-7.76825	88.01651	60419.25005	2024-04-19 06:00:04	60420.37782	2024-04-20 09:04:04	53.276	30.000	53.276	37.795	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	40.427	37.795	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 07:43:35	2025-08-31 00:00:00	2024-04-28 12:12:37	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100008020/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
274	100008010	Cygnus_Loop	312.70472	31.89003	312.19131	31.70215	327.8228	47.12897	74.9207	-7.76829	87.99898	60418.26810	2024-04-18 06:26:04	60419.25005	2024-04-19 06:00:04	51.640	30.000	51.640	37.910	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		37.910	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 19:11:55	2025-08-31 00:00:00	2024-04-28 11:37:47	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100008010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
275	300039010	4U1916-053	289.69838	-5.23805	289.03332	-5.33038	290.52657	16.80856	31.35731	-8.46261	79.97322	60415.43894	2024-04-15 10:32:04	60418.26810	2024-04-18 06:26:04	113.852	50.000	113.852	93.806	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	100.340	93.806	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 18:17:37	2025-08-31 00:00:00	2024-04-28 13:02:25	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000064	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.	BH AND NS BINARIES	3	A	XRISM Collaboration		JAP	0	NOR	MAPPING THE ACCRETION DISC WITH IONISED PLASMAS IN DIPPING SOURCES	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300039010/	WINDOW2	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
276	300041010	SS433	287.95612	4.98315	287.33829	4.89874	290.19541	27.17226	39.69429	-2.24405	80.53479	60410.57019	2024-04-10 13:41:04	60415.43894	2024-04-15 10:32:04	206.351	80.000	206.351	184.118	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		184.118	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 20:37:55	2025-08-31 00:00:00	2024-04-24 19:27:28	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000066	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.	BH AND NS BINARIES	3	A	XRISM Collaboration		JAP	0	NOR	INVESTIGATING JET STRUCTURE OF SS 433	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300041010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
277	300049010	CYGNUS_X-1	299.58968	35.20116	299.11966	35.06469	313.67244	54.24553	71.33434	3.06704	89.7827	60407.70491	2024-04-07 16:55:04	60410.57019	2024-04-10 13:41:04	132.023	100.000	132.023	15.088	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	32000010	120.455	0.000	0.000	15.088	11110	313430	11310	PROCESSED	2024-09-24 23:32:16	2025-08-31 00:00:00	2024-04-23 17:23:35	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000075	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.	BH AND NS BINARIES	3	A	XRISM Collaboration		JAP	0	NOR	WARPS, WINDS, AND REFLECTION IN THE BLACK HOLE CYGNUS X-1	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300049010/	WINDOW2BURST	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
278	300013030	3C397	286.91107	7.12972	286.30349	7.05014	289.3559	29.43974	41.12055	-0.33236	103.00106	60405.30352	2024-04-05 07:17:04	60407.70491	2024-04-07 16:55:04	103.517	100.000	103.517	94.405	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		94.405	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 19:00:04	2025-08-31 00:00:00	2024-04-23 16:23:06	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000031	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.	SUPERNOVA REMNANTS	3	C	XRISM Collaboration		JAP	0	NOR	PROBING CENTRAL DENSITY OF TYPE IA SUPERNOVA PROGENITOR IN SINGLE DEGENERATE SYSTEM BY AN OBSERVATION OF 3C 397	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300013030/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
279	300040020	4U1624-490	247.01035	-49.19849	246.07427	-49.08763	253.34345	-27.08001	334.91438	-0.26245	115.99714	60404.17088	2024-04-04 04:06:04	60405.30352	2024-04-05 07:17:04	63.708	50.000	63.708	52.483	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	56.139	52.483	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 17:09:10	2025-08-31 00:00:00	2024-04-23 15:05:30	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000064	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.	BH AND NS BINARIES	3	A	XRISM Collaboration		JAP	0	NOR	MAPPING THE ACCRETION DISC WITH IONISED PLASMAS IN DIPPING SOURCES	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300040020/	WINDOW2	WINDOW1	2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
280	300013020	3C397	286.91121	7.12974	286.30363	7.05016	289.35606	29.43974	41.12064	-0.33247	103.00103	60400.10769	2024-03-31 02:35:04	60404.17088	2024-04-04 04:06:04	185.886	100.000	185.886	175.923	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		175.923	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 18:48:38	2025-08-31 00:00:00	2024-04-23 20:31:31	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000031	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.	SUPERNOVA REMNANTS	3	C	XRISM Collaboration		JAP	0	NOR	PROBING CENTRAL DENSITY OF TYPE IA SUPERNOVA PROGENITOR IN SINGLE DEGENERATE SYSTEM BY AN OBSERVATION OF 3C 397	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300013020/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
281	300040010	4U1624-490	247.01205	-49.19808	246.07597	-49.08723	253.34459	-27.07941	334.91544	-0.26297	126.997	60398.96324	2024-03-29 23:07:04	60400.10769	2024-03-31 02:35:04	81.260	50.000	81.260	60.018	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	64.198	60.018	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 19:18:07	2025-08-31 00:00:00	2024-04-23 11:57:17	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000064	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.	BH AND NS BINARIES	3	A	XRISM Collaboration		JAP	0	NOR	MAPPING THE ACCRETION DISC WITH IONISED PLASMAS IN DIPPING SOURCES	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300040010/	WINDOW2	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
282	300013010	3C397	286.91133	7.12976	286.30375	7.05018	289.3562	29.43974	41.12071	-0.33257	103.00104	60394.69032	2024-03-25 16:34:04	60398.96324	2024-03-29 23:07:04	206.209	100.000	206.209	195.229	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		195.229	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 04:05:10	2025-08-31 00:00:00	2024-04-23 18:23:00	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000031	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.	SUPERNOVA REMNANTS	3	C	XRISM Collaboration		JAP	0	NOR	PROBING CENTRAL DENSITY OF TYPE IA SUPERNOVA PROGENITOR IN SINGLE DEGENERATE SYSTEM BY AN OBSERVATION OF 3C 397	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300013010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
283	300065010	Cyg_X-3	308.10708	40.95864	307.65646	40.78771	328.60334	56.90753	79.84605	0.70079	112.25882	60393.25282	2024-03-24 06:04:04	60394.69032	2024-03-25 16:34:04	67.339	40.000	67.339	8.116	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	32000010	64.791	0.000	0.000	8.116	11110	313430	11310	PROCESSED	2024-09-23 16:29:55	2025-08-31 00:00:00	2024-04-23 11:22:30	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000089	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.	BH AND NS BINARIES	3	A	XRISM Collaboration		JAP	0	NOR	UNVEILING THE BLACK HOLE IN CYG X-3	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300065010/	WINDOW2BURST	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
