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 241

Download WgetScript

No.	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	observation_id	exposure	awarded_exposure	xis0_exposure	xis1_exposure	xis2_exposure	xis3_exposure	xis0_observation_mode	xis1_observation_mode	xis2_observation_mode	xis3_observation_mode	hxd_observation_mode	hxd_coarse_clock_rate_exposure	hxd_first_clock_rate_exposure	hxd_normal_clock_rate_exposure	hxd_all_clock_rate_exposure	hxd_wam_exposure	quantity_of_hxd_burst	processing_status	processing_date_mjd	processing_date	public_date_mjd	public_date	distribution_date_mjd	distribution_date	processing_version	processing_count	processing_software	proposal_id	proposal_abstract	proposal_category	proposal_category_code	proposal_priority	pi_name	co_pi_name	proposal_affiliated_country	proposal_cycle	observation_type	proposal_title	main_instrument	has_xis_injection	data_access_url	ql_access_url	ql_image_url
1	4U0142+61	26.5176	61.8112	25.649771	61.561225	52.160955	46.451759	129.33625727	-0.37933599	61.041	55055.0703125	2009-08-12 01:41:15	55057.3654976852	2009-08-14 08:46:19	404079010	107.4129	100	107.4129	107.4209	0	107.4227	2	2	0	2	1	0	0	99.7576	99.7576	198.2838	2	PROCESSED	57548.2012152778	2016-06-09 04:49:45	54922	2009-04-01 00:00:00	55068.3037268518	2009-08-25 07:17:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	4	AO4	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404079010/	Quick Look
2	PSR J1846-0258	281.5972	-2.9106	280.942424	-2.965017	282.329422	20.034924	29.7662115	-0.20474108	86.0001	54936.8175578704	2009-04-15 19:37:17	54939.6779398148	2009-04-18 16:16:14	404081010	104.3451	100	104.3451	104.3675	0	104.3531	2	2	0	2	1	0	0	76.0065	76.0065	247.1018	1	PROCESSED	57546.2746990741	2016-06-07 06:35:34	54922	2009-04-01 00:00:00	54959.5006018518	2009-05-08 12:00:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	4	AO4	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404081010/	Quick Look
3	ZWCL0008.8+5215 WEST	2.7765	52.5416	2.120361	52.263518	29.435357	45.775484	116.7279282	-9.84363991	63.9984	56847.5889351852	2014-07-09 14:08:04	56849.9925115741	2014-07-11 23:49:13	809117010	102.3736	100	102.3816	102.3736	0	102.3896	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.3796643518	2016-08-15 09:06:43	56748	2014-04-01 00:00:00	56861.6478703704	2014-07-23 15:32:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096003	Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROKI AKAMATSU		EUR	9	AO9	EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809117010/	Quick Look
4	VIRGO W12	184.4921	10.4589	183.855234	10.736542	179.90666	11.371427	276.03236295	71.56080365	100	56277.5402546296	2012-12-16 12:57:58	56278.125150463	2012-12-17 03:00:13	807105010	27.0915	24	27.0995	27.0915	0	27.0995	1	1	0	1	1	0	0	26.8528	26.8528	50.488	1	PROCESSED	57608.2964930556	2016-08-08 07:06:57	56018	2012-04-01 00:00:00	56344.6765162037	2013-02-21 16:14:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807105010/	Quick Look
5	GALACTIC_BULGE10	268.297	-31.6627	267.484676	-31.652449	268.525852	-8.230314	358.49964198	-2.80216044	277.1297	55091.579525463	2009-09-17 13:54:31	55093.1508564815	2009-09-19 03:37:14	504093010	53.2416	50	53.2495	53.2416	0	53.2575	2	2	0	2	1	0	0	46.9072	46.9072	135.734	1	PROCESSED	57548.6254513889	2016-06-09 15:00:39	54922	2009-04-01 00:00:00	55110.3193865741	2009-10-06 07:39:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504093010/	Quick Look
6	GALACTIC_BULGE8	267.0897	-31.0498	266.281644	-31.033699	267.475091	-7.634163	358.49976827	-1.60277837	260.4349	55088.8177777778	2009-09-14 19:37:36	55090.3043287037	2009-09-16 07:18:14	504091010	51.3316	50	51.3316	51.3392	0	51.3316	2	2	0	2	1	0	0	47.7514	47.7514	128.4258	2	PROCESSED	57548.5976041667	2016-06-09 14:20:33	54922	2009-04-01 00:00:00	55109.4226736111	2009-10-05 10:08:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504091010/	Quick Look
7	ABELL2255_RELIC	258.3088	64.2709	258.23432	64.327456	199.782032	84.629727	94.17355304	34.84143708	3.193	56810.1311458333	2014-06-02 03:08:51	56812.4147569444	2014-06-04 09:57:15	809121010	100.6045	100	100.6045	100.8125	0	100.8045	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.1987731482	2016-08-15 04:46:14	56748	2014-04-01 00:00:00	56867.7458217593	2014-07-29 17:53:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096003	Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROKI AKAMATSU		EUR	9	AO9	EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809121010/	Quick Look
8	A2199 OFFSET6	247.2752	38.7861	246.840866	38.894582	233.723395	59.394916	61.88224995	43.57632899	299.9992	55792.1844212963	2011-08-19 04:25:34	55792.9321875	2011-08-19 22:22:21	806152010	29.7851	30	29.7851	29.7851	0	29.7851	2	2	0	2	1	0	0	22.2105	22.2105	64.5979	1	PROCESSED	57602.8830324074	2016-08-02 21:11:34	55652	2011-04-01 00:00:00	55806.2639467593	2011-09-02 06:20:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806152010/	Quick Look
9	SGR 1900+14	286.7986	9.3873	286.201777	9.308221	289.568815	31.69386	43.07377535	0.80526184	82.6704	54947.7664814815	2009-04-26 18:23:44	54949.0807175926	2009-04-28 01:56:14	404077010	53.1374	50	53.3934	53.3934	0	53.1374	2	2	0	2	1	0	0	42.1011	42.1011	113.5479	1	PROCESSED	57546.4694444444	2016-06-07 11:16:00	54922	2009-04-01 00:00:00	54973.4547222222	2009-05-22 10:54:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	4	AO4	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404077010/	Quick Look
10	A2199 OFFSET7	247.8714	39.0623	247.44001	39.168102	234.433925	59.797533	62.28955825	43.12499555	270.0014	55792.9380324074	2011-08-19 22:30:46	55793.5717708333	2011-08-20 13:43:21	806153010	28.9786	30	28.9946	28.9786	0	28.9946	1	1	0	1	1	0	0	23.6221	23.6221	54.7439	1	PROCESSED	57602.8895138889	2016-08-02 21:20:54	55652	2011-04-01 00:00:00	55806.2932175926	2011-09-02 07:02:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806153010/	Quick Look
11	RXCJ1053.7+5453	163.1919	54.9274	162.433556	55.193301	139.011043	43.216014	152.52898808	54.84022784	128.7233	56962.235150463	2014-11-01 05:38:37	56964.4029513889	2014-11-03 09:40:15	809120010	87.0847	100	87.0847	101.5529	0	101.5529	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7267708333	2016-08-16 17:26:33	56748	2014-04-01 00:00:00	57071.4205671296	2015-02-18 10:05:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096003	Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROKI AKAMATSU		EUR	9	AO9	EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809120010/	Quick Look
12	A2199 OFFSET11	246.6136	39.2216	246.181473	39.33303	232.494915	59.651332	62.4602069	44.10568707	268	55815.9308449074	2011-09-11 22:20:25	55816.4036342593	2011-09-12 09:41:14	806157010	20.6533	20	20.6613	20.6533	0	20.6613	2	2	0	2	1	0	0	20.551	20.551	40.8439	3	PROCESSED	57603.1066898148	2016-08-03 02:33:38	55652	2011-04-01 00:00:00	55865.9405555556	2011-10-31 22:34:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806157010/	Quick Look
13	GRXE_E_10	267.9015	-25.9408	267.12546	-25.928719	268.101648	-2.513628	3.25115356	0.4070413	105.0001	56362.3793865741	2013-03-11 09:06:19	56364.8778472222	2013-03-13 21:04:06	507075010	101.3428	100	101.3428	101.3428	0	101.3428	2	2	0	2	1	0	0	88.2422	88.2422	215.806	2	PROCESSED	57610.8450462963	2016-08-10 20:16:52	56018	2012-04-01 00:00:00	56377.5882175926	2013-03-26 14:07:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507075010/	Quick Look
14	MBM16	49.7694	11.5801	49.085806	11.399029	50.444533	-6.508969	170.60605682	-37.27197306	254.9211	56331.4284606482	2013-02-08 10:16:59	56333.553587963	2013-02-10 13:17:10	507076020	80.9506	80	80.9746	80.9506	0	80.9746	2	2	0	2	1	0	0	69.3076	69.3076	183.5839	2	PROCESSED	57610.5874074074	2016-08-10 14:05:52	56018	2012-04-01 00:00:00	56349.5813657407	2013-02-26 13:57:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076003	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	7	AO7	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507076020/	Quick Look
15	A2199 OFFSET2	247.0222	38.9947	246.589024	39.104311	233.2293	59.533721	62.15962406	43.78139177	300.0001	55790.2001851852	2011-08-17 04:48:16	55790.5974884259	2011-08-17 14:20:23	806148010	20.2856	20	20.2856	20.2856	0	20.2856	1	1	0	1	1	0	0	15.074	15.074	34.3199	1	PROCESSED	57602.8518287037	2016-08-02 20:26:38	55652	2011-04-01 00:00:00	55806.1895601852	2011-09-02 04:32:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806148010/	Quick Look
16	MBM36	238.3613	-4.7912	237.701072	-4.643799	237.20756	15.120262	4.0047136	35.6981582	275.8793	56894.6980324074	2014-08-25 16:45:10	56896.6598958333	2014-08-27 15:50:15	509074010	83.1887	80	83.1967	83.1887	0	83.1967	2	2	0	2	1	0	0	3.755	3.755	8.94	0	PROCESSED	57616.559525463	2016-08-16 13:25:43	56748	2014-04-01 00:00:00	56929.2087615741	2014-09-29 05:00:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096001	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	9	AO9	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509074010/	Quick Look
17	GB_NORTH_4	264.8998	-28.3109	264.109826	-28.284233	265.484852	-4.949634	359.83607677	1.45248781	106.6967	57110.9717708333	2015-03-29 23:19:21	57113.0203472222	2015-04-01 00:29:18	509080010	88.1941	100	88.1941	95.0455	0	95.0615	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8835648148	2016-08-17 21:12:20	56748	2014-04-01 00:00:00	57125.4051736111	2015-04-13 09:43:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096002	The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	9	AO9	MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY-	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509080010/	Quick Look
18	A2199 OFFSET16	247.7994	39.696	247.372677	39.802115	233.944751	60.385033	63.15474779	43.20527386	235.0008	55840.9241666667	2011-10-06 22:10:48	55841.4308217593	2011-10-07 10:20:23	806162010	28.3158	30	28.3158	28.3158	0	28.3158	1	1	0	1	1	0	0	28.6983	28.6983	43.7679	0	PROCESSED	57603.3467824074	2016-08-03 08:19:22	55652	2011-04-01 00:00:00	55858.377037037	2011-10-24 09:02:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806162010/	Quick Look