284	300063010	Tycho_S	6.33423	64.08731	5.63416	63.81051	42.78744	53.71286	120.08457	1.35996	183.69221	60392.22296	2024-03-23 05:21:04	60393.25282	2024-03-24 06:04:04	54.967	20.000	54.967	49.870	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		49.870	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-25 02:31:49	2025-08-31 00:00:00	2024-04-23 10:05:03	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000088	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.	SUPERNOVA REMNANTS	3	C	XRISM Collaboration		JAP	0	NOR	XRISM OBSERVATIONS OF TYCHO'S SUPERNOVA REMNANT	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300063010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
285	300062010	Tycho_N	6.33397	64.19052	5.63363	63.91371	42.904	53.78968	120.0949	1.46264	184.87293	60391.14519	2024-03-22 03:29:04	60392.22296	2024-03-23 05:21:04	53.447	20.000	53.447	50.351	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		50.351	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 00:26:08	2025-08-31 00:00:00	2024-04-20 09:50:31	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000088	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.	SUPERNOVA REMNANTS	3	C	XRISM Collaboration		JAP	0	NOR	XRISM OBSERVATIONS OF TYCHO'S SUPERNOVA REMNANT	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300062010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
286	100007020	Crab_stray_weak	82.59063	21.75217	81.8401	21.71447	83.11846	-1.5103	184.25587	-6.74075	241.89054	60389.62296	2024-03-20 14:57:04	60391.14519	2024-03-22 03:29:04	64.471	-999.000	64.471	51.418	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		51.418	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-20 16:14:41	2025-08-31 00:00:00	2024-04-20 13:23:44	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100007020/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
287	100007010	Crab_stray_strong	82.5906	21.75153	81.84007	21.71382	83.1184	-1.51094	184.2564	-6.74112	293.31136	60389.42366	2024-03-20 10:10:04	60389.62296	2024-03-20 14:57:04	11.003	45.000	11.003	9.952	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		9.952	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 16:09:26	2025-08-31 00:00:00	2024-04-20 09:37:34	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100007010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
288	100006050	Crab_SWoffset	83.6203	22.00251	82.8681	21.96976	84.08513	-1.30589	184.56125	-5.80079	269.99998	60389.19380	2024-03-20 04:39:04	60389.42366	2024-03-20 10:10:04	13.101	5.000	13.101	0.181	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	OFF	OFF	2	31200010		11.809	0.000	0.181	0.000	11110	313430	11310	PROCESSED	2024-09-21 11:49:25	2025-08-31 00:00:00	2024-04-20 04:27:54	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100006050/	WINDOW1BURST		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
289	100006040	Crab_SEoffset	83.64819	22.00182	82.89599	21.96921	84.11094	-1.30771	184.57575	-5.77931	270.00225	60388.75769	2024-03-19 18:11:04	60389.19380	2024-03-20 04:39:04	15.333	5.000	15.333	0.174	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	OFF	OFF	2	31200010		11.347	0.000	0.174	0.000	11110	313430	11310	PROCESSED	2024-09-21 11:38:04	2025-08-31 00:00:00	2024-04-20 05:13:31	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100006040/	WINDOW1BURST		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
290	100006030	Crab_NWoffset	83.62066	22.02802	82.86832	21.99528	84.08659	-1.28041	184.53977	-5.78685	270.00058	60388.49032	2024-03-19 11:46:04	60388.75769	2024-03-19 18:11:04	13.527	5.000	13.527	0.169	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	OFF	OFF	2	31200010		11.066	0.000	0.169	0.000	11110	313430	11310	PROCESSED	2024-09-26 01:11:21	2025-08-31 00:00:00	2024-04-03 15:20:55	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100006030/	WINDOW1BURST		5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
291	100006020	Crab_NEoffset_1	83.6479	22.02734	82.89556	21.99473	84.1118	-1.28221	184.55394	-5.76588	270.00172	60388.15699	2024-03-19 03:46:04	60388.49032	2024-03-19 11:46:04	17.889	9.000	17.889	0.245	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	OFF	OFF	2	31200010		16.035	0.000	0.245	0.000	11110	313430	11310	PROCESSED	2024-09-26 02:30:03	2025-08-31 00:00:00	2024-04-20 04:39:48	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100006020/	WINDOW1BURST		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
292	100006010	Crab_NEoffset_2	83.66076	22.04336	82.90832	22.0108	84.12441	-1.26673	184.54675	-5.74724	270.00189	60387.56324	2024-03-18 13:31:04	60388.15699	2024-03-19 03:46:04	23.017	9.000	23.017	0.281	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	OFF	OFF	2	31200010		18.352	0.000	0.281	0.000	11110	313430	11310	PROCESSED	2024-09-22 11:34:44	2025-08-31 00:00:00	2024-04-20 04:35:26	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100006010/	WINDOW1BURST		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
293	100001010	G21.5-0.9	278.38936	-10.56832	277.69706	-10.60728	278.45185	12.62517	21.50075	-0.88483	104.00109	60386.07782	2024-03-17 01:52:04	60387.56324	2024-03-18 13:31:04	66.954	75.000	66.954	57.927	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		57.927	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 09:44:52	2025-08-31 00:00:00	2024-04-20 06:08:17	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100001010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
294	300072010	PDS456	262.08175	-14.26541	261.37104	-14.22535	262.23203	8.96062	10.39188	11.16421	92.97208	60379.98269	2024-03-10 23:35:04	60386.07782	2024-03-17 01:52:04	264.056	150.000	264.056	223.860	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	300000A0		223.860	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-25 07:56:52	2025-08-31 00:00:00	2024-04-20 18:21:37	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000100	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.	NON-JET-DOMINATED AGN	3	A	XRISM Collaboration		JAP	0	NOR	THE DEFINITIVE PROOF OF AN ULTRA-FAST OUTFLOW	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300072010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
295	100011012	HR1099	54.19738	0.58763	53.55479	0.42349	51.97893	-18.25131	184.91165	-41.56856	264.66644	60378.81324	2024-03-09 19:31:04	60379.98269	2024-03-10 23:35:04	54.764	50.000	54.764	8.060	PX_MIDRES	N	Y	N	N	Y	Y	Y	BRIGHT	OFF	BRIGHT	OFF	1	30000010		43.015	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-16 00:45:20	2025-08-31 00:00:00	2024-04-20 15:49:50	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000008001		CALIBRATION	1	A	ERIC MILLER		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100011012/	WINDOW1		4	Observation Log: No remarks ; Pre-pipeline Log: A WRONG EXPOSURE LONGER THAN A DURATION MAY BE RECORDED DUE TO THE DATA INCLUSION OF BOTH DATAMODE=PX_NORMAL AND PX_MIDRES.
296	100011011	HR1099	54.19757	0.5876	53.55498	0.42346	51.97911	-18.25138	184.91183	-41.56843	264.66607	60376.54241	2024-03-07 13:01:04	60378.81324	2024-03-09 19:31:04	217.501	50.000	217.501	102.669	PX_NORMAL	N	Y	N	N	Y	Y	Y	BRIGHT	OFF	BRIGHT	OFF	1	30000010		102.669	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 10:26:27	2025-08-31 00:00:00	2024-04-20 20:38:52	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	ERIC MILLER		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100011011/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: A WRONG EXPOSURE LONGER THAN A DURATION MAY BE RECORDED DUE TO THE DATA INCLUSION OF BOTH DATAMODE=PX_NORMAL AND PX_MIDRES.
297	100011010	HR1099	54.19747	0.58757	53.55488	0.42343	51.979	-18.25139	184.91178	-41.56853	264.66588	60375.01880	2024-03-06 00:27:04	60376.54241	2024-03-07 13:01:04	0.000	50.000	0.000	68.753	PX_NORMAL	N	Y	N	N	Y	Y	Y	BRIGHT	OFF	OFF	OFF	1	30000010		68.753	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 01:05:11	2025-08-31 00:00:00	2024-04-04 00:31:26	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	ERIC MILLER		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100011010/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
298	300060010	Tycho_Center	6.33388	64.13847	5.63369	63.86166	42.84504	53.75101	120.08959	1.41086	219.35997	60371.36880	2024-03-02 08:51:04	60375.01880	2024-03-06 00:27:04	183.921	75.000	183.921	169.090	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		169.090	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-25 10:11:26	2025-08-31 00:00:00	2024-04-20 20:00:29	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000088	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.	SUPERNOVA REMNANTS	3	A	XRISM Collaboration		JAP	0	NOR	XRISM OBSERVATIONS OF TYCHO'S SUPERNOVA REMNANT	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300060010/	WINDOW1		2	Observation Log: No remarks ; Pre-pipeline Log: No remarks
299	300045010	Galactic_Center_2	266.55713	-28.88941	265.76313	-28.87076	266.97212	-5.4863	0.10924	-0.08937	80.00106	60369.41741	2024-02-29 10:01:04	60371.36880	2024-03-02 08:51:04	76.817	100.000	76.817	63.254	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		63.254	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 00:19:05	2025-08-31 00:00:00	2024-03-14 12:27:56	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000072	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.	GALACTIC DIFFUSE EMISSION AND SURVEYS	3	A	XRISM Collaboration		JAP	0	NOR	INVESTIGATION OF THE ACTIVITIES IN THE GALACTIC CENTER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300045010/	WINDOW1		5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
300	300044010	Galactic_Center_1	266.42149	-28.99699	265.62684	-28.97768	266.85554	-5.59675	359.95561	-0.044	89.58787	60366.02852	2024-02-26 00:41:04	60369.41741	2024-02-29 10:01:04	132.142	100.000	132.142	107.877	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		107.877	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-27 02:10:03	2025-08-31 00:00:00	2024-03-14 13:43:56	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000072	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.	GALACTIC DIFFUSE EMISSION AND SURVEYS	3	A	XRISM Collaboration		JAP	0	NOR	INVESTIGATION OF THE ACTIVITIES IN THE GALACTIC CENTER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300044010/	WINDOW1		5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
301	300036010	GX13+1	273.63051	-17.15669	272.90389	-17.17256	273.48944	6.23864	13.51673	0.1075	91.39026	60365.04935	2024-02-25 01:11:04	60366.02852	2024-02-26 00:41:04	38.274	30.000	38.274	27.916	PX_NORMAL	N	Y	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	29.860	27.916	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 13:18:40	2025-08-31 00:00:00	2024-03-10 11:27:59	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000059	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.	BH AND NS BINARIES	3	A	XRISM Collaboration		JAP	0	NOR	THE LAUNCH MECHANISM OF ACCRETION DISC WINDS: THE BEST TESTS FROM THE NEUTRON STAR BINARIES GX13+1 AND 2S0921-630	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300036010/	WINDOW2	WINDOW1	5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
302	300075010	NGC1365	53.40257	-36.1399	52.9252	-36.30686	36.80618	-53.03435	237.95517	-54.5973	268.77822	60360.51602	2024-02-20 12:23:04	60365.04935	2024-02-25 01:11:04	213.118	125.000	213.118	171.316	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	183.247	171.316	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-25 04:42:36	2025-08-31 00:00:00	2024-03-07 15:48:48	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000103	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.	NON-JET-DOMINATED AGN	3	A	XRISM Collaboration		JAP	0	NOR	STUDYING PHOTOIONISED OUTFLOWS IN A LUMINOUS STAR-FORMING AGN	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300075010/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
303	100010010	1E0102.2-7219	16.00975	-72.03121	15.60483	-72.29918	314.63728	-65.03641	301.55655	-45.06337	312.83833	60359.51671	2024-02-19 12:24:04	60360.51602	2024-02-20 12:23:04	43.357	30.000	43.357	33.628	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	OFF	OFF	1	31100010	32000010	36.015	33.628	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-26 05:25:45	2025-08-31 00:00:00	2024-03-08 11:01:01	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		CALIBRATION	1	A	XRISM Collaboration		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/1/100010010/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
304	300080010	SN1006	225.56502	-41.98188	224.74727	-41.78551	235.35256	-23.73853	327.45194	14.57726	109.00052	60358.56532	2024-02-18 13:34:04	60359.51671	2024-02-19 12:24:04	43.529	20.000	43.529	38.067	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	OFF	OFF	1	30000010		38.067	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-20 21:27:29	2025-08-31 00:00:00	2024-02-28 23:17:26	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000015	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.	SUPERNOVA REMNANTS	3	A	XRISM Collaboration		JAP	0	NOR	COLLISIONLESS SHOCK HEATING AND NON-EQUILIBRIUM PLASMA IN SN 1006	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300080010/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
305	300005010	Kepler_SNR	262.66411	-21.48209	261.91487	-21.44474	263.17291	1.78351	4.52182	6.82944	90.00056	60357.23269	2024-02-17 05:35:04	60358.56532	2024-02-18 13:34:04	55.337	50.000	55.337	46.304	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		46.304	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 23:11:27	2025-08-31 00:00:00	2024-03-01 03:03:27	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000016	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.	SUPERNOVA REMNANTS	3	C	XRISM Collaboration		JAP	0	NOR	THE PROGENITOR SYSTEM AND EXPLOSION PHYSICS FOR KEPLER'S SNR	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300005010/	WINDOW1		6	Observation Log: No remarks ; Pre-pipeline Log: No remarks
306	900001010	4U1630-472	248.50661	-47.3929	247.58559	-47.28878	254.09902	-25.13311	336.9113	0.25035	91.78994	60356.03546	2024-02-16 00:51:04	60357.23269	2024-02-17 05:35:04	52.732	40.000	52.732	6.015	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	32000010	48.018	0.000	0.000	6.015	11110	313430	11310	PROCESSED	2024-09-21 00:12:55	2025-08-31 00:00:00	2024-02-22 13:20:22	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000009001	We propose two ToO observations of a Galactic transient black hole X-ray binary with a high inclination angle, at different spectral states during its outburst. The main science goal is to understand the launching mechanism of disk winds in black hole X-ray binaries and the evolution of the wind structure in their outbursts. Resolve 50 ks observations enable us to obtain the velocity structure of the winds by resolving the detailed profiles of Fe XXV He alpha and Fe XXVI Ly alpha absorption lines. The line profile can also constrain the geometry of the wind, which makes possible to accurately estimate the mass loss rate. Resolve is also capable of detecting weak absorption lines in the states where significant lines have rarely been observed.	BH AND NS BINARIES	9	A	XRISM Collaboration		DDT	0	DDT-TOO	UNDERSTANDING DISK WINDS IN TRANSIENT BLACK HOLE X-RAY BINARIES	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/9/900001010/	WINDOW2BURST	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
307	300028010	Circinus_X-1	230.17057	-57.16647	229.20194	-56.9863	244.13333	-37.24938	322.1188	0.03782	103.99338	60355.26324	2024-02-15 06:19:04	60356.03546	2024-02-16 00:51:04	34.906	40.000	34.906	26.215	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	28.041	26.215	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 05:30:52	2025-08-31 00:00:00	2024-02-21 19:30:30	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000054	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.	BH AND NS BINARIES	3	C	XRISM Collaboration		JAP	0	NOR	DYNAMIC CHANGE OF ACCRETION STRUCTURE IN THE YOUNGEST X-RAY BINARY CIRCINUS X-1 HOSTING A WEAKLY MAGNETIZED NEUTRON STAR	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300028010/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
308	300003010	Cen_X-3	170.31269	-60.62389	169.7572	-60.34961	209.25896	-56.34036	292.09029	0.33539	156.79982	60352.99727	2024-02-12 23:56:04	60355.26324	2024-02-15 06:19:04	169.162	90.000	169.162	148.954	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	159.332	148.954	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 18:19:17	2025-08-31 00:00:00	2024-02-21 23:55:29	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000012	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.	BH AND NS BINARIES	3	A	XRISM Collaboration		JAP	0	NOR	MAPPING WIND MASS LOSS IN A NEUTRON STAR HOSTING BINARY WITH X-RAYS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300003010/	WINDOW2	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