19	VIRGO E13	191.4157	14.448	190.788981	14.721164	184.610172	17.765771	296.58532586	77.24852866	284.9997	56486.2639351852	2013-07-13 06:20:04	56486.8515856482	2013-07-13 20:26:17	808128010	20.4817	20	20.4897	20.4817	0	20.4897	2	2	0	2	1	0	0	18.787	18.787	50.7599	0	PROCESSED	57611.9056134259	2016-08-11 21:44:05	56383	2013-04-01 00:00:00	56503.6194444444	2013-07-30 14:52:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808128010/	Quick Look
20	ABELL 426 W5.5	47.9127	41.6204	47.090331	41.432362	57.05648	22.874112	149.19418163	-13.99181892	94.0012	55429.9950115741	2010-08-21 23:52:49	55430.3626967593	2010-08-22 08:42:17	805115010	9.8216	10	9.8256	9.8356	0	9.8216	2	2	0	2	1	0	0	6.999	6.999	31.768	0	PROCESSED	57553.1611342593	2016-06-14 03:52:02	55287	2010-04-01 00:00:00	55446.1245023148	2010-09-07 02:59:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805115010/	Quick Look
21	SN1006_SE1	225.8641	-42.0384	225.045074	-41.843059	235.594631	-23.72201	327.62177329	14.41744154	286.0629	56883.8521064815	2014-08-14 20:27:02	56887.5210648148	2014-08-18 12:30:20	509082010	201.8322	480	201.8322	202.4881	0	202.5201	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5228240741	2016-08-16 12:32:52	56748	2014-04-01 00:00:00	56910.6390509259	2014-09-10 15:20:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096004	We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		USA	9	AO9	THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509082010/	Quick Look
22	SN1006_SE1	225.857	-42.039	225.037992	-41.843634	235.58934	-23.724178	327.61674963	14.4195613	107.6985	57063.4521643518	2015-02-10 10:51:07	57069.9807060185	2015-02-16 23:32:13	509082020	258.382	280	258.382	278.7901	0	278.8541	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6457523148	2016-08-17 15:29:53	56748	2014-04-01 00:00:00	57080.4416898148	2015-02-27 10:36:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096004	We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		USA	9	AO9	THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509082020/	Quick Look
23	VIRGO W5	186.3906	11.6158	185.756069	11.892616	181.170087	13.184054	280.29277845	73.33982916	99.9992	56273.927037037	2012-12-12 22:14:56	56274.3467476852	2012-12-13 08:19:19	807098010	16.6144	15	16.6261	16.6224	0	16.6144	2	2	0	2	1	0	0	18.174	18.174	36.256	0	PROCESSED	57608.2663078704	2016-08-08 06:23:29	56018	2012-04-01 00:00:00	56303.5207407407	2013-01-11 12:29:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807098010/	Quick Look
24	VIRGO S5	187.6482	10.8577	187.014441	11.133804	182.643107	12.991025	285.16119801	73.00623042	308.4993	56112.5062037037	2012-07-04 12:08:56	56112.7681828704	2012-07-04 18:26:11	807119010	12.7732	10	12.7812	12.7732	0	12.7892	1	1	0	1	1	0	0	12.087	12.087	22.6239	0	PROCESSED	57606.5630439815	2016-08-06 13:30:47	56018	2012-04-01 00:00:00	56141.1590625	2012-08-02 03:49:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807119010/	Quick Look
25	VIRGO E6	189.4489	13.3515	188.818836	13.626346	183.257959	15.984737	289.22685608	75.85896695	284.9998	56482.9353935185	2013-07-09 22:26:58	56483.2543171296	2013-07-10 06:06:13	808121010	14.633	14	14.641	14.641	0	14.633	1	1	0	1	1	0	0	11.0441	11.0441	27.5519	0	PROCESSED	57611.7799421296	2016-08-11 18:43:07	56383	2013-04-01 00:00:00	56496.5976157407	2013-07-23 14:20:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808121010/	Quick Look
26	VIRGO E10	190.6018	13.9952	189.973652	14.269099	184.050004	17.029845	293.36819262	76.69896749	284.9995	56484.6167476852	2013-07-11 14:48:07	56485.1960416667	2013-07-12 04:42:18	808125010	21.4435	20	21.4435	21.4435	0	21.4435	2	2	0	2	1	0	0	19.152	19.152	50.044	1	PROCESSED	57611.8325115741	2016-08-11 19:58:49	56383	2013-04-01 00:00:00	56498.6333796296	2013-07-25 15:12:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808125010/	Quick Look
27	GALACTIC_BULGE1	267.2201	-29.3677	266.422949	-29.352259	267.554885	-5.950193	359.99969448	-0.83243485	274.7	55118.4798148148	2009-10-14 11:30:56	55119.6453587963	2009-10-15 15:29:19	504088010	47.23	50	47.23	47.23	0	47.23	2	2	0	2	1	0	0	32.6139	32.6139	100.7	2	PROCESSED	57548.8825231482	2016-06-09 21:10:50	54922	2009-04-01 00:00:00	55134.0688425926	2009-10-30 01:39:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504088010/	Quick Look
28	GALACTIC_BULGE9	267.6768	-31.2805	266.867115	-31.267244	267.986252	-7.855618	358.55970985	-2.15232996	265.3076	55090.3066550926	2009-09-16 07:21:35	55091.5758564815	2009-09-17 13:49:14	504092010	50.9199	50	50.9439	50.9359	0	50.9199	2	2	0	2	1	0	0	45.5744	45.5744	109.6459	1	PROCESSED	57548.6135069444	2016-06-09 14:43:27	54922	2009-04-01 00:00:00	55109.4315740741	2009-10-05 10:21:28	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504092010/	Quick Look
29	ABELL 426 W7	47.3511	41.6379	46.530265	41.447862	56.625896	23.013072	148.81593544	-14.19658633	93.9992	55431.0429398148	2010-08-23 01:01:50	55431.5078356482	2010-08-23 12:11:17	805109010	15.4161	15	15.4481	15.4321	0	15.4161	1	1	0	1	1	0	0	13.2824	13.2824	40.1599	0	PROCESSED	57553.1742824074	2016-06-14 04:10:58	55287	2010-04-01 00:00:00	55449.2612731482	2010-09-10 06:16:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805109010/	Quick Look
30	A2199 OFFSET1	247.4695	38.9998	247.037043	39.107408	233.880438	59.644289	62.18539249	43.43422484	299.9971	55789.6293171296	2011-08-16 15:06:13	55790.1995717593	2011-08-17 04:47:23	806147010	20.2965	20	20.2965	20.2965	0	20.2965	2	2	0	2	1	0	0	19.2982	19.2982	49.2599	0	PROCESSED	57602.803287037	2016-08-02 19:16:44	55652	2011-04-01 00:00:00	55806.270150463	2011-09-02 06:29:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806147010/	Quick Look
31	A2199 OFFSET15	246.482	39.889	246.05467	40.001004	231.881042	60.252338	63.3872074	44.22195617	255.0003	55823.9923726852	2011-09-19 23:49:01	55824.6403935185	2011-09-20 15:22:10	806161010	28.1669	30	28.1829	28.1669	0	28.1829	3	2	0	2	1	0	0	28.0746	28.0746	55.9819	0	PROCESSED	57603.196412037	2016-08-03 04:42:50	55652	2011-04-01 00:00:00	55851.4457060185	2011-10-17 10:41:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806161010/	Quick Look
32	KEPLER_BG_GE	263.5357	-20.2632	262.792974	-20.230061	263.919291	3.041451	5.99779838	6.79710869	273.0028	55072.0030208333	2009-08-29 00:04:21	55072.5002662037	2009-08-29 12:00:23	504101020	24.7227	60	24.7467	24.7387	0	24.7227	2	2	0	2	1	0	0	19.2528	19.2528	42.9559	0	PROCESSED	57548.3891550926	2016-06-09 09:20:23	54922	2009-04-01 00:00:00	55109.4155324074	2009-10-05 09:58:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	4	AO4	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504101020/	Quick Look
33	KEPLER_BG_GW	261.806	-22.7684	261.049806	-22.726898	262.438757	0.457902	2.99933771	6.7960859	273.0885	55109.2984143518	2009-10-05 07:09:43	55111.1057175926	2009-10-07 02:32:14	504102010	65.2949	60	65.3029	65.2949	0	65.3029	2	2	0	2	1	0	0	50.7821	50.7821	156.128	1	PROCESSED	57548.8038425926	2016-06-09 19:17:32	54922	2009-04-01 00:00:00	55125.6963888889	2009-10-21 16:42:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	4	AO4	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504102010/	Quick Look
34	KEPLER_BG_GS	263.1005	-22.949	262.342899	-22.913725	263.639389	0.339875	3.49961978	5.69692486	272.6396	55107.43	2009-10-03 10:19:12	55109.2973842593	2009-10-05 07:08:14	504104010	67.2508	60	67.2508	67.2805	0	67.2748	2	2	0	2	1	0	0	53.1585	53.1585	161.3298	1	PROCESSED	57548.7538425926	2016-06-09 18:05:32	54922	2009-04-01 00:00:00	55125.3521180556	2009-10-21 08:27:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	4	AO4	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504104010/	Quick Look
35	GALACTIC_BULGE3	267.9488	-29.7963	267.148788	-29.784389	268.199437	-6.368042	359.95634845	-1.5962466	107.1729	55624.8013310185	2011-03-04 19:13:55	55626.2292939815	2011-03-06 05:30:11	505078010	51.2756	50	51.2756	51.2756	0	51.2756	2	2	0	2	1	0	0	39.3124	39.3124	123.3618	0	PROCESSED	57601.0957407407	2016-08-01 02:17:52	55287	2010-04-01 00:00:00	55642.1205787037	2011-03-22 02:53:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505078010/	Quick Look
36	GALACTIC_BULGE15	265.6963	-32.7784	264.876935	-32.755516	266.323781	-9.39206	356.40742505	-1.49294303	89.8786	55626.2338425926	2011-03-06 05:36:44	55627.5424884259	2011-03-07 13:01:11	505084010	50.3097	50	50.3172	50.3097	0	50.3252	1	1	0	1	1	0	0	37.5095	37.5095	113.0559	0	PROCESSED	57601.1030439815	2016-08-01 02:28:23	55287	2010-04-01 00:00:00	55645.2697222222	2011-03-25 06:28:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505084010/	Quick Look
37	GALACTIC_BULGE16	266.5113	-33.2224	265.68867	-33.203457	267.02907	-9.817155	356.38592507	-2.30771737	275.4625	55482.2533217593	2010-10-13 06:04:47	55483.5626967593	2010-10-14 13:30:17	505085010	55.0315	50	55.0315	55.0315	0	55.0315	2	2	0	2	1	0	0	48.6341	48.6341	113.1139	1	PROCESSED	57553.750787037	2016-06-14 18:01:08	55287	2010-04-01 00:00:00	55502.290150463	2010-11-02 06:57:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505085010/	Quick Look
38	GALACTIC_BULGE17	267.7467	-33.8391	266.919516	-33.82614	268.087567	-10.412886	356.3863118	-3.50805248	275.261	55483.5637731482	2010-10-14 13:31:50	55485.0627893518	2010-10-16 01:30:25	505086010	53.1266	50	53.1266	54.0895	0	54.0895	2	2	0	2	1	0	0	46.2769	46.2769	129.4938	1	PROCESSED	57553.7652430556	2016-06-14 18:21:57	55287	2010-04-01 00:00:00	55508.2025694444	2010-11-08 04:51:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505086010/	Quick Look
39	HESS J1841-55 3	280.1471	-5.609	279.479279	-5.656459	280.581257	17.459575	26.70525302	-0.15199861	87.0298	55647.6397685185	2011-03-27 15:21:16	55648.791875	2011-03-28 19:00:18	505090010	49.549	50	49.581	49.549	0	49.581	2	2	0	2	1	0	0	42.7935	42.7935	99.5239	1	PROCESSED	57601.3633101852	2016-08-01 08:43:10	55287	2010-04-01 00:00:00	55666.2655439815	2011-04-15 06:22:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505090010/	Quick Look
40	KES 27	237.1872	-53.7777	236.229597	-53.624833	247.581589	-32.858337	327.32071311	0.47884394	101.6269	55983.5400231482	2012-02-26 12:57:38	55985.4633217593	2012-02-28 11:07:11	506063010	109.3535	120	109.4015	109.3535	0	109.4015	3	2	0	2	1	0	0	115.3321	115.3321	166.148	4	PROCESSED	57604.7717592593	2016-08-04 18:31:20	55652	2011-04-01 00:00:00	55995.1904976852	2012-03-09 04:34:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506063010/	Quick Look