309	000162000	Circinus_Galaxy	213.29011	-65.33927	212.32257	-65.10519	238.61027	-47.96236	311.32543	-3.80794	114.47734	60348.47088	2024-02-08 11:18:04	60352.99727	2024-02-12 23:56:04	328.030	100.000	328.030	286.818	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	306.795	286.818	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 00:16:21	2025-08-31 00:00:00	2024-03-04 02:22:31	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000058	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.	NON-JET-DOMINATED AGN	0	A	XRISM Collaboration		JAP	0	NOR	UNVEILING NATURE OF COMPTON-THICK TORUS IN CIRCINUS GALAXY	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000162000/	WINDOW2	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
310	000161000	MCG-6-30-15	203.97365	-34.29511	203.25725	-34.03997	215.17974	-22.54666	313.292	27.68072	118.12164	60345.94727	2024-02-05 22:44:04	60348.47088	2024-02-08 11:18:04	150.007	100.000	150.007	114.666	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	31100010	32000010	122.702	114.666	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 15:15:27	2025-08-31 00:00:00	2024-03-02 15:55:42	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000074	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.	NON-JET-DOMINATED AGN	0	A	XRISM Collaboration		JAP	0	NOR	A DETAILED EXPLORATION OF REFLECTION AND ABSORPTION IN MCG 6-30-15 WITH XRISM	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000161000/	WINDOW2	WINDOW1	6	Observation Log: No remarks ; Pre-pipeline Log: No remarks
311	000160000	Tycho_NW	6.23264	64.16759	5.53337	63.89074	42.82251	53.80219	120.04864	1.44434	226.36684	60342.34519	2024-02-02 08:17:04	60345.94727	2024-02-05 22:44:04	217.863	75.000	217.863	194.561	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		194.561	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 16:55:54	2025-08-31 00:00:00	2024-02-18 11:50:08	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000088	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.	SUPERNOVA REMNANTS	0	A	XRISM Collaboration		JAP	0	NOR	XRISM OBSERVATIONS OF TYCHO'S SUPERNOVA REMNANT	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000160000/	WINDOW1		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
312	000159000	V834_Cen	212.27978	-45.28775	211.49113	-45.05129	226.52756	-30.16886	316.97798	15.45485	110.1644	60338.70838	2024-01-29 17:00:04	60342.34519	2024-02-02 08:17:04	189.113	100.000	189.113	128.322	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	137.259	128.322	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 07:38:03	2025-08-31 00:00:00	2024-02-15 13:13:08	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000026	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.	ACCRETING WHITE DWARFS AND NOVAE	0	A	XRISM Collaboration		JAP	0	NOR	NEW PLASMA DIAGNOSTICS USING RESONANCE LINES ON MCV PLASMA	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000159000/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
313	000158000	Perseus_O1	49.76693	41.57609	48.93955	41.39479	58.48264	22.43805	150.42143	-13.28312	262.87788	60335.88199	2024-01-26 21:10:04	60338.70838	2024-01-29 17:00:04	139.965	80.000	139.965	117.853	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		117.853	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 20:28:28	2025-08-31 00:00:00	2024-02-09 13:54:19	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000055	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.	GROUPS AND CLUSTERS OF GALAXIES	0	A	Irina Zhuravleva		JAP	0	NOR	XRISM OBSERVATIONS OF THE PERSEUS CLUSTER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000158000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
314	000157000	Perseus_M1	49.82903	41.55406	49.00162	41.37298	58.5243	22.40399	150.47375	-13.276	262.87754	60333.70560	2024-01-24 16:56:04	60335.88199	2024-01-26 21:10:04	105.138	50.000	105.138	88.997	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		88.997	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 09:25:48	2025-08-31 00:00:00	2024-02-09 13:25:13	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000055	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.	GROUPS AND CLUSTERS OF GALAXIES	0	A	Irina Zhuravleva		JAP	0	NOR	XRISM OBSERVATIONS OF THE PERSEUS CLUSTER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000157000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
315	000156000	Perseus_C1	49.88895	41.53412	49.0615	41.35326	58.56492	22.37238	150.5235	-13.26797	262.87835	60332.37227	2024-01-23 08:56:04	60333.70560	2024-01-24 16:56:04	63.848	50.000	63.848	58.541	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		58.541	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-25 23:52:57	2025-08-31 00:00:00	2024-02-09 11:46:58	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000055	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.	GROUPS AND CLUSTERS OF GALAXIES	0	A	Irina Zhuravleva		JAP	0	NOR	XRISM OBSERVATIONS OF THE PERSEUS CLUSTER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000156000/	WINDOW1		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
316	000155000	Perseus_CAL2	49.95077	41.5116	49.12329	41.33097	58.60626	22.33793	150.57593	-13.26126	264.59714	60331.23338	2024-01-22 05:36:04	60332.37227	2024-01-23 08:56:04	55.927	40.000	55.927	45.189	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	48.337	45.189	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 18:04:56	2025-08-31 00:00:00	2024-02-03 06:37:50	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		GROUPS AND CLUSTERS OF GALAXIES	0	A	Eric Miller		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000155000/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
317	000154000	Perseus_CAL1	49.95068	41.51173	49.1232	41.3311	58.60623	22.33807	150.5758	-13.26119	264.61419	60330.02157	2024-01-21 00:31:04	60331.23338	2024-01-22 05:36:04	50.733	40.000	50.733	47.103	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		47.103	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 11:47:55	2025-08-31 00:00:00	2024-02-02 11:07:11	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		GROUPS AND CLUSTERS OF GALAXIES	0	A	Eric Miller		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000154000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
318	000153400	Abell2319_BS	289.76199	44.10466	289.37503	44.01141	305.27871	65.14175	75.67284	13.91885	170.0338	60329.06527	2024-01-20 01:33:59	60330.02157	2024-01-21 00:31:04	0.000	-999.000	0.000	41.213	PX_NORMAL	N	Y	N	N	N	N	Y	BRIGHT	OFF	OFF	OFF	1	30000010		41.213	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-28 11:40:04	2025-08-31 00:00:00	2024-01-28 20:31:42	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	MAKOTO TASHIRO		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000153400/	WINDOW1		4	Observation Log: No remarks ; Pre-pipeline Log: A WRONG EXPOSURE LONGER THAN A DURATION MAY BE RECORDED DUE TO THE DATA INCLUSION OF BOTH DATAMODE=PX_NORMAL AND PX_MIDRES.
319	000153300	Abell2319_BS	289.76201	44.1047	289.37505	44.01145	305.27877	65.14179	75.67289	13.91886	170.03377	60328.11463	2024-01-19 02:45:04	60329.06527	2024-01-20 01:33:59	26.861	-999.000	26.861	42.010	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	BRIGHT	OFF	1	30000010		42.010	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-28 11:21:50	2025-08-31 00:00:00	2024-01-28 17:07:53	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	MAKOTO TASHIRO		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000153300/	WINDOW1		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
320	000153200	Abell2319_BS	289.76212	44.10468	289.37516	44.01143	305.27893	65.14174	75.67291	13.91878	170.03392	60327.11417	2024-01-18 02:44:24	60328.11463	2024-01-19 02:45:04	0.000	-999.000	0.000	44.383	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	BRIGHT	OFF	1	30000010		44.383	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-28 14:11:49	2025-08-31 00:00:00	2024-01-27 22:49:00	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	MAKOTO TASHIRO		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000153200/	WINDOW1		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
321	000153100	Abell2319_BS	289.76214	44.10462	289.37518	44.01137	305.27892	65.14168	75.67286	13.91874	170.03385	60324.23230	2024-01-15 05:34:31	60327.11417	2024-01-18 02:44:24	2.778	-999.000	2.778	124.476	PX_NORMAL	N	Y	N	N	Y	N	Y	OFF	OFF	BRIGHT	OFF	1	30000010		124.476	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-04-28 14:07:42	2025-08-31 00:00:00	2024-01-27 20:28:01	03.00.013.010	gen20241115_xtd20241115_rsl20241115	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	MAKOTO TASHIRO		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000153100/	WINDOW1		5	Observation Log: No remarks ; Pre-pipeline Log: A WRONG EXPOSURE LONGER THAN A DURATION MAY BE RECORDED DUE TO THE DATA INCLUSION OF BOTH DATAMODE=PX_NORMAL AND PX_MIDRES.