41	G349.7+0.2	259.4954	-37.4452	258.645482	-37.392398	261.399155	-14.316641	349.72102569	0.17051597	282.4112	55833.4324537037	2011-09-29 10:22:44	55838.1341898148	2011-10-04 03:13:14	506064010	160.4024	160	160.4264	160.4024	0	160.4344	2	2	0	2	1	0	0	144.6151	144.6151	404.22	5	PROCESSED	57603.3931134259	2016-08-03 09:26:05	55652	2011-04-01 00:00:00	55858.5356018518	2011-10-24 12:51:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506064010/	Quick Look
42	GRXE_E_2	267.6193	-27.2463	266.835371	-27.232829	267.869305	-3.822869	2.00029183	-0.04392641	105.0002	56366.4085532407	2013-03-15 09:48:19	56368.7772569444	2013-03-17 18:39:15	507069010	103.6873	100	103.6873	103.6873	0	103.6873	2	2	0	2	1	0	0	95.5834	95.5834	204.6259	2	PROCESSED	57610.8702314815	2016-08-10 20:53:08	56018	2012-04-01 00:00:00	56379.6047106482	2013-03-28 14:30:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507069010/	Quick Look
43	GRXE_E_3	267.7634	-27.0307	266.980773	-27.017932	267.994323	-3.605243	2.25114568	-0.04369036	105.0001	56368.7777314815	2013-03-17 18:39:56	56371.1111458333	2013-03-20 02:40:03	507070010	101.1726	100	101.1806	101.1726	0	101.1806	2	2	0	2	1	0	0	103.6028	103.6028	201.5898	0	PROCESSED	57610.8916782407	2016-08-10 21:24:01	56018	2012-04-01 00:00:00	56380.5799768518	2013-03-29 13:55:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507070010/	Quick Look
44	MBM36	238.3612	-4.7913	237.700971	-4.643898	237.207481	15.120143	4.00454082	35.69817373	279.4993	56155.0155787037	2012-08-16 00:22:26	56156.7563425926	2012-08-17 18:09:08	507077010	81.0158	80	81.0158	81.0176	0	81.0176	2	2	0	2	1	0	0	80.3301	80.3301	150.3877	4	PROCESSED	57606.8991782407	2016-08-06 21:34:49	56018	2012-04-01 00:00:00	56170.1653240741	2012-08-31 03:58:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076003	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	7	AO7	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507077010/	Quick Look
45	MBM20	68.9377	-14.6308	68.365051	-14.732172	64.468357	-36.225149	211.4041789	-36.56532035	78.376	56164.0544328704	2012-08-25 01:18:23	56166.3530092593	2012-08-27 08:28:20	507079010	82.8814	80	82.8814	82.8814	0	82.8814	2	2	0	2	1	0	0	73.8668	73.8668	198.5577	2	PROCESSED	57606.9726851852	2016-08-06 23:20:40	56018	2012-04-01 00:00:00	56212.7316087963	2012-10-12 17:33:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076003	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	7	AO7	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507079010/	Quick Look
46	GRXE_E_1	267.4747	-27.4596	266.689479	-27.445424	267.744238	-4.038324	1.75131157	-0.04310182	105.3995	56726.0649537037	2014-03-10 01:33:32	56728.6459722222	2014-03-12 15:30:12	508075010	103.5331	100	103.5491	103.5331	0	103.5559	3	2	0	2	1	0	0	85.3446	85.3446	222.9818	2	PROCESSED	57614.0622453704	2016-08-14 01:29:38	56383	2013-04-01 00:00:00	56740.8547453704	2014-03-24 20:30:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086001	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	8	AO8	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508075010/	Quick Look
47	LDN1563	75.5195	13.8744	74.812622	13.803125	75.779261	-8.85474	187.14092451	-16.70693442	81.1182	56523.4274768518	2013-08-19 10:15:34	56525.2535648148	2013-08-21 06:05:08	508080010	83.588	80	83.588	83.596	0	83.604	2	2	0	2	1	0	0	79.6741	79.6741	157.7538	2	PROCESSED	57612.368912037	2016-08-12 08:51:14	56383	2013-04-01 00:00:00	56587.8175694445	2013-10-22 19:37:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086002	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	8	AO8	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508080010/	Quick Look
48	MBM16	49.7701	11.5795	49.086508	11.398432	50.445044	-6.509726	170.60720168	-37.27195697	254.3636	57057.0973726852	2015-02-04 02:20:13	57059.5349421296	2015-02-06 12:50:19	509073020	92.0425	80	92.0425	92.0665	0	92.0665	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6060763889	2016-08-17 14:32:45	56748	2014-04-01 00:00:00	57107.434224537	2015-03-26 10:25:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096001	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	9	AO9	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509073020/	Quick Look
49	NGC3783	174.7201	-37.7846	174.100385	-37.507469	192.672057	-36.228861	287.44066962	22.89477473	305.9228	55022.9100115741	2009-07-10 21:50:25	55027.0016087963	2009-07-15 00:02:19	704063010	209.5034	200	209.5034	210.3114	0	210.3194	3	2	0	2	1	0	0	174.0404	174.0404	353.4535	2	PROCESSED	57547.9411342593	2016-06-08 22:35:14	54922	2009-04-01 00:00:00	55040.5612615741	2009-07-28 13:28:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046003	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	4	AO4	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704063010/	Quick Look
50	FAIRALL 9	20.848	-58.7784	20.369866	-59.039074	340.553777	-59.094561	295.14856402	-57.86436534	32.7271	55335.1255671296	2010-05-19 03:00:49	55338.764837963	2010-05-22 18:21:22	705063010	229.2963	250	229.302	229.302	0	229.2963	2	2	0	2	1	0	0	174.9412	174.9412	288.656	1	PROCESSED	57551.9874074074	2016-06-12 23:41:52	55287	2010-04-01 00:00:00	55434.4437615741	2010-08-26 10:39:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056003	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	5	AO5	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705063010/	Quick Look
51	3C120	68.2984	5.3496	67.633882	5.245152	67.432526	-16.407924	190.37864439	-27.39774516	260.9996	55966.4234143518	2012-02-09 10:09:43	55970.8752083333	2012-02-13 21:00:18	706042010	183.0015	300	183.0255	183.0015	0	183.0255	3	2	0	2	1	0	0	158.0306	158.0306	384.5957	3	PROCESSED	57604.7163310185	2016-08-04 17:11:31	55652	2011-04-01 00:00:00	55992.4178819444	2012-03-06 10:01:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066003	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	6	AO6-KP	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706042010/	Quick Look
52	3C120	68.2996	5.3511	67.635075	5.246657	67.433996	-16.406625	190.37800916	-27.39591229	261.0003	55971.7483564815	2012-02-14 17:57:38	55974.8819907407	2012-02-17 21:10:04	706042020	118.0689	120	118.0689	118.0689	0	118.0689	2	2	0	2	1	0	0	103.5365	103.5365	270.7359	2	PROCESSED	57604.7019791667	2016-08-04 16:50:51	55652	2011-04-01 00:00:00	55992.3150694444	2012-03-06 07:33:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066003	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	6	AO6-KP	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706042020/	Quick Look
53	GALACTIC_BULGE11	269.3164	-32.1646	268.50059	-32.159293	269.404915	-8.724949	358.50010375	-3.80248777	271.7893	55093.1531365741	2009-09-19 03:40:31	55095.6064699074	2009-09-21 14:33:19	504094010	93.1403	50	93.1403	93.1403	0	93.1403	2	2	0	2	1	0	0	82.9543	82.9543	211.9538	1	PROCESSED	57548.674224537	2016-06-09 16:10:53	54922	2009-04-01 00:00:00	55110.4114236111	2009-10-06 09:52:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504094010/	Quick Look
54	ABELL 426 S4	49.6689	40.4337	48.849146	40.252043	58.065773	21.361001	151.00436531	-14.27811504	87.9984	55425.804849537	2010-08-17 19:18:59	55426.0731018518	2010-08-18 01:45:16	805099010	12.3072	10	12.3072	12.3072	0	12.3072	2	2	0	2	1	0	0	9.95	9.95	23.1699	0	PROCESSED	57553.1090277778	2016-06-14 02:37:00	55287	2010-04-01 00:00:00	55439.1353009259	2010-08-31 03:14:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805099010/	Quick Look
55	ABELL 426 W4	48.4696	41.6016	47.645739	41.415563	57.483228	22.736303	149.56812051	-13.78700029	86.9981	55429.3049884259	2010-08-21 07:19:11	55429.5696527778	2010-08-21 13:40:18	805106010	10.3652	10	10.3652	10.3732	0	10.3732	1	1	0	1	1	0	0	9.68	9.68	22.8559	0	PROCESSED	57553.1536111111	2016-06-14 03:41:12	55287	2010-04-01 00:00:00	55445.2490509259	2010-09-06 05:58:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805106010/	Quick Look
56	ABELL 426 SW2	49.3858	41.1787	48.562066	40.995997	58.067168	22.136253	150.39892317	-13.77223683	94.9997	55800.6450115741	2011-08-27 15:28:49	55800.8411111111	2011-08-27 20:11:12	806100010	9.0043	10	9.0043	9.0123	0	9.0203	2	2	0	2	1	0	0	8.933	8.933	16.934	0	PROCESSED	57602.9794791667	2016-08-02 23:30:27	55652	2011-04-01 00:00:00	55818.1552083333	2011-09-14 03:43:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806100010/	Quick Look
57	ABELL 426 SW4	48.8197	40.8139	47.99987	40.629138	57.514249	21.906179	150.23286022	-14.31045471	88.4993	55801.606724537	2011-08-28 14:33:41	55801.8501388889	2011-08-28 20:24:12	806104010	13.203	10	13.203	13.203	0	13.203	1	1	0	1	1	0	0	13.335	13.335	21.0079	0	PROCESSED	57602.9897685185	2016-08-02 23:45:16	55652	2011-04-01 00:00:00	55826.0785763889	2011-09-22 01:53:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806104010/	Quick Look
58	ABELL 426 SW5.5	48.3936	40.5388	47.576679	40.352499	57.096428	21.733914	150.10390207	-14.71606913	88.4991	55802.4900694445	2011-08-29 11:45:42	55802.8161458333	2011-08-29 19:35:15	806107010	15.1951	15	15.1951	15.1991	0	15.2121	2	2	0	2	1	0	0	14.8247	14.8247	28.17	0	PROCESSED	57603.0002083333	2016-08-03 00:00:18	55652	2011-04-01 00:00:00	55826.144224537	2011-09-22 03:27:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806107010/	Quick Look
59	ABELL 426 SW7	47.984	40.268	47.169889	40.080231	56.691635	21.563368	149.97996332	-15.11138755	88.498	55803.3012037037	2011-08-30 07:13:44	55803.5903935185	2011-08-30 14:10:10	806110010	10.409	10	10.409	10.409	0	10.409	2	2	0	2	1	0	0	9.72	9.72	24.9599	0	PROCESSED	57603.007662037	2016-08-03 00:11:02	55652	2011-04-01 00:00:00	55826.1493287037	2011-09-22 03:35:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806110010/	Quick Look
60	ABELL 426 SE3	50.6611	40.9157	49.835576	40.737712	58.985501	21.618486	151.37300481	-13.45928131	89.561	55798.1679398148	2011-08-25 04:01:50	55798.4321990741	2011-08-25 10:22:22	806114010	11.7919	10	11.7999	11.7919	0	11.7999	1	1	0	1	1	0	0	9.2468	9.2468	22.8239	1	PROCESSED	57602.9457407407	2016-08-02 22:41:52	55652	2011-04-01 00:00:00	55855.1445949074	2011-10-21 03:28:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806114010/	Quick Look