322	000153000	Abell2319_BS	289.76168	44.10502	289.37472	44.01178	305.27847	65.14217	75.67309	13.91921	170.03357	60324.00074	2024-01-15 00:01:04	60324.23230	2024-01-15 05:34:31	11.603	-999.000	11.603	10.479	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	OFF	OFF	1	30000010		10.479	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 10:07:32	2025-08-31 00:00:00	2024-01-27 01:56:33	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	MAKOTO TASHIRO		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000153000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
323	000152000	Abell2029_N2	227.79385	5.82502	227.1744	6.01315	223.56787	22.7208	6.63113	50.54559	105.00179	60322.81324	2024-01-13 19:31:04	60324.00074	2024-01-15 00:01:04	50.437	50.000	50.437	43.194	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		43.194	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 10:08:42	2025-08-31 00:00:00	2024-01-19 14:38:34	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000080	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.	GROUPS AND CLUSTERS OF GALAXIES	0	A	Eric Miller		JAP	0	NOR	NON-THERMAL PRESSURE SUPPORT IN RELAXED GALAXY CLUSTERS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000152000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
324	000151000	Abell2029_Center	227.73315	5.74506	227.1134	5.9334	223.53034	22.62677	6.47345	50.54616	105.00177	60322.07713	2024-01-13 01:51:04	60322.81324	2024-01-13 19:31:04	29.337	20.000	29.337	21.918	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	1	30000010		21.918	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 07:22:39	2025-08-31 00:00:00	2024-01-18 14:19:51	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000080	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.	GROUPS AND CLUSTERS OF GALAXIES	0	A	Eric Miller		JAP	0	NOR	NON-THERMAL PRESSURE SUPPORT IN RELAXED GALAXY CLUSTERS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000151000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
325	000150000	Abell2029_N1	227.76354	5.78505	227.14394	5.97329	223.54914	22.67381	6.55234	50.54588	105.00131	60319.68130	2024-01-10 16:21:04	60322.07713	2024-01-13 01:51:04	106.210	-999.000	106.210	86.086	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		86.086	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 09:07:56	2025-08-31 00:00:00	2024-01-18 20:24:07	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000080	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.	GROUPS AND CLUSTERS OF GALAXIES	0	A	Eric Miller		JAP	0	NOR	NON-THERMAL PRESSURE SUPPORT IN RELAXED GALAXY CLUSTERS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000150000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
326	000149000	Abell2029_Center	227.73412	5.74519	227.11436	5.93353	223.5313	22.62718	6.47452	50.54547	105.0018	60319.14657	2024-01-10 03:31:04	60319.68130	2024-01-10 16:21:04	16.324	20.000	16.324	12.219	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	1	30000010		12.219	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 12:57:28	2025-08-31 00:00:00	2024-01-18 10:07:39	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000080	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.	GROUPS AND CLUSTERS OF GALAXIES	0	A	Eric Miller		JAP	0	NOR	NON-THERMAL PRESSURE SUPPORT IN RELAXED GALAXY CLUSTERS	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000149000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
327	000148000	Abell2029_SW	227.57527	5.65309	226.95513	5.842	223.39644	22.49318	6.20909	50.61661	105.00218	60318.61185	2024-01-09 14:41:04	60319.14657	2024-01-10 03:31:04	27.591	-999.000	27.591	23.479	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	1	30000010		23.479	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 12:31:48	2025-08-31 00:00:00	2024-01-17 11:01:10	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		GROUPS AND CLUSTERS OF GALAXIES	0	A	Eric Miller		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000148000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
328	000147000	Abell2029_E	227.84764	5.71433	227.22781	5.90227	223.65811	22.63035	6.54195	50.43652	105.00097	60318.02852	2024-01-09 00:41:04	60318.61185	2024-01-09 14:41:04	23.026	-999.000	23.026	16.086	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	1	30000010		16.086	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 04:42:25	2025-08-31 00:00:00	2024-01-14 16:13:01	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		GROUPS AND CLUSTERS OF GALAXIES	0	A	Eric Miller		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000147000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
329	000146000	Abell2029_N	227.76517	5.858	227.14583	6.04623	223.5279	22.74409	6.64594	50.58818	105.001	60317.61185	2024-01-08 14:41:04	60318.02852	2024-01-09 00:41:04	20.112	-999.000	20.112	17.629	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		17.629	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 01:28:39	2025-08-31 00:00:00	2024-01-14 11:21:55	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		GROUPS AND CLUSTERS OF GALAXIES	0	A	Eric Miller		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000146000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
330	000145000	3C273	187.27643	2.0529	186.63706	2.32924	185.86794	4.77338	289.9473	64.36018	112.43204	60315.00074	2024-01-06 00:01:04	60317.61185	2024-01-08 14:41:04	104.516	50.000	104.516	86.689	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	92.727	86.689	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 23:45:12	2025-08-31 00:00:00	2024-01-14 06:46:17	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		BLAZARS AND OTHER JET-DOMINATED AGN	0	A	Eric Miller		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000145000/	WINDOW2	WINDOW1	8	Observation Log: No remarks ; Pre-pipeline Log: No remarks
331	000144000	Vela_X-1_6	135.52811	-40.55445	135.05456	-40.35656	157.03677	-53.92504	263.05787	3.92974	148.42006	60314.73685	2024-01-05 17:41:04	60315.00074	2024-01-06 00:01:04	14.670	-999.000	14.670	1.661	PX_NORMAL	N	Y	Y	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	32000010	13.259	0.000	0.000	1.661	11110	313430	11310	PROCESSED	2024-09-22 14:44:03	2025-08-31 00:00:00	2024-01-13 08:40:31	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000144000/	WINDOW2BURST	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
332	000143000	Vela_X-1_5	135.5276	-40.55407	135.05405	-40.35618	157.03588	-53.92489	263.05732	3.9297	152.42034	60314.33407	2024-01-05 08:01:04	60314.73685	2024-01-05 17:41:04	16.416	-999.000	16.416	1.912	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	32000010	15.261	0.000	0.000	1.912	11110	313430	11310	PROCESSED	2024-09-22 12:39:45	2025-08-31 00:00:00	2024-01-12 17:13:29	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000143000/	WINDOW2BURST	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
333	000142000	Vela_X-1_4	135.52761	-40.55406	135.05406	-40.35617	157.03588	-53.92487	263.05732	3.92971	150.42019	60314.07019	2024-01-05 01:41:04	60314.33407	2024-01-05 08:01:04	12.321	-999.000	12.321	1.189	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31300010	32000010	9.496	0.000	0.000	1.189	11110	313430	11310	PROCESSED	2024-09-22 09:36:41	2025-08-31 00:00:00	2024-01-12 11:47:10	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000142000/	WINDOW2BURST	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
334	000141000	Vela_X-1_3	135.52787	-40.55439	135.05432	-40.3565	157.03645	-53.92506	263.0577	3.92965	147.4799	60313.66741	2024-01-04 16:01:04	60314.07019	2024-01-05 01:41:04	19.172	-999.000	19.172	2.511	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	32000010	20.046	0.000	0.000	2.511	11110	313430	11310	PROCESSED	2024-09-25 21:51:42	2025-08-31 00:00:00	2024-01-11 15:43:12	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000141000/	WINDOW2BURST	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
335	000140000	Vela_X-1_2	135.52742	-40.55397	135.05387	-40.35609	157.0356	-53.92487	263.05716	3.92966	151.47972	60313.40352	2024-01-04 09:41:04	60313.66741	2024-01-04 16:01:04	10.753	-999.000	10.753	1.278	PX_NORMAL	N	N	Y	N	N	Y	Y	OFF	OFF	OFF	OFF	2	31300010	32000010	10.199	0.000	0.000	1.278	11110	313430	11310	PROCESSED	2024-09-21 23:41:07	2025-08-31 00:00:00	2024-01-11 07:59:57	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000140000/	WINDOW2BURST	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