61	ABELL 426 SE3.5	50.7904	40.8069	49.965238	40.629396	59.055043	21.487263	151.51904657	-13.49435734	89.5614	55798.4325347222	2011-08-25 10:22:51	55798.7085763889	2011-08-25 17:00:21	806115010	11.9045	10	11.9125	11.9045	0	11.9205	2	2	0	2	1	0	0	11.3326	11.3326	23.8479	0	PROCESSED	57602.9521643518	2016-08-02 22:51:07	55652	2011-04-01 00:00:00	55855.1551157407	2011-10-21 03:43:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806115010/	Quick Look
62	ABELL 426 NNE1	50.001	41.7793	49.17162	41.598852	58.726624	22.584898	150.45648036	-13.01724466	60.4921	55803.8286805556	2011-08-30 19:53:18	55804.0543171296	2011-08-31 01:18:13	806135010	11.392	10	11.392	11.392	0	11.392	1	1	0	1	1	0	0	9.824	9.824	19.4879	0	PROCESSED	57603.0136574074	2016-08-03 00:19:40	55652	2011-04-01 00:00:00	55830.2051273148	2011-09-26 04:55:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806135010/	Quick Look
63	ABELL 426 NNE4	50.2584	42.5938	49.422813	42.414295	59.170643	23.314758	150.15840734	-12.23290919	60.4999	55805.0005902778	2011-09-01 00:00:51	55805.2398263889	2011-09-01 05:45:21	806140010	11.8082	10	11.8082	11.8082	0	11.8082	1	1	0	1	1	0	0	7.2361	7.2361	20.656	1	PROCESSED	57603.0290509259	2016-08-03 00:41:50	55652	2011-04-01 00:00:00	55871.8764583333	2011-11-06 21:02:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806140010/	Quick Look
64	ABELL 426 NNE4.5	50.2947	42.7325	49.458059	42.553128	59.240445	23.440644	150.10266361	-12.10259839	60.4962	55806.265	2011-09-02 06:21:36	55806.5613078704	2011-09-02 13:28:17	806141010	11.085	10	11.085	11.085	0	11.085	2	2	0	2	1	0	0	11.0954	11.0954	25.5959	1	PROCESSED	57603.0357060185	2016-08-03 00:51:25	55652	2011-04-01 00:00:00	55845.2700578704	2011-10-11 06:28:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806141010/	Quick Look
65	ABELL 426 NNE5	50.3399	42.8692	49.502189	42.689995	59.316492	23.562815	150.05355099	-11.97038799	60.497	55806.5616898148	2011-09-02 13:28:50	55806.8931944444	2011-09-02 21:26:12	806142010	16.3359	15	16.3471	16.3359	0	16.3359	2	2	0	2	1	0	0	17.0342	17.0342	28.638	0	PROCESSED	57603.0391898148	2016-08-03 00:56:26	55652	2011-04-01 00:00:00	55845.258900463	2011-10-11 06:12:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806142010/	Quick Look
66	VIRGO W2	187.236	12.0886	186.602607	12.36495	181.750104	13.952177	282.50975725	74.06175724	285.4993	56110.9396180556	2012-07-02 22:33:03	56111.2640509259	2012-07-03 06:20:14	807095010	12.4847	10	12.4927	12.4847	0	12.5007	2	2	0	2	1	0	0	12.3335	12.3335	28.0259	1	PROCESSED	57606.5414583333	2016-08-06 12:59:42	56018	2012-04-01 00:00:00	56139.0870717593	2012-07-31 02:05:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807095010/	Quick Look
67	VIRGO W10	185.0059	10.7782	184.369631	11.055649	180.246148	11.867747	277.10217205	72.05623626	99.9987	56276.4098263889	2012-12-15 09:50:09	56276.9828935185	2012-12-15 23:35:22	807103010	27.9677	24	27.9677	27.9677	0	27.9677	2	2	0	2	1	0	0	25.7604	25.7604	49.5039	0	PROCESSED	57608.287974537	2016-08-08 06:54:41	56018	2012-04-01 00:00:00	56315.5187037037	2013-01-23 12:26:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807103010/	Quick Look
68	VIRGO N3	187.7014	13.8904	187.06968	14.166465	181.417647	15.781989	281.91864672	75.91344863	313.997	56098.2612037037	2012-06-20 06:16:08	56098.5176388889	2012-06-20 12:25:24	807108010	12.266	10	12.266	12.266	0	12.266	2	2	0	2	1	0	0	12.6997	12.6997	22.1399	1	PROCESSED	57605.7217013889	2016-08-05 17:19:15	56018	2012-04-01 00:00:00	56214.9569907407	2012-10-14 22:58:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807108010/	Quick Look
69	VIRGO S11	187.5325	8.9432	186.897427	9.219378	183.326019	11.193327	286.45864166	71.13028831	122.0016	56269.7576851852	2012-12-08 18:11:04	56270.1612384259	2012-12-09 03:52:11	807125010	17.2823	16	17.2823	17.2823	0	17.2823	2	2	0	2	1	0	0	18.5627	18.5627	34.82	0	PROCESSED	57608.2142013889	2016-08-08 05:08:27	56018	2012-04-01 00:00:00	56336.4686111111	2013-02-13 11:14:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807125010/	Quick Look
70	VIRGO S16	187.3813	7.0531	186.744958	7.329373	183.956748	9.401927	287.41240339	69.26194594	122.0008	56271.6277314815	2012-12-10 15:03:56	56272.0709722222	2012-12-11 01:42:12	807130010	21.6482	18	21.6482	21.6482	0	21.6482	2	2	0	2	1	0	0	21.3081	21.3081	38.2679	1	PROCESSED	57608.2349652778	2016-08-08 05:38:21	56018	2012-04-01 00:00:00	56330.5084837963	2013-02-07 12:12:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807130010/	Quick Look
71	VIRGO E12	191.1366	14.3009	190.509391	14.574322	184.414539	17.520905	295.44935056	77.07241976	285.0012	56485.8160185185	2013-07-12 19:35:04	56486.2634143518	2013-07-13 06:19:19	808127010	20.5979	20	20.6139	20.5979	0	20.6139	1	1	0	1	1	0	0	17.42	17.42	38.6479	0	PROCESSED	57611.9024768518	2016-08-11 21:39:34	56383	2013-04-01 00:00:00	56498.6479976852	2013-07-25 15:33:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808127010/	Quick Look
72	MBM16	49.752	11.6015	49.068335	11.420365	50.433531	-6.483887	170.57212752	-37.26756171	73.5786	56139.0841666667	2012-07-31 02:01:12	56140.9710416667	2012-08-01 23:18:18	507076010	24.9499	80	24.9499	24.9499	0	24.9499	2	2	0	2	1	0	0	18.2376	18.2376	162.962	1	PROCESSED	57606.7578703704	2016-08-06 18:11:20	56018	2012-04-01 00:00:00	56260.533125	2012-11-29 12:47:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076003	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	7	AO7	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507076010/	Quick Look
73	1E 2259+586	345.2716	58.9493	344.749816	58.680435	23.84389	56.952455	109.11022544	-0.92895504	86.3239	54976.8335300926	2009-05-25 20:00:17	54978.6446064815	2009-05-27 15:28:14	404076010	122.5791	120	122.5809	122.5809	0	122.5791	2	2	0	2	1	0	0	103.4462	103.4462	156.4638	1	PROCESSED	57546.7298726852	2016-06-07 17:31:01	54922	2009-04-01 00:00:00	54992.6935069444	2009-06-10 16:38:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	4	AO4	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404076010/	Quick Look
74	1RXS J1708-4009	257.2038	-40.2142	256.334135	-40.15046	259.790997	-17.224743	346.43162325	-0.00870489	267.1357	55466.6124074074	2010-09-27 14:41:52	55467.7738425926	2010-09-28 18:34:20	405076010	62.8109	60	62.8189	62.8226	0	62.8109	3	2	0	2	1	0	0	59.5114	59.5114	100.3239	1	PROCESSED	57553.5661342593	2016-06-14 13:35:14	55287	2010-04-01 00:00:00	55477.2762268518	2010-10-08 06:37:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	5	AO5	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405076010/	Quick Look
75	GALACTIC_BULGE2	267.5552	-29.599	266.756514	-29.585181	267.852413	-6.176134	359.95115697	-1.20153587	277.9812	55113.1708217593	2009-10-09 04:05:59	55114.5903472222	2009-10-10 14:10:06	504089010	55.2601	50	55.2671	55.2601	0	55.2736	2	2	0	2	1	0	0	40.226	40.226	122.6338	1	PROCESSED	57548.8316666667	2016-06-09 19:57:36	54922	2009-04-01 00:00:00	55131.3309953704	2009-10-27 07:56:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504089010/	Quick Look
76	KEPLER_BG_GE	263.5353	-20.2634	262.792573	-20.230259	263.918925	3.041235	5.99742641	6.79731937	272.7609	55087.1593171296	2009-09-13 03:49:25	55088.3606365741	2009-09-14 08:39:19	504101010	46.9895	60	46.9895	46.9895	0	46.9895	2	2	0	2	1	0	0	40.8993	40.8993	103.786	0	PROCESSED	57548.5758564815	2016-06-09 13:49:14	54922	2009-04-01 00:00:00	55099.2516782407	2009-09-25 06:02:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	4	AO4	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504101010/	Quick Look
77	THE KEPLER SNR	262.6737	-21.5073	261.92432	-21.469989	263.173689	1.760317	4.50532186	6.80830692	272.2663	55475.6914583333	2010-10-06 16:35:42	55478.2863194445	2010-10-09 06:52:18	505092020	111.1941	620	111.1941	111.2021	0	111.2021	2	2	0	2	1	0	0	99.8413	99.8413	224.1437	2	PROCESSED	57553.7268402778	2016-06-14 17:26:39	55287	2010-04-01 00:00:00	55488.3311689815	2010-10-19 07:56:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092020/	Quick Look
78	THE KEPLER SNR	262.671	-21.4826	261.921758	-21.445276	263.169925	1.784856	4.5248811	6.82377384	98.1034	55628.0376736111	2011-03-08 00:54:15	55632.2696643518	2011-03-12 06:28:19	505092050	84.5913	100	84.5913	85.6632	0	85.7192	4	3	0	3	1	0	0	122.4881	122.4881	365.616	3	PROCESSED	57601.284537037	2016-08-01 06:49:44	55287	2010-04-01 00:00:00	55648.4964699074	2011-03-28 11:54:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092050/	Quick Look
79	G272.2-3.2	136.7067	-52.1223	136.311595	-51.920282	170.81242	-63.078479	272.22054405	-3.18534238	101.7643	55877.9477777778	2011-11-12 22:44:48	55878.6272916667	2011-11-13 15:03:18	506060020	25.5265	20	25.5345	25.5345	0	25.5265	2	2	0	2	1	0	0	27.028	27.028	58.706	0	PROCESSED	57603.7829282407	2016-08-03 18:47:25	55652	2011-04-01 00:00:00	55895.0737962963	2011-11-30 01:46:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506060020/	Quick Look
80	G290.1-0.8	165.7447	-60.8884	165.228717	-60.618807	206.73964	-58.122992	290.11957377	-0.7436408	293.2659	55737.4551388889	2011-06-25 10:55:24	55740.5883333333	2011-06-28 14:07:12	506061010	110.5931	110	110.6091	110.5931	0	110.6011	2	2	0	2	1	0	0	99.3596	99.3596	270.6596	4	PROCESSED	57602.4993634259	2016-08-02 11:59:05	55652	2011-04-01 00:00:00	55775.3693287037	2011-08-02 08:51:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506061010/	Quick Look
81	GRXE_E_4	267.9068	-26.8159	267.125467	-26.803832	268.119163	-3.388548	2.50111874	-0.04382328	104.4995	56371.1118518518	2013-03-20 02:41:04	56373.3049421296	2013-03-22 07:19:07	507071010	101.2086	100	101.2166	101.2086	0	101.2166	2	2	0	2	1	0	0	105.6491	105.6491	189.4519	1	PROCESSED	57610.9065625	2016-08-10 21:45:27	56018	2012-04-01 00:00:00	56384.6094560185	2013-04-02 14:37:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507071010/	Quick Look
82	G355.6-0.0	263.7798	-32.6083	262.962219	-32.576152	264.68406	-9.281685	355.69106204	-0.03789327	90.0013	55246.5249074074	2010-02-19 12:35:52	55247.6293287037	2010-02-20 15:06:14	504098010	52.5044	50	52.5275	52.5204	0	52.5044	2	2	0	2	1	0	0	43.7346	43.7346	95.4118	0	PROCESSED	57550.6569560185	2016-06-11 15:46:01	54922	2009-04-01 00:00:00	55257.1119444444	2010-03-02 02:41:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504098010/	Quick Look
83	MBM36	238.3604	-4.7951	237.700156	-4.647695	237.207526	15.116261	4.00027103	35.69642682	294.5973	56525.2685300926	2013-08-21 06:26:41	56526.5655092593	2013-08-22 13:34:20	508079010	49.6555	80	49.6555	49.6555	0	49.6555	2	2	0	2	1	0	0	42.8799	42.8799	112.0458	2	PROCESSED	57612.3808912037	2016-08-12 09:08:29	56383	2013-04-01 00:00:00	56587.6359027778	2013-10-22 15:15:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086002	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	8	AO8	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508079010/	Quick Look
84	MBM20	68.9307	-14.6229	68.358009	-14.724304	64.461829	-36.216174	211.39181931	-36.56844204	64.9904	56520.8174074074	2013-08-16 19:37:04	56522.5001967593	2013-08-18 12:00:17	508081010	56.4905	80	56.4905	56.4905	0	56.4905	2	2	0	2	1	0	0	55.086	55.086	145.38	1	PROCESSED	57612.3311111111	2016-08-12 07:56:48	56383	2013-04-01 00:00:00	56587.6432291667	2013-10-22 15:26:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086002	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	8	AO8	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508081010/	Quick Look
85	MBM16	49.7641	11.5835	49.080496	11.40241	50.44037	-6.504342	170.59835317	-37.27294118	77.8263	56867.2632638889	2014-07-29 06:19:06	56869.0606018518	2014-07-31 01:27:16	509073010	78.81	80	78.818	78.818	0	78.81	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.4583449074	2016-08-16 11:00:01	56748	2014-04-01 00:00:00	56902.6996180556	2014-09-02 16:47:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096001	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	9	AO9	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509073010/	Quick Look
86	GB_NORTH_1	266.1004	-28.3619	265.30982	-28.341045	266.546613	-4.967513	0.35022505	0.52781175	106.0661	57104.6393981482	2015-03-23 15:20:44	57106.6752777778	2015-03-25 16:12:24	509077010	98.2407	100	98.2407	98.4407	0	98.4407	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8715277778	2016-08-17 20:55:00	56748	2014-04-01 00:00:00	57120.4153125	2015-04-08 09:58:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096002	The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	9	AO9	MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY-	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509077010/	Quick Look
87	GALACTIC_BULGE7	266.6764	-30.8281	265.869887	-30.809998	267.112733	-7.42025	358.50617228	-1.18471698	274.4326	55117.1787037037	2009-10-13 04:17:20	55118.4785416667	2009-10-14 11:29:06	504090010	41.2607	50	41.2607	52.9033	0	52.9033	3	2	0	2	1	0	0	34.964	34.964	112.2938	2	PROCESSED	57548.8825694444	2016-06-09 21:10:54	54922	2009-04-01 00:00:00	55133.2421643518	2009-10-29 05:48:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504090010/	Quick Look
88	GALACTIC_BULGE4	269.1417	-30.4015	268.337633	-30.395373	269.244618	-6.962713	359.95546853	-2.79264334	69.3552	55632.2752314815	2011-03-12 06:36:20	55633.4287152778	2011-03-13 10:17:21	505079010	50.2193	50	50.2273	50.2193	0	50.2273	2	2	0	2	1	0	0	43.375	43.375	99.648	1	PROCESSED	57601.1540277778	2016-08-01 03:41:48	55287	2010-04-01 00:00:00	55645.5706134259	2011-03-25 13:41:41	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505079010/	Quick Look
89	GALACTIC_BULGE5	270.1525	-30.903	269.345086	-30.901777	270.122341	-7.462063	359.95222621	-3.79644913	86.7823	55293.7188657407	2010-04-07 17:15:10	55295.8849074074	2010-04-09 21:14:16	505080010	56.1396	50	56.1396	56.1396	0	56.1396	2	2	0	2	1	0	0	55.1498	55.1498	185.0058	1	PROCESSED	57553.0630439815	2016-06-14 01:30:47	55287	2010-04-01 00:00:00	55441.4355555556	2010-09-02 10:27:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505080010/	Quick Look
90	THE KEPLER SNR	262.6707	-21.4823	261.92146	-21.444975	263.169631	1.785142	4.52498329	6.82417088	98.3356	55620.8079166667	2011-02-28 19:23:24	55624.797337963	2011-03-04 19:08:10	505092040	146.2337	250	146.2337	146.2541	0	146.2577	2	2	0	2	1	0	0	113.8022	113.8022	344.6577	6	PROCESSED	57601.192337963	2016-08-01 04:36:58	55287	2010-04-01 00:00:00	55642.4090046296	2011-03-22 09:48:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092040/	Quick Look
91	G350.1-0.3	260.2697	-37.4549	259.419167	-37.405796	262.032562	-14.282003	350.06545974	-0.33871818	266.4234	55821.2580787037	2011-09-17 06:11:38	55822.9126388889	2011-09-18 21:54:12	506065010	70.1813	70	70.1973	70.1813	0	70.1973	2	2	0	2	1	0	0	60.0704	60.0704	142.9159	0	PROCESSED	57603.2088541667	2016-08-03 05:00:45	55652	2011-04-01 00:00:00	55865.2679282407	2011-10-31 06:25:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506065010/	Quick Look
92	G337.2-0.7	249.8782	-47.8314	248.950154	-47.733478	255.175293	-25.419144	337.20769447	-0.7291284	280.8005	56172.5530439815	2012-09-02 13:16:23	56181.2598263889	2012-09-11 06:14:09	507068010	304.1484	300	304.1564	304.1484	0	304.1484	2	2	0	2	1	0	0	275.8448	275.8448	461.2638	9	PROCESSED	57607.2211111111	2016-08-07 05:18:24	56018	2012-04-01 00:00:00	56271.4641203704	2012-12-10 11:08:20	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	7	Ao7	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507068010/	Quick Look
93	GRXE_E_6	268.1913	-26.3855	267.412548	-26.37482	268.368065	-2.954748	3.00107417	-0.0433749	104.9996	56375.3653125	2013-03-24 08:46:03	56377.4119444445	2013-03-26 09:53:12	507073010	101.6745	100	101.6745	101.6745	0	101.6745	2	2	0	2	1	0	0	100.2473	100.2473	176.8078	1	PROCESSED	57610.9396296296	2016-08-10 22:33:04	56018	2012-04-01 00:00:00	56387.5561574074	2013-04-05 13:20:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507073010/	Quick Look
94	NGC3516	166.8656	72.6213	166.014761	72.891861	123.359499	58.056735	133.14023939	42.38468378	135.8338	55132.2328125	2009-10-28 05:35:15	55137.5272453704	2009-11-02 12:39:14	704062010	251.3555	250	251.3795	251.3715	0	251.3555	2	2	0	2	1	0	0	190.8372	190.8372	333.01	5	PROCESSED	57549.2037268518	2016-06-10 04:53:22	54922	2009-04-01 00:00:00	55152.2729398148	2009-11-17 06:33:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046003	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	4	AO4	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704062010/	Quick Look
95	GRXE_E_8	268.4708	-25.9492	267.69465	-25.939883	268.614118	-2.515578	3.50431952	-0.037979	86.7223	56718.7089236111	2014-03-02 17:00:51	56720.9585069445	2014-03-04 23:00:15	508077010	103.132	100	103.14	103.132	0	103.14	2	2	0	2	1	0	0	94.8538	94.8538	194.3449	2	PROCESSED	57613.971712963	2016-08-13 23:19:16	56383	2013-04-01 00:00:00	56775.6980787037	2014-04-28 16:45:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086001	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	8	AO8	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508077010/	Quick Look
96	GB_NORTH_2	265.5401	-28.4005	264.749404	-28.376931	266.05313	-5.020438	0.05846164	0.92703829	108.0199	57106.6765856482	2015-03-25 16:14:17	57108.7243634259	2015-03-27 17:23:05	509078010	95.3893	100	95.3893	99.8284	0	99.8124	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8717361111	2016-08-17 20:55:18	56748	2014-04-01 00:00:00	57119.4143981482	2015-04-07 09:56:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096002	The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	9	AO9	MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY-	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509078010/	Quick Look
97	GB_NORTH_3	265.8335	-28.3716	265.042917	-28.349452	266.311245	-4.983802	0.21886292	0.72273612	108.0564	57108.7249074074	2015-03-27 17:23:52	57110.9703703704	2015-03-29 23:17:20	509079010	106.9674	100	106.9674	108.1889	0	108.1889	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8792939815	2016-08-17 21:06:11	56748	2014-04-01 00:00:00	57119.4192708333	2015-04-07 10:03:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096002	The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	9	AO9	MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY-	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509079010/	Quick Look
98	SN1006_BGD4	226.2633	-42.7499	225.438524	-42.555935	236.137627	-24.311137	327.5160888	13.6541367	286.3809	56889.2090740741	2014-08-20 05:01:04	56889.7793865741	2014-08-20 18:42:19	509086010	33.5116	30	33.5156	33.5116	0	33.5196	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5076851852	2016-08-16 12:11:04	56748	2014-04-01 00:00:00	56910.6440162037	2014-09-10 15:27:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096004	We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		USA	9	AO9	THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509086010/	Quick Look
99	ABELL 426 SW1	49.6666	41.3604	48.840906	41.178725	58.340814	22.251887	150.47849352	-13.50469455	88.4985	55803.5918402778	2011-08-30 14:12:15	55803.8230671296	2011-08-30 19:45:13	806099010	11.5592	10	11.5752	11.5592	0	11.5752	2	2	0	2	1	0	0	11.5421	11.5421	19.9701	0	PROCESSED	57603.0124189815	2016-08-03 00:17:53	55652	2011-04-01 00:00:00	55826.1721875	2011-09-22 04:07:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806099010/	Quick Look
100	ABELL 426 SE4.5	51.0328	40.5957	50.208366	40.419106	59.183999	21.234356	151.7976658	-13.56504097	89.5625	55798.9213657407	2011-08-25 22:06:46	55799.1758912037	2011-08-26 04:13:17	806117010	12.0196	10	12.0196	12.0196	0	12.0356	1	1	0	1	1	0	0	10.4959	10.4959	21.9839	0	PROCESSED	57602.9577893518	2016-08-02 22:59:13	55652	2011-04-01 00:00:00	55855.1616435185	2011-10-21 03:52:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806117010/	Quick Look
101	ABELL 426 NE2.5	50.6676	41.9537	49.835188	41.775725	59.295588	22.616024	150.78054856	-12.59654862	89.499	55808.8756134259	2011-09-04 21:00:53	55809.0717592593	2011-09-05 01:43:20	806125010	9.7394	10	9.7554	9.7394	0	9.7634	1	1	0	1	1	0	0	7.3671	7.3671	16.9439	0	PROCESSED	57603.064224537	2016-08-03 01:32:29	55652	2011-04-01 00:00:00	55865.9792361111	2011-10-31 23:30:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806125010/	Quick Look
102	ABELL 426 NE4.5	51.271	42.2915	50.434611	42.115781	59.862037	22.81958	150.96498821	-12.06556882	89.4971	55809.84625	2011-09-05 20:18:36	55810.0452662037	2011-09-06 01:05:11	806129010	10.381	10	10.381	10.381	0	10.381	1	1	0	1	1	0	0	8.933	8.933	17.184	0	PROCESSED	57603.0777777778	2016-08-03 01:52:00	55652	2011-04-01 00:00:00	55866.1125462963	2011-11-01 02:42:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806129010/	Quick Look