336	000139000	Vela_X-1_1	135.5275	-40.55377	135.05395	-40.35588	157.03553	-53.92466	263.05705	3.92985	149.48041	60313.00074	2024-01-04 00:01:04	60313.40352	2024-01-04 09:41:04	19.414	-999.000	19.414	1.901	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31300010	32000010	15.175	0.000	0.000	1.901	11110	313430	11310	PROCESSED	2024-09-20 18:57:25	2025-08-31 00:00:00	2024-01-11 04:27:57	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000139000/	WINDOW2BURST	WINDOW1	14	Observation Log: No remarks ; Pre-pipeline Log: No remarks
337	000138000	Centaurus_Cluster	192.19638	-41.30043	191.50572	-41.0279	209.06692	-32.84801	302.39626	21.56856	106.67227	60306.00074	2023-12-28 00:01:04	60313.00074	2024-01-04 00:01:04	298.446	150.000	298.446	270.625	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		270.625	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 06:21:54	2025-08-31 00:00:00	2024-01-11 04:24:50	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000049	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.	GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	XRISM OBSERVATIONS OF THE CENTAURUS CLUSTER	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000138000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
338	000137000	NGC4151	182.63447	39.40651	182.00312	39.68462	164.09544	36.62401	155.07849	75.06195	106.63975	60304.71602	2023-12-26 17:11:04	60306.00074	2023-12-28 00:01:04	62.891	45.000	62.891	54.081	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	57.848	54.081	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 08:58:37	2025-08-31 00:00:00	2024-01-07 01:04:29	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000073	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.	NON-JET-DOMINATED AGN	0	A	Makoto Tashiro		JAP	0	NOR	SHAPING NEW AGN HORIZONS WITH NGC 4151	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000137000/	WINDOW2	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
339	000136000	1E0102.2-7219	16.01004	-72.03134	15.60512	-72.29931	314.63708	-65.03655	301.55644	-45.06323	251.37109	60302.95907	2023-12-24 23:01:04	60304.71602	2023-12-26 17:11:04	78.608	-999.000	78.608	64.637	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		64.637	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 08:54:27	2025-08-31 00:00:00	2024-01-07 02:18:24	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		SUPERNOVA REMNANTS	0	A	Makoto Tashiro		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000136000/	WINDOW1		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
340	000135000	RESOLVE_THERM5	319.32756	58.90574	318.98739	58.69516	4.64314	66.85943	98.21049	6.73478	227.99366	60302.00074	2023-12-24 00:01:04	60302.95907	2023-12-24 23:01:04	69.541	-999.000	69.541	65.902	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		65.902	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 02:40:21	2025-08-31 00:00:00	2024-01-07 00:20:16	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		SPECIAL OPERATIONS	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000135000/	WINDOW1		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
341	000134000	RESOLVE_THERM4	325.65334	58.89821	325.27299	58.66892	9.73943	64.35913	100.58493	4.48003	233.81333	60301.00074	2023-12-23 00:01:04	60302.00074	2023-12-24 00:01:04	75.267	-999.000	75.267	69.537	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	OFF	OFF	1	30000010		69.537	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-20 12:18:25	2025-08-31 00:00:00	2024-01-06 21:24:00	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		SPECIAL OPERATIONS	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000134000/	WINDOW1		5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
342	000133000	RESOLVE_THERM3	331.97875	58.89266	331.55518	58.64743	14.49264	61.89634	103.14972	2.45108	239.90399	60300.00074	2023-12-22 00:01:04	60301.00074	2023-12-23 00:01:04	58.201	-999.000	58.201	56.328	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	OFF	OFF	1	30000010		56.328	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 09:36:37	2025-08-31 00:00:00	2023-12-30 13:09:16	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		SPECIAL OPERATIONS	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000133000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
343	000132000	RESOLVE_THERM2	338.30644	58.89103	337.83708	58.63283	19.0049	59.48585	105.89081	0.66993	245.54281	60299.00074	2023-12-21 00:01:04	60300.00074	2023-12-22 00:01:04	17.972	-999.000	17.972	17.942	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	OFF	OFF	1	30000010		17.942	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-24 03:44:03	2025-08-31 00:00:00	2023-12-29 05:17:43	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		SPECIAL OPERATIONS	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000132000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
344	000131000	RESOLVE_THERM1	344.63042	58.88477	344.11327	58.61672	23.32844	57.13642	108.78237	-0.84971	250.99591	60298.00074	2023-12-20 00:01:04	60299.00074	2023-12-21 00:01:04	15.153	-999.000	15.153	0.199	PX_NORMAL	N	Y	N	N	N	N	Y	OFF	OFF	OFF	OFF	2	31200010		13.043	0.000	0.199	0.000	11110	313430	11310	PROCESSED	2024-09-23 23:34:58	2025-08-31 00:00:00	2023-12-28 15:12:21	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		SPECIAL OPERATIONS	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000131000/	WINDOW1BURST		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
345	000130000	Cas_A_NW	350.83062	58.82244	350.26504	58.54789	27.3752	54.86343	111.72777	-2.1192	254.05723	60292.58407	2023-12-14 14:01:04	60295.66741	2023-12-17 16:01:04	223.024	-999.000	223.024	212.498	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		212.498	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 02:35:11	2025-08-31 00:00:00	2024-01-09 18:42:12	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000069	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.	SUPERNOVA REMNANTS	0	A	Makoto Tashiro		JAP	0	NOR	OBSERVING CAS A WITH XRISM: FROM A SUPERNOVA'S INNER WORKINGS TO THE IMPRINTS OF COSMIC-RAY ACCELERATION	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000130000/	WINDOW1		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
346	000129000	Cas_A_SE	350.92213	58.80674	350.35579	58.53211	27.41678	54.81963	111.76724	-2.14981	258.51498	60289.15699	2023-12-11 03:46:04	60292.58407	2023-12-14 14:01:04	219.357	-999.000	219.357	215.207	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000010		215.207	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 16:07:51	2025-08-31 00:00:00	2023-12-22 15:37:15	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000069	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.	SUPERNOVA REMNANTS	0	A	Makoto Tashiro		JAP	0	NOR	OBSERVING CAS A WITH XRISM: FROM A SUPERNOVA'S INNER WORKINGS TO THE IMPRINTS OF COSMIC-RAY ACCELERATION	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000129000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
347	000128000	N132D	81.25879	-69.64129	81.36087	-69.68339	312.62406	-85.52214	280.30364	-32.78468	171.05364	60287.41185	2023-12-09 09:53:04	60289.15699	2023-12-11 03:46:04	75.267	50.000	75.267	52.568	PX_NORMAL	N	Y	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	56.229	52.568	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 19:46:00	2025-01-16 00:00:00	2023-12-15 16:37:24	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000999		SUPERNOVA REMNANTS	0	A	Makoto Tashiro		JAP	0	NOR	Early Release Science Targets	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000128000/	WINDOW2	WINDOW1	5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
348	000127000	PKS2155-304	329.71739	-30.22498	328.99358	-30.46454	321.19647	-16.7706	17.73155	-52.24617	256.51192	60285.00074	2023-12-07 00:01:04	60287.41185	2023-12-09 09:53:04	106.533	-999.000	106.533	84.371	PX_NORMAL	N	Y	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	90.248	84.371	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 08:13:16	2025-08-31 00:00:00	2023-12-15 17:00:15	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		BLAZARS AND OTHER JET-DOMINATED AGN	0	A	Makoto Tashiro		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000127000/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
349	000126000	N132D	81.25849	-69.64122	81.36057	-69.68332	312.62552	-85.5221	280.30359	-32.78479	171.05486	60281.91741	2023-12-03 22:01:04	60285.00074	2023-12-07 00:01:04	128.936	50.000	128.936	91.240	PX_NORMAL	N	Y	N	N	Y	N	Y	OFF	OFF	OFF	OFF	1	30000010		91.240	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 22:22:35	2025-01-16 00:00:00	2023-12-13 04:20:03	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000999		SUPERNOVA REMNANTS	0	A	Makoto Tashiro		JAP	0	NOR	Early Release Science Targets	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000126000/	WINDOW1		11	Observation Log: No remarks ; Pre-pipeline Log: No remarks
350	000125000	NGC4151	182.63493	39.40655	182.00358	39.68466	164.0958	36.62422	155.07731	75.06213	121.10456	60280.20907	2023-12-02 05:01:04	60281.91741	2023-12-03 22:01:04	79.824	45.000	79.824	33.055	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	68.232	33.055	0.000	4.118	11110	313430	11310	PROCESSED	2024-09-21 14:39:10	2025-08-31 00:00:00	2023-12-09 16:21:57	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		NON-JET-DOMINATED AGN	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000125000/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
351	000124000	LMC_X-3_Case1	84.73599	-64.08363	84.66635	-64.10937	46.00405	-86.69062	273.5757	-32.08146	163.2029	60278.29241	2023-11-30 07:01:04	60280.20907	2023-12-02 05:01:04	78.883	-999.000	78.883	60.766	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	64.999	60.766	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 12:40:38	2025-08-31 00:00:00	2023-12-07 01:52:28	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000124000/	WINDOW2	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
352	000123000	PSR_B1937+21	294.90959	21.5827	294.36863	21.46663	301.97181	42.29661	57.50805	-0.28892	233.0419	60273.35491	2023-11-25 08:31:04	60278.29241	2023-11-30 07:01:04	245.115	-999.000	245.115	210.271	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	224.916	210.271	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-20 15:30:07	2025-08-31 00:00:00	2023-12-06 10:52:35	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000123000/	WINDOW2	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
353	000122000	PSR_B1937+21_OFFSET	294.914	21.62205	294.37324	21.50596	301.98926	42.334	57.54432	-0.27311	233.65414	60272.12574	2023-11-24 03:01:04	60273.35491	2023-11-25 08:31:04	58.114	-999.000	58.114	51.123	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	54.683	51.123	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-20 13:36:01	2025-08-31 00:00:00	2023-11-29 18:52:34	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000122000/	WINDOW2	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
354	000121000	Eta_Carinae	161.26707	-59.68453	160.78051	-59.42119	202.15653	-58.92669	287.59785	-0.62906	89.78391	60271.05630	2023-11-23 01:21:04	60272.12574	2023-11-24 03:01:04	44.248	-999.000	44.248	32.871	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	35.160	32.871	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-20 10:34:35	2025-08-31 00:00:00	2023-11-29 04:23:50	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		STELLAR CORONAE, WINDS, AND YOUNG STARS	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000121000/	WINDOW2	WINDOW1	5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
355	000120000	LMC_X-3_Case1	84.73798	-64.08528	84.66838	-64.11101	45.99756	-86.69245	273.57759	-32.08049	154.42433	60270.05630	2023-11-22 01:21:04	60271.05630	2023-11-23 01:21:04	45.984	-999.000	45.984	35.784	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	38.276	35.784	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-20 10:21:15	2025-08-31 00:00:00	2023-12-10 13:32:40	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000120000/	WINDOW2	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
356	000119000	LMC_X-3_Case3	84.73837	-64.08505	84.66876	-64.11077	46.00245	-86.69237	273.5773	-32.08034	133.41325	60269.00074	2023-11-21 00:01:04	60270.05630	2023-11-22 01:21:04	48.970	-999.000	48.970	39.230	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100010	32000010	41.963	39.230	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 11:15:16	2025-08-31 00:00:00	2023-11-28 18:08:39	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000119000/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
357	000118000	1E0102.2-7219	16.00491	-72.03255	15.59993	-72.30053	314.6329	-65.03563	301.55879	-45.06214	217.73422	60267.62574	2023-11-19 15:01:04	60269.00074	2023-11-21 00:01:04	103.268	-999.000	103.268	0.000	PX_NORMAL	N	Y	N	N	Y	Y	Y	BRIGHT	OFF	OFF	OFF	1	31100070	32000070	74.936	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-23 03:18:36	2025-08-31 00:00:00	2023-11-24 16:10:19	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		SUPERNOVA REMNANTS	0	A	Makoto Tashiro		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000118000/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
358	000117000	Z_Cam	126.31989	73.11946	124.92995	73.28159	106.11468	51.70999	141.37102	32.63072	78.14335	60266.61880	2023-11-18 14:51:04	60267.62574	2023-11-19 15:01:04	52.726	-999.000	52.726	0.000	PX_NORMAL	N	Y	N	N	Y	Y	Y	BRIGHT	OFF	OFF	OFF	1	31200070		44.515	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-25 18:20:58	2025-08-31 00:00:00	2023-11-24 13:21:15	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		ACCRETING WHITE DWARFS AND NOVAE	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000117000/	WINDOW1BURST		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
359	000116000	AO_Psc	343.82289	-3.17819	343.1776	-3.44515	343.87258	3.42757	68.66931	-53.34157	248.66304	60265.57713	2023-11-17 13:51:04	60266.61880	2023-11-18 14:51:04	53.002	-999.000	53.002	44.202	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100070	32000070	47.280	44.202	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-20 17:06:58	2025-08-31 00:00:00	2023-11-23 12:28:51	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		ACCRETING WHITE DWARFS AND NOVAE	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000116000/	WINDOW2	WINDOW1	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
360	000115000	LMC_X-3_Case5	84.7376	-64.08574	84.66801	-64.11147	45.99032	-86.6927	273.57814	-32.08063	168.86754	60264.50491	2023-11-16 12:07:04	60265.57713	2023-11-17 13:51:04	50.885	-999.000	50.885	40.475	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100070	32000070	43.294	40.475	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-25 17:57:51	2025-08-31 00:00:00	2023-11-23 12:58:38	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000115000/	WINDOW2	WINDOW1	5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
361	000114000	Abell2319_BS2	289.69038	44.1639	289.30406	44.07098	305.20784	65.21432	75.70652	13.99015	238.50528	60261.43130	2023-11-13 10:21:04	60264.50491	2023-11-16 12:07:04	145.436	-999.000	145.436	121.328	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	2	31100070	32000070	129.778	121.328	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-22 03:31:53	2025-08-31 00:00:00	2023-11-23 14:39:15	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000114000/	WINDOW2	WINDOW1	4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
362	000113000	Abell2319_BS	289.75898	44.10366	289.37202	44.01043	305.27307	65.1415	75.67099	13.92041	238.57418	60259.50074	2023-11-11 12:01:04	60261.43130	2023-11-13 10:21:04	94.756	-999.000	94.756	0.000	PX_NORMAL	N	Y	N	N	N	N	Y	BRIGHT	OFF	OFF	OFF	2	31200070		81.423	69.912	0.000	0.843	11110	313430	11310	PROCESSED	2024-09-21 18:24:34	2025-08-31 00:00:00	2023-11-15 09:30:48	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000113000/	WINDOW1BURST		4	Observation Log: No remarks ; Pre-pipeline Log: No remarks