103	ABELL 426 NE5.5	51.5754	42.4541	50.737042	42.279527	60.14462	22.915633	151.06006994	-11.8041168	89.4991	55810.5422569444	2011-09-06 13:00:51	55810.8217361111	2011-09-06 19:43:18	806131010	14.8458	15	14.8618	14.8618	0	14.8458	1	1	0	1	1	0	0	16.2198	16.2198	24.1439	0	PROCESSED	57603.0838310185	2016-08-03 02:00:43	55652	2011-04-01 00:00:00	55866.1408101852	2011-11-01 03:22:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806131010/	Quick Look
104	ABELL 426 NNE3.5	50.2092	42.4612	49.374656	42.281515	59.092741	23.197382	150.20252687	-12.36344342	60.4978	55804.7853125	2011-08-31 18:50:51	55805.0002546296	2011-09-01 00:00:22	806139010	10.02	10	10.02	10.02	0	10.02	1	1	0	1	1	0	0	9.507	9.507	18.5599	0	PROCESSED	57603.0247916667	2016-08-03 00:35:42	55652	2011-04-01 00:00:00	55830.1973958333	2011-09-26 04:44:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806139010/	Quick Look
105	A2199 OFFSET10	245.7785	38.4489	245.339389	38.564051	231.762092	58.713673	61.35085602	44.73212253	143.0073	55922.3113541667	2011-12-27 07:28:21	55923.0174074074	2011-12-28 00:25:04	806156010	32.686	30	32.686	32.686	0	32.686	2	2	0	2	1	0	0	30.452	30.452	60.9959	1	PROCESSED	57604.2399074074	2016-08-04 05:45:28	55652	2011-04-01 00:00:00	55972.658599537	2012-02-15 15:48:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806156010/	Quick Look
106	A2199 OFFSET13	247.4008	39.9951	246.975742	40.102999	233.166969	60.575403	63.55387948	43.51978117	252.5011	55815.2934375	2011-09-11 07:02:33	55815.9266203704	2011-09-11 22:14:20	806159010	28.648	20	28.648	29.3429	0	29.3589	1	1	0	1	1	0	0	26.7831	26.7831	54.6959	0	PROCESSED	57603.1066087963	2016-08-03 02:33:31	55652	2011-04-01 00:00:00	55851.4378703704	2011-10-17 10:30:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806159010/	Quick Look
107	ABELL 426 S2	49.8015	40.983	48.977877	40.801825	58.333099	21.861106	150.77920085	-13.76419767	87.9994	55425.2999884259	2010-08-17 07:11:59	55425.5946527778	2010-08-17 14:16:18	805097010	10.9046	10	10.9347	10.9286	0	10.9046	1	1	0	1	1	0	0	8.2387	8.2387	25.4559	0	PROCESSED	57553.0977546296	2016-06-14 02:20:46	55287	2010-04-01 00:00:00	55439.1113888889	2010-08-31 02:40:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805097010/	Quick Look
108	ABELL 426 S7	49.4762	39.609	48.662108	39.426644	57.669776	20.609139	151.34578769	-15.04805542	88.0004	55427.7102430556	2010-08-19 17:02:45	55428.0731481482	2010-08-20 01:45:20	805102010	17.2093	15	17.2093	17.2333	0	17.2173	2	2	0	2	1	0	0	13.7954	13.7954	31.3479	0	PROCESSED	57553.1341550926	2016-06-14 03:13:11	55287	2010-04-01 00:00:00	55439.2187847222	2010-08-31 05:15:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805102010/	Quick Look
109	ABELL 426 W2	49.2188	41.5721	48.392989	41.388782	58.056414	22.549036	150.07049245	-13.51031958	93.9951	55428.7403240741	2010-08-20 17:46:04	55428.9654513889	2010-08-20 23:10:15	805104010	9.9892	10	9.9972	9.9972	0	9.9892	1	1	0	1	1	0	0	7.2787	7.2787	19.4479	1	PROCESSED	57553.1453240741	2016-06-14 03:29:16	55287	2010-04-01 00:00:00	55460.9467708333	2010-09-21 22:43:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805104010/	Quick Look
110	ABELL 426 S6.5	49.508	39.7472	48.692971	39.56496	57.735719	20.735211	151.28830519	-14.91915669	87.9995	55427.3325115741	2010-08-19 07:58:49	55427.7099537037	2010-08-19 17:02:20	805112010	15.7046	15	15.7126	15.7046	0	15.7205	1	1	0	1	1	0	0	14.4033	14.4033	32.6079	0	PROCESSED	57553.1322222222	2016-06-14 03:10:24	55287	2010-04-01 00:00:00	55439.1853587963	2010-08-31 04:26:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805112010/	Quick Look
111	A2199 OFFSET9	246.619	38.9138	246.184603	39.025211	232.691568	59.360139	62.03199075	44.09189055	267.0002	55816.7374652778	2011-09-12 17:41:57	55817.4077546296	2011-09-13 09:47:10	806155010	28.1304	30	28.1304	28.1304	0	28.1304	3	2	0	2	1	0	0	27.0303	27.0303	57.8979	0	PROCESSED	57603.128287037	2016-08-03 03:04:44	55652	2011-04-01 00:00:00	55851.4428356482	2011-10-17 10:37:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806155010/	Quick Look
112	ABELL 426 W4.5	48.2846	41.6054	47.461248	41.418696	57.340677	22.779589	149.44545041	-13.85744176	86.9992	55429.5700347222	2010-08-21 13:40:51	55429.7800694444	2010-08-21 18:43:18	805114010	10.8576	10	10.8796	10.8656	0	10.8576	1	1	0	1	1	0	0	7.7343	7.7343	18.1439	0	PROCESSED	57553.1551388889	2016-06-14 03:43:24	55287	2010-04-01 00:00:00	55445.224224537	2010-09-06 05:22:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805114010/	Quick Look
113	ABELL 426 W6.5	47.5391	41.63	46.717762	41.440629	56.769366	22.964447	148.94387316	-14.13011853	94.0011	55430.6970601852	2010-08-22 16:43:46	55431.0425578704	2010-08-23 01:01:17	805116010	15.4086	15	16.0162	15.4086	0	16.0482	1	1	0	1	1	0	0	12.5812	12.5812	29.8399	0	PROCESSED	57553.1669560185	2016-06-14 04:00:25	55287	2010-04-01 00:00:00	55449.2772916667	2010-09-10 06:39:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805116010/	Quick Look
114	ABELL 426 SW2.5	49.2375	41.0889	48.414756	40.905656	57.924284	22.08131	150.35281041	-13.90838125	95.0009	55800.8414467593	2011-08-27 20:11:41	55801.0598611111	2011-08-28 01:26:12	806101010	10.6344	10	10.6584	10.6504	0	10.6344	1	1	0	1	1	0	0	10.3417	10.3417	18.8559	0	PROCESSED	57602.9850925926	2016-08-02 23:38:32	55652	2011-04-01 00:00:00	55818.1410069444	2011-09-14 03:23:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806101010/	Quick Look
115	ABELL 426 SW5	48.5394	40.6338	47.721481	40.448025	57.239803	21.793555	150.14795961	-14.57654163	88.4979	55802.0865856482	2011-08-29 02:04:41	55802.4896875	2011-08-29 11:45:09	806106010	16.7241	15	16.7401	16.7241	0	16.7481	2	2	0	2	1	0	0	13.0406	13.0406	34.8239	0	PROCESSED	57602.9971990741	2016-08-02 23:55:58	55652	2011-04-01 00:00:00	55826.1207638889	2011-09-22 02:53:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806106010/	Quick Look
116	ABELL 426 SE2.5	50.5437	41.0145	49.717849	40.836073	58.92258	21.737665	151.24059841	-13.42708975	89.5612	55797.9346180556	2011-08-24 22:25:51	55798.1676041667	2011-08-25 04:01:21	806113010	11.0423	10	11.0503	11.0583	0	11.0423	1	1	0	1	1	0	0	9.6711	9.6711	20.1199	0	PROCESSED	57602.9433217593	2016-08-02 22:38:23	55652	2011-04-01 00:00:00	55855.134849537	2011-10-21 03:14:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806113010/	Quick Look
117	ABELL 426 NE3.5	50.9699	42.1175	50.135538	41.940653	59.578071	22.712479	150.87690614	-12.33503289	89.4979	55809.4033333333	2011-09-05 09:40:48	55809.6251273148	2011-09-05 15:00:11	806127010	10.32	10	10.332	10.32	0	10.336	2	2	0	2	1	0	0	9.379	9.379	19.156	0	PROCESSED	57603.0714583333	2016-08-03 01:42:54	55652	2011-04-01 00:00:00	55866.0295833333	2011-11-01 00:42:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806127010/	Quick Look
118	ABELL 426 NE4	51.1184	42.2072	50.283013	42.030909	59.719337	22.768966	150.91831547	-12.19892536	89.4976	55808.4229282407	2011-09-04 10:09:01	55808.6738425926	2011-09-04 16:10:20	806128010	10.3385	10	10.3385	10.3465	0	10.3465	1	1	0	1	1	0	0	9.7761	9.7761	21.6719	0	PROCESSED	57603.0579282407	2016-08-03 01:23:25	55652	2011-04-01 00:00:00	55865.1235069444	2011-10-31 02:57:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806128010/	Quick Look
119	ABELL 426 NNE7	50.5088	43.4191	49.666767	43.240516	59.612457	24.057079	149.84713218	-11.44434377	60.4957	55807.8394560185	2011-09-03 20:08:49	55808.0773148148	2011-09-04 01:51:20	806146010	11.0932	10	11.0932	11.0932	0	11.0932	1	1	0	1	1	0	0	8.9534	8.9534	20.5199	0	PROCESSED	57603.0508217593	2016-08-03 01:13:11	55652	2011-04-01 00:00:00	55845.2850578704	2011-10-11 06:50:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806146010/	Quick Look
120	A2199 OFFSET4	247.7662	39.3698	247.336958	39.47607	234.094682	60.066425	62.70620415	43.21916708	270.0003	55791.1922337963	2011-08-18 04:36:49	55791.5912037037	2011-08-18 14:11:20	806150010	18.7116	20	18.7116	18.7116	0	18.7116	1	1	0	1	1	0	0	13.643	13.643	34.4639	0	PROCESSED	57602.8546064815	2016-08-02 20:30:38	55652	2011-04-01 00:00:00	55806.2666087963	2011-09-02 06:23:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806150010/	Quick Look
121	A2199 OFFSET5	248.9722	38.6569	248.539372	38.75774	236.294551	59.658507	61.80111812	42.24739511	272.0003	55791.5924652778	2011-08-18 14:13:09	55792.1787152778	2011-08-19 04:17:21	806151010	21.084	20	21.092	21.092	0	21.084	2	2	0	2	1	0	0	18.9536	18.9536	50.6459	0	PROCESSED	57602.8747916667	2016-08-02 20:59:42	55652	2011-04-01 00:00:00	55806.2354050926	2011-09-02 05:38:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806151010/	Quick Look
122	VIRGO N5	187.7004	14.5243	187.069101	14.800365	181.146119	16.359636	281.02135681	76.51020537	313.9964	56098.5183449074	2012-06-20 12:26:25	56098.9203125	2012-06-20 22:05:15	807110010	15.7789	13	15.7789	15.7894	0	15.7829	2	2	0	2	1	0	0	16.0728	16.0728	34.728	0	PROCESSED	57605.7329166667	2016-08-05 17:35:24	56018	2012-04-01 00:00:00	56214.963587963	2012-10-14 23:07:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807110010/	Quick Look
123	VIRGO S1	187.7666	12.1106	187.133775	12.386627	182.229484	14.183198	284.29495534	74.24059367	308.501	56111.2691087963	2012-07-03 06:27:31	56111.5314583333	2012-07-03 12:45:18	807115010	12.5216	10	12.5336	12.5216	0	12.5366	2	2	0	2	1	0	0	13.182	13.182	22.642	0	PROCESSED	57606.5476736111	2016-08-06 13:08:39	56018	2012-04-01 00:00:00	56226.6475	2012-10-26 15:32:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807115010/	Quick Look
124	A2199 OFFSET3	246.6242	39.5648	246.194654	39.676177	232.295962	59.97972	62.9383018	44.10633033	299.9982	55790.598287037	2011-08-17 14:21:32	55791.1863425926	2011-08-18 04:28:20	806149010	21.366	20	21.374	21.374	0	21.366	2	2	0	2	1	0	0	20.2743	20.2743	50.8019	1	PROCESSED	57602.8605787037	2016-08-02 20:39:14	55652	2011-04-01 00:00:00	55806.2156365741	2011-09-02 05:10:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806149010/	Quick Look
125	VIRGO S12	187.4953	8.619	186.859997	8.895202	183.424434	10.881709	286.60241823	70.80739613	122.0035	56270.1617592593	2012-12-09 03:52:56	56270.5772106482	2012-12-09 13:51:11	807126010	16.4275	16	16.4275	16.4275	0	16.4275	1	1	0	1	1	0	0	16.1837	16.1837	35.8639	0	PROCESSED	57608.2146527778	2016-08-08 05:09:06	56018	2012-04-01 00:00:00	56338.4929166667	2013-02-15 11:49:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807126010/	Quick Look
126	VIRGO S17	187.3614	6.7452	186.724859	7.021486	184.063087	9.111826	287.56473465	68.95823146	122.4996	56272.071724537	2012-12-11 01:43:17	56272.5258796296	2012-12-11 12:37:16	807131010	18.9432	18	18.9512	18.9432	0	18.9512	1	1	0	1	1	0	0	18.6145	18.6145	39.2319	1	PROCESSED	57608.241712963	2016-08-08 05:48:04	56018	2012-04-01 00:00:00	56291.7338773148	2012-12-30 17:36:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807131010/	Quick Look
127	VIRGO E1	188.0634	12.5322	187.431175	12.808036	182.325865	14.686251	284.88156742	74.72763223	285	56481.2981828704	2013-07-08 07:09:23	56481.5626736111	2013-07-08 13:30:15	808116010	10.3353	10	10.3353	10.3353	0	10.3353	2	2	0	2	1	0	0	8.8323	8.8323	22.8459	0	PROCESSED	57611.7060416667	2016-08-11 16:56:42	56383	2013-04-01 00:00:00	56524.6432407407	2013-08-20 15:26:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808116010/	Quick Look
128	VIRGO E5	189.1714	13.1819	188.540883	13.456957	183.073594	15.719707	288.31179147	75.63323247	284.9999	56482.4931365741	2013-07-09 11:50:07	56482.9348726852	2013-07-09 22:26:13	808120010	12.2986	12	12.2986	12.2986	0	12.2986	2	2	0	2	1	0	0	12.2671	12.2671	38.1619	0	PROCESSED	57611.7660300926	2016-08-11 18:23:05	56383	2013-04-01 00:00:00	56496.6035416667	2013-07-23 14:29:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808120010/	Quick Look
129	ABELL 426 SW3	49.102	40.9982	48.280214	40.814462	57.790981	22.022932	150.31514223	-14.0400409	94.9993	55801.0601967593	2011-08-28 01:26:41	55801.3084722222	2011-08-28 07:24:12	806102010	11.955	10	11.955	11.955	0	11.955	1	1	0	1	1	0	0	7.864	7.864	21.4239	1	PROCESSED	57602.9856134259	2016-08-02 23:39:17	55652	2011-04-01 00:00:00	55818.1485185185	2011-09-14 03:33:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806102010/	Quick Look
130	ABELL 426 SW6	48.2625	40.4485	47.446504	40.261728	56.965884	21.67573	150.06660907	-14.84565948	88.4982	55802.8164814815	2011-08-29 19:35:44	55803.0348958333	2011-08-30 00:50:15	806108010	11.5336	10	11.5656	11.5576	0	11.5336	1	1	0	1	1	0	0	10.7551	10.7551	18.8561	0	PROCESSED	57603.0017476852	2016-08-03 00:02:31	55652	2011-04-01 00:00:00	55826.1269444444	2011-09-22 03:02:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806108010/	Quick Look
131	ABELL 426 NE6	51.7255	42.539	50.886134	42.364994	60.28512	22.967764	151.10360581	-11.67130403	89.4994	55810.8220717593	2011-09-06 19:43:47	55811.0314583333	2011-09-07 00:45:18	806132010	11.4246	10	11.4406	11.4246	0	11.4486	1	1	0	1	1	0	0	10.0645	10.0645	18.0879	0	PROCESSED	57603.0828703704	2016-08-03 01:59:20	55652	2011-04-01 00:00:00	55866.2046759259	2011-11-01 04:54:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806132010/	Quick Look
132	ABELL 426 NNE6	50.4234	43.1429	49.58355	42.964001	59.463368	23.808902	149.95061465	-11.70868128	60.4955	55807.3026967593	2011-09-03 07:15:53	55807.5834375	2011-09-03 14:00:09	806144010	10.4306	10	10.4306	10.4306	0	10.4306	2	2	0	2	1	0	0	10.723	10.723	24.2539	0	PROCESSED	57603.0471990741	2016-08-03 01:07:58	55652	2011-04-01 00:00:00	55845.2864467593	2011-10-11 06:52:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806144010/	Quick Look
133	ABELL2345EAST	321.8675	-12.1557	321.189104	-12.37369	320.327375	2.690486	39.92441578	-40.06382879	77.2002	56777.6418402778	2014-04-30 15:24:15	56780.1466550926	2014-05-03 03:31:11	809119010	101.3009	100	101.3169	101.3009	0	101.3169	2	2	0	2	1	0	0	88.0885	88.0885	216.38	1	PROCESSED	57615.0703935185	2016-08-15 01:41:22	56748	2014-04-01 00:00:00	56790.7271759259	2014-05-13 17:27:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096003	Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROKI AKAMATSU		EUR	9	AO9	EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809119010/	Quick Look
134	VIRGO W4	186.6838	11.7876	186.04966	12.064261	181.367978	13.457626	281.0321598	73.60000956	100.001	56273.6409143518	2012-12-12 15:22:55	56273.9264699074	2012-12-12 22:14:07	807097010	14.512	11	14.512	14.536	0	14.52	2	2	0	2	1	0	0	13.7379	13.7379	24.6659	0	PROCESSED	57608.2576388889	2016-08-08 06:11:00	56018	2012-04-01 00:00:00	56342.5158680556	2013-02-19 12:22:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807097010/	Quick Look
135	VIRGO W9	185.2783	10.9356	184.642354	11.212937	180.431009	12.119991	277.70610968	72.30561596	99.9989	56275.8085763889	2012-12-14 19:24:21	56276.4093055556	2012-12-15 09:49:24	807102010	27.1057	23	27.1057	27.1057	0	27.1057	2	2	0	2	1	0	0	28.4791	28.4791	51.896	0	PROCESSED	57608.2880092593	2016-08-08 06:54:44	56018	2012-04-01 00:00:00	56315.5260300926	2013-01-23 12:37:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807102010/	Quick Look
136	VIRGO N4	187.7041	14.2061	187.072593	14.482163	181.285557	16.070988	281.49354158	76.21209693	310.9981	56104.178900463	2012-06-26 04:17:37	56104.463275463	2012-06-26 11:07:07	807109010	12.7577	12	12.7577	12.7577	0	12.7577	2	2	0	2	1	0	0	13.291	13.291	24.5619	0	PROCESSED	57606.4838541667	2016-08-06 11:36:45	56018	2012-04-01 00:00:00	56219.6559953704	2012-10-19 15:44:38	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807109010/	Quick Look
137	VIRGO S4	187.668	11.1668	187.034459	11.442891	182.532865	13.281501	284.92853674	73.30851588	308.5011	56112.2229861111	2012-07-04 05:21:06	56112.5056828704	2012-07-04 12:08:11	807118010	12.852	10	12.852	12.852	0	12.852	2	2	0	2	1	0	0	13.8622	13.8622	24.4179	0	PROCESSED	57606.5554282407	2016-08-06 13:19:49	56018	2012-04-01 00:00:00	56141.1138194445	2012-08-02 02:43:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807118010/	Quick Look
138	VIRGO S13	187.4758	8.312	186.840292	8.588214	183.531882	10.592818	286.77930619	70.50542211	122.0007	56270.5777314815	2012-12-09 13:51:56	56270.8459606482	2012-12-09 20:18:11	807127010	13.0666	12	13.0984	13.0906	0	13.0666	1	1	0	1	1	0	0	11.5411	11.5411	23.1679	0	PROCESSED	57608.2217824074	2016-08-08 05:19:22	56018	2012-04-01 00:00:00	56291.6901273148	2012-12-30 16:33:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807127010/	Quick Look
139	ABELL 426 S5	49.6049	40.1572	48.78706	39.975311	57.933438	21.108752	151.11933243	-14.5358666	87.9995	55426.4039930556	2010-08-18 09:41:45	55426.6474537037	2010-08-18 15:32:20	805100010	10.6209	10	10.6289	10.6209	0	10.6289	1	1	0	1	1	0	0	10.3257	10.3257	21.0319	0	PROCESSED	57553.1198148148	2016-06-14 02:52:32	55287	2010-04-01 00:00:00	55439.1414699074	2010-08-31 03:23:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805100010/	Quick Look
140	VIRGO S19	187.324	6.1182	186.687061	6.394509	184.281915	8.522189	287.8702994	68.34005974	122.7988	56272.9313310185	2012-12-11 22:21:07	56273.403587963	2012-12-12 09:41:10	807133010	19.3484	19	19.3601	19.3564	0	19.3484	2	2	0	2	1	0	0	20.7099	20.7099	40.798	0	PROCESSED	57608.2512384259	2016-08-08 06:01:47	56018	2012-04-01 00:00:00	56338.5094907407	2013-02-15 12:13:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807133010/	Quick Look
141	ABELL 426 S5.5	49.5719	40.0219	48.754994	39.839891	57.867374	20.985689	151.17444164	-14.66274998	88.0005	55426.6477430556	2010-08-18 15:32:45	55426.8585648148	2010-08-18 20:36:20	805111010	11.1329	10	11.1569	11.1409	0	11.1329	1	1	0	1	1	0	0	7.1518	7.1518	18.2079	0	PROCESSED	57553.1273032407	2016-06-14 03:03:19	55287	2010-04-01 00:00:00	55439.1544212963	2010-08-31 03:42:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805111010/	Quick Look
142	LDN1563	75.5225	13.8674	74.815655	13.796139	75.781481	-8.861998	187.1486738	-16.70848186	83.2339	56902.1301041667	2014-09-02 03:07:21	56904.0071643518	2014-09-04 00:10:19	509075010	41.1155	80	41.1396	41.1395	0	41.1155	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5646296296	2016-08-16 13:33:04	56748	2014-04-01 00:00:00	56926.5705439815	2014-09-26 13:41:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096001	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	9	AO9	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509075010/	Quick Look
143	SN1006_BGD1	225.9444	-42.5002	225.122216	-42.305131	235.809577	-24.144105	327.43636425	13.98792654	286.4314	56887.5218171296	2014-08-18 12:31:25	56888.0141203704	2014-08-19 00:20:20	509083010	32.1009	30	32.1089	32.1089	0	32.1009	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.5011111111	2016-08-16 12:01:36	56748	2014-04-01 00:00:00	56910.6401736111	2014-09-10 15:21:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096004	We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		USA	9	AO9	THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509083010/	Quick Look
144	VIRGO E8	190.0457	13.6937	189.416619	13.968069	183.664073	16.534019	291.30515449	76.31072684	284.9998	56483.6999768518	2013-07-10 16:47:58	56484.1918634259	2013-07-11 04:36:17	808123010	18.4482	18	18.4482	18.4482	0	18.4482	2	2	0	2	1	0	0	16.2122	16.2122	42.492	0	PROCESSED	57611.7962268518	2016-08-11 19:06:34	56383	2013-04-01 00:00:00	56498.6264351852	2013-07-25 15:02:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808123010/	Quick Look
145	G25.5+0.0	279.4506	-6.6057	278.777895	-6.649808	279.78518	16.514382	25.50196825	0.00652115	74.2354	54927.1234490741	2009-04-06 02:57:46	54928.7446064815	2009-04-07 17:52:14	504099010	52.7375	50	52.7375	52.7375	0	52.7375	2	2	0	2	1	0	0	44.5703	44.5703	140.042	3	PROCESSED	57546.0819675926	2016-06-07 01:58:02	54922	2009-04-01 00:00:00	54949.4845023148	2009-04-28 11:37:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504099010/	Quick Look
146	SN1006_BGD2	226.2226	-42.2202	225.40133	-42.0261	235.931519	-23.815123	327.76465581	14.12663913	286.4366	56888.0146875	2014-08-19 00:21:09	56888.6460416667	2014-08-19 15:30:18	509084010	34.8497	30	34.8793	34.8817	0	34.8497	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5054050926	2016-08-16 12:07:47	56748	2014-04-01 00:00:00	56910.6406365741	2014-09-10 15:22:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096004	We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		USA	9	AO9	THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509084010/	Quick Look