363	000112000	PKS_0745-19	116.88131	-19.29489	116.32758	-19.17021	123.65625	-39.64511	236.44209	3.0297	111.79751	60256.43130	2023-11-08 10:21:04	60259.50074	2023-11-11 12:01:04	143.663	-999.000	143.663	0.000	PX_NORMAL	Y	Y	Y	Y	Y	Y	Y	BRIGHT	OFF	OFF	OFF	1	31100070		99.653	0.000	0.000	4.184	11110	313430	11310	PROCESSED	2024-09-21 20:14:15	2025-08-31 00:00:00	2023-11-14 20:00:31	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000112000/	WINDOW1		3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
364	000111000	Abell2319_BS	289.75909	44.10363	289.37213	44.01039	305.27323	65.14144	75.67099	13.92032	242.68478	60254.54935	2023-11-06 13:11:04	60256.43130	2023-11-08 10:21:04	101.349	-999.000	101.349	0.000	PX_NORMAL	N	Y	N	N	Y	Y	Y	BRIGHT	OFF	OFF	OFF		31100070	32000070	0.000	0.000	0.000	0.000	00100	313430	11310	PROCESSED	2024-09-20 14:00:50	2025-08-31 00:00:00	2023-11-11 17:18:01	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000111000/	WINDOW2	WINDOW1	5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
365	000110000	1E0102.2-7219	16.0064	-72.03299	15.60145	-72.30097	314.63242	-65.03623	301.55818	-45.06167	203.57912	60252.90352	2023-11-04 21:41:04	60254.54935	2023-11-06 13:11:04	80.809	-999.000	80.809	0.000	PX_NORMAL	N	N	N	N	Y	N	Y	BRIGHT	OFF	OFF	OFF		30000070		0.000	0.000	0.000	0.000	00100	313430	11310	PROCESSED	2024-09-21 05:43:57	2025-08-31 00:00:00	2023-11-11 16:02:09	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000008001		SUPERNOVA REMNANTS	0	A	Makoto Tashiro		CAL	0	CAL	PV Calibration Targets (1)	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000110000/	WINDOW1		6	Observation Log: No remarks ; Pre-pipeline Log: No remarks
366	000109000	Cygnus_X-1_OFFSET	299.59684	35.21533	299.12689	35.07883	313.69003	54.25691	71.34951	3.06944	251.97894	60252.58407	2023-11-04 14:01:04	60252.90352	2023-11-04 21:41:04	13.582	-999.000	13.582	0.000	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF		30000050		0.000	0.000	0.000	0.000	00100	313430	11310	PROCESSED	2024-09-21 04:39:55	2025-08-31 00:00:00	2023-11-11 16:03:45	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000109000/	WINDOW1		5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
367	000108000	Cygnus_X-1_BS	306.04125	33.91085	305.55182	33.74802	321.11694	51.15052	73.16659	-2.08362	255.57983	60251.99380	2023-11-03 23:51:04	60252.58407	2023-11-04 14:01:04	32.431	-999.000	32.431	0.000	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF		30000050		0.000	0.000	0.000	0.000	00100	313430	11310	PROCESSED	2024-09-25 16:40:41	2025-08-31 00:00:00	2023-11-11 16:00:09	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000108000/	WINDOW1		6	Observation Log: No remarks ; Pre-pipeline Log: No remarks
368	000107000	Cygnus_X-1_OFFSET	299.59693	35.21531	299.12698	35.07881	313.69013	54.25686	71.34953	3.06936	251.97945	60251.85491	2023-11-03 20:31:04	60251.99380	2023-11-03 23:51:04	6.611	-999.000	6.611	0.000	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF		30000050		0.000	0.000	0.000	0.000	00100	313430	11310	PROCESSED	2024-09-21 03:34:37	2025-08-31 00:00:00	2023-11-08 11:07:06	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		BH AND NS BINARIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000107000/	WINDOW1		5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
369	000106000	Abell2319_BS	289.75794	44.10361	289.37097	44.01038	305.27134	65.14169	75.67062	13.92107	246.09854	60251.64657	2023-11-03 15:31:04	60251.85491	2023-11-03 20:31:04	0.000	-999.000	0.000	0.000	PX_NORMAL	N	Y	N	N	Y	Y	Y	BRIGHT	OFF	OFF	OFF	2	31100070	32000070	3.881	0.000	0.000	0.493	11110	313430	11310	PROCESSED	2024-09-21 03:16:51	2025-08-31 00:00:00	2023-11-08 12:05:58	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000106000/	WINDOW2	WINDOW1	6	Observation Log: No remarks ; Pre-pipeline Log: No remarks
370	000105000	1E0102.2-7219	16.00641	-72.03317	15.60146	-72.30115	314.63203	-65.03631	301.5582	-45.06149	200.74897	60249.57713	2023-11-01 13:51:04	60251.64657	2023-11-03 15:31:04	0.000	-999.000	0.000	28.333	PX_NORMAL	N	Y	N	N	N	Y	Y	BRIGHT	OFF	OFF	OFF	1	31100070	32000070	65.720	28.333	0.000	3.408	11110	313430	11310	PROCESSED	2025-07-15 17:54:44	2025-08-31 00:00:00	2023-11-07 14:20:44	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000000888		SUPERNOVA REMNANTS	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000105000/	WINDOW2	WINDOW1	7	Observation Log: No remarks ; Pre-pipeline Log: No remarks
371	000104200	Abell2319_BS	289.75951	44.10405	289.37255	44.01081	305.27423	65.14174	75.67151	13.92022	248.68659	60246.00074	2023-10-29 00:01:04	60249.57713	2023-11-01 13:51:04	241.787	-999.000	241.787	201.371	PX_NORMAL	N	Y	N	N	Y	Y	Y	BRIGHT	OFF	BRIGHT	OFF	1	30000050		201.371	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-20 16:41:08	2025-08-31 00:00:00	2023-11-06 13:45:11	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000104200/	WINDOW1		5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
372	000104100	Abell2319_BS	289.76016	44.1044	289.3732	44.01116	305.27555	65.14193	75.67204	13.91994	248.68711	60243.00074	2023-10-26 00:01:04	60246.00074	2023-10-29 00:01:04	153.775	-999.000	153.775	129.665	PX_NORMAL	N	N	N	N	Y	N	Y	BRIGHT	OFF	OFF	OFF	1	30000050		129.665	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-25 19:49:14	2025-08-31 00:00:00	2023-11-07 03:15:20	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000104100/	WINDOW1		5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
373	000104000	Abell2319_BS	289.75978	44.10398	289.37281	44.01074	305.2746	65.14162	75.67153	13.92002	248.68665	60240.85491	2023-10-23 20:31:04	60243.00074	2023-10-26 00:01:04	101.905	-999.000	101.905	87.278	PX_NORMAL	N	N	N	N	Y	N	Y	OFF	OFF	OFF	OFF	1	30000050		87.278	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2024-09-21 15:34:54	2025-08-31 00:00:00	2023-11-05 12:22:27	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000104000/	WINDOW1		5	Observation Log: No remarks ; Pre-pipeline Log: No remarks
374	000103000	Abell2319	290.29786	43.94516	289.90863	43.84947	306.02017	64.86654	75.68899	13.50214	256.21257	60236.99380	2023-10-19 23:51:04	60240.85491	2023-10-23 20:31:04	97.672	-999.000	97.672	92.637	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF	1	30000050		92.637	0.000	0.000	0.000	11110	313430	11310	PROCESSED	2025-07-15 11:17:06	2025-08-31 00:00:00	2023-10-28 16:43:54	03.02.014.010	gen20241115_xtd20241115_rsl20241115	Hea_12Mar2025_V6.35_XRISM_28Feb2025_V002	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000103000/	WINDOW1		6	Observation Log: No remarks ; Pre-pipeline Log: No remarks
375	000102000	Abell2319_Cor1	290.29775	43.94522	289.90853	43.84953	306.02005	64.86662	75.68901	13.50223	256.21295	60234.06223	2023-10-17 01:29:37	60236.99380	2023-10-19 23:51:04	140.565	-999.000	140.565	0.000	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF		UNKNOWN	UNKNOWN	0.000	0.000	0.000	0.000	01100	313430	11310	PROCESSED	2024-09-21 06:06:56	2025-08-31 00:00:00	2023-10-27 10:56:26	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000102000/	OFF	OFF	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
376	000101000	Abell2319	290.30022	43.92363	289.9108	43.82793	306.00751	64.84562	75.66963	13.49155	256.21518	60230.99380	2023-10-13 23:51:04	60234.06223	2023-10-17 01:29:37	146.644	-999.000	146.644	0.000	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF		UNKNOWN	UNKNOWN	0.000	0.000	0.000	0.000	00100	313430	11310	PROCESSED	2024-09-20 11:50:42	2025-08-31 00:00:00	2023-10-21 17:25:10	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000101000/	OFF	OFF	3	Observation Log: No remarks ; Pre-pipeline Log: No remarks
377	000100000	Abell2319_BS	289.75543	44.08346	289.36829	43.99024	305.25196	65.12317	75.65095	13.91437	267.14349	60226.08407	2023-10-09 02:01:04	60230.99380	2023-10-13 23:51:04	234.129	-999.000	234.129	0.000	PX_NORMAL	N	Y	N	N	Y	Y	Y	OFF	OFF	OFF	OFF		UNKNOWN	UNKNOWN	0.000	0.000	0.000	0.000	00100	313430	11310	PROCESSED	2024-09-20 11:47:32	2025-08-31 00:00:00	2023-10-19 11:59:34	03.00.013.009	gen20240315_xtd20240815_rsl20240815	Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001	000000888		GROUPS AND CLUSTERS OF GALAXIES	0	A	Makoto Tashiro		JAP	0	NOR	IN-ORBIT COMMISSIONING	archived	https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/0/000100000/	OFF	OFF	7	Observation Log: No remarks ; Pre-pipeline Log: No remarks

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