147	HESS J1841-55 1	279.8307	-5.8897	279.161498	-5.93564	280.231092	17.202355	26.31151486	-0.00077944	87.7391	55645.2916782407	2011-03-25 07:00:01	55646.4446180556	2011-03-26 10:40:15	505088010	49.652	50	49.652	49.652	0	49.652	2	2	0	2	1	0	0	39.8604	39.8604	99.5978	0	PROCESSED	57601.3329976852	2016-08-01 07:59:31	55287	2010-04-01 00:00:00	55658.1566087963	2011-04-07 03:45:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505088010/	Quick Look
148	SGR 0501+4516	75.2795	45.3414	74.367379	45.268539	78.857896	22.469212	161.49568149	1.98976538	93.3341	55060.8485069445	2009-08-17 20:21:51	55061.8348842593	2009-08-18 20:02:14	404078010	42.6753	40	42.6753	42.9553	0	42.8913	2	2	0	2	1	0	0	27.4878	27.4878	85.1858	0	PROCESSED	57548.1780092593	2016-06-09 04:16:20	54922	2009-04-01 00:00:00	55071.2594328704	2009-08-28 06:13:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	4	AO4	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404078010/	Quick Look
149	GALACTIC_BULGE12	270.5539	-32.7559	269.734001	-32.756597	270.462385	-9.315774	358.50046577	-5.00243267	271.4834	55119.6475462963	2009-10-15 15:32:28	55120.7502199074	2009-10-16 18:00:19	504095010	48.2622	50	48.2622	48.2622	0	48.2622	3	2	0	2	1	0	0	38.358	38.358	95.2619	1	PROCESSED	57548.9040856482	2016-06-09 21:41:53	54922	2009-04-01 00:00:00	55133.2742824074	2009-10-29 06:34:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504095010/	Quick Look
150	G346.6-0.2	257.5822	-40.1827	256.712432	-40.120751	260.089291	-17.167114	346.62898747	-0.22219097	278.7363	55111.704525463	2009-10-07 16:54:31	55113.1668287037	2009-10-09 04:00:14	504096010	56.7543	50	56.7543	56.7623	0	56.7703	2	2	0	2	1	0	0	42.4121	42.4121	126.3239	0	PROCESSED	57548.806724537	2016-06-09 19:21:41	54922	2009-04-01 00:00:00	55127.3766898148	2009-10-23 09:02:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504096010/	Quick Look
151	HESS J1841-55 4	280.4555	-5.2917	279.789233	-5.340638	280.927287	17.753088	27.12788601	-0.27973073	86.6744	55648.7926273148	2011-03-28 19:01:23	55649.9633449074	2011-03-29 23:07:13	505091010	51.2539	50	51.2539	51.2539	0	51.2539	2	2	0	2	1	0	0	45.0078	45.0078	101.142	1	PROCESSED	57601.3663310185	2016-08-01 08:47:31	55287	2010-04-01 00:00:00	55666.3000115741	2011-04-15 07:12:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505091010/	Quick Look
152	THE KEPLER SNR	262.671	-21.485	261.921744	-21.447676	263.170047	1.78246	4.52284766	6.82247636	99.4153	55649.9685416667	2011-03-29 23:14:42	55653.0828356482	2011-04-02 01:59:17	505092070	133.3906	90	133.3986	133.3986	0	133.3906	2	2	0	2	1	0	0	112.2172	112.2172	269.0278	1	PROCESSED	57601.4459490741	2016-08-01 10:42:10	55287	2010-04-01 00:00:00	55666.5226736111	2011-04-15 12:32:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092070/	Quick Look
153	G292.0+1.8	171.1489	-59.2723	170.582246	-58.997353	208.114622	-55.074076	292.03159099	1.74911685	309.5957	55764.9604050926	2011-07-22 23:02:59	55765.6883449074	2011-07-23 16:31:13	506062010	43.6592	40	43.6592	43.6592	0	43.6592	2	2	0	2	1	0	0	40.2364	40.2364	62.8859	1	PROCESSED	57602.6430902778	2016-08-02 15:26:03	55652	2011-04-01 00:00:00	55785.0141782407	2011-08-12 00:20:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506062010/	Quick Look
154	MBM20	68.9408	-14.6235	68.368117	-14.724858	64.47362	-36.218496	211.39729046	-36.55969232	255.8156	57069.9923842593	2015-02-16 23:49:02	57071.9654050926	2015-02-18 23:10:11	509076010	81.154	80	81.154	81.162	0	81.162	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.624537037	2016-08-17 14:59:20	56748	2014-04-01 00:00:00	57083.4173032407	2015-03-02 10:00:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096001	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	9	AO9	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509076010/	Quick Look
155	A2199 OFFSET14	246.2604	39.5212	245.829944	39.634196	231.792856	59.849359	62.86911341	44.38588157	254.9999	55825.6665625	2011-09-21 15:59:51	55826.3946527778	2011-09-22 09:28:18	806160010	27.4413	30	27.4414	27.4413	0	27.4413	3	2	0	2	1	0	0	26.9491	26.9491	62.9019	0	PROCESSED	57603.222962963	2016-08-03 05:21:04	55652	2011-04-01 00:00:00	55851.4517361111	2011-10-17 10:50:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806160010/	Quick Look
156	GALACTIC_BULGE13	264.5912	-32.1955	263.77613	-32.167278	265.360141	-8.841295	356.40747371	-0.39354159	92.0351	55635.5794907407	2011-03-15 13:54:28	55636.621099537	2011-03-16 14:54:23	505082010	48.4969	50	48.5129	48.5129	0	48.4969	2	2	0	2	1	0	0	41.255	41.255	89.9798	0	PROCESSED	57601.201412037	2016-08-01 04:50:02	55287	2010-04-01 00:00:00	55648.3385763889	2011-03-28 08:07:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505082010/	Quick Look
157	ABELL 426 W1	49.5928	41.5523	48.766062	41.370352	58.34119	22.451611	150.3228425	-13.37443973	94.0008	55428.5346759259	2010-08-20 12:49:56	55428.7397569445	2010-08-20 17:45:15	805103010	10.068	10	10.068	10.068	0	10.068	1	1	0	1	1	0	0	7.3213	7.3213	17.7119	0	PROCESSED	57553.1427777778	2016-06-14 03:25:36	55287	2010-04-01 00:00:00	55439.2175	2010-08-31 05:13:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805103010/	Quick Look
158	HESS J1841-55 2	280.1473	-5.9564	279.477798	-6.003856	280.554771	17.113097	26.39650339	-0.31125339	87.3564	55646.4452777778	2011-03-26 10:41:12	55647.6391550926	2011-03-27 15:20:23	505089010	50.0053	50	50.0304	50.0053	0	50.0304	3	2	0	2	1	0	0	43.1789	43.1789	103.1139	0	PROCESSED	57601.3264236111	2016-08-01 07:50:03	55287	2010-04-01 00:00:00	55658.2084606482	2011-04-07 05:00:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505089010/	Quick Look
159	LDN1563	75.5223	13.867	74.815457	13.795738	75.781245	-8.862376	187.14890409	-16.70886793	81.7388	56161.9528356482	2012-08-22 22:52:05	56164.0488194444	2012-08-25 01:10:18	507078010	78.6693	80	78.6693	78.6693	0	78.6693	2	2	0	2	1	0	0	69.6801	69.6801	181.0619	0	PROCESSED	57606.963275463	2016-08-06 23:07:07	56018	2012-04-01 00:00:00	56212.8492476852	2012-10-12 20:22:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076003	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	7	AO7	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507078010/	Quick Look
160	SGR 0501+4516	75.2625	45.3425	74.350391	45.26956	78.845173	22.471613	161.48747118	1.98100999	82.3996	55459.7272569444	2010-09-20 17:27:15	55460.9897337963	2010-09-21 23:45:13	405075010	59.7205	50	59.8085	59.8123	0	59.7205	3	2	0	2	1	0	0	52.9357	52.9357	109.0658	0	PROCESSED	57553.4903935185	2016-06-14 11:46:10	55287	2010-04-01 00:00:00	55470.1458449074	2010-10-01 03:30:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	5	AO5	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405075010/	Quick Look
161	ABELL 426 SW3.5	48.9544	40.9043	48.133622	40.720026	57.647111	21.964183	150.27094965	-14.17935173	88.4992	55801.3110763889	2011-08-28 07:27:57	55801.6063888889	2011-08-28 14:33:12	806103010	10.2636	10	10.2636	10.2636	0	10.2636	1	1	0	1	1	0	0	9.5689	9.5689	25.4719	1	PROCESSED	57602.9865046296	2016-08-02 23:40:34	55652	2011-04-01 00:00:00	55825.0922337963	2011-09-21 02:12:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806103010/	Quick Look
162	ABELL 426 SW4.5	48.6726	40.7228	47.853753	40.537505	57.371332	21.850286	150.18660509	-14.44721412	88.498	55801.850474537	2011-08-28 20:24:41	55802.08625	2011-08-29 02:04:12	806105010	10.7494	10	10.7574	10.7574	0	10.7494	1	1	0	1	1	0	0	8.915	8.915	20.3679	0	PROCESSED	57602.9947337963	2016-08-02 23:52:25	55652	2011-04-01 00:00:00	55826.0978935185	2011-09-22 02:20:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806105010/	Quick Look
163	ABELL 426 SW6.5	48.1163	40.3561	47.301281	40.168804	56.822706	21.618937	150.02002462	-14.98316021	88.4979	55803.0352314815	2011-08-30 00:50:44	55803.3008680556	2011-08-30 07:13:15	806109010	11.5806	10	11.5886	11.5806	0	11.5966	1	1	0	1	1	0	0	7.0679	7.0679	22.9359	0	PROCESSED	57603.0076041667	2016-08-03 00:10:57	55652	2011-04-01 00:00:00	55826.1781481482	2011-09-22 04:16:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806109010/	Quick Look
164	ABELL 426 SE5.5	51.277	40.3868	50.453278	40.211126	59.315931	20.983376	152.07695425	-13.63166747	96.5598	55799.6056828704	2011-08-26 14:32:11	55799.9189351852	2011-08-26 22:03:16	806119010	16.2703	15	16.2783	16.2703	0	16.2783	2	2	0	2	1	0	0	16.209	16.209	27.058	0	PROCESSED	57602.9656597222	2016-08-02 23:10:33	55652	2011-04-01 00:00:00	55865.074224537	2011-10-31 01:46:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806119010/	Quick Look
165	ABELL 426 NE1	50.2177	41.6975	49.388255	41.517855	58.870415	22.461609	150.64118254	-12.9960031	89.2472	55809.6259259259	2011-09-05 15:01:20	55809.8452662037	2011-09-05 20:17:11	806123010	10.9325	10	10.9325	10.9533	0	10.9405	1	1	0	1	1	0	0	12.2451	12.2451	18.9361	0	PROCESSED	57603.0729398148	2016-08-03 01:45:02	55652	2011-04-01 00:00:00	55866.0873842593	2011-11-01 02:05:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806123010/	Quick Look
166	ABELL 426 NNE6.5	50.4676	43.2769	49.626686	43.098164	59.537818	23.928739	149.90216136	-11.57929144	60.499	55807.5838194445	2011-09-03 14:00:42	55807.8391203704	2011-09-03 20:08:20	806145010	13.3332	10	13.3332	13.3332	0	13.3332	2	2	0	2	1	0	0	14.1621	14.1621	22.052	0	PROCESSED	57603.0507060185	2016-08-03 01:13:01	55652	2011-04-01 00:00:00	55845.2486226852	2011-10-11 05:58:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806145010/	Quick Look
167	GALACTIC_BULGE6	271.3758	-31.4828	270.564538	-31.487512	271.175264	-8.047458	359.95693453	-4.99276165	88.0304	55639.361087963	2011-03-19 08:39:58	55640.3565162037	2011-03-20 08:33:23	505081010	50.1669	50	50.1714	50.1669	0	50.1795	3	2	0	2	1	0	0	43.6357	43.6357	85.9898	0	PROCESSED	57601.2415277778	2016-08-01 05:47:48	55287	2010-04-01 00:00:00	55649.2186574074	2011-03-29 05:14:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505081010/	Quick Look
168	GALACTIC_BULGE14	264.9946	-32.433	264.177795	-32.406725	265.713815	-9.066176	356.38820164	-0.80858885	270.5244	55479.5865509259	2010-10-10 14:04:38	55480.8980671296	2010-10-11 21:33:13	505083010	52.9383	50	52.9383	52.9383	0	52.9383	1	1	0	1	1	0	0	42.4073	42.4073	113.3039	1	PROCESSED	57553.7064236111	2016-06-14 16:57:15	55287	2010-04-01 00:00:00	55491.0402893518	2010-10-22 00:58:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505083010/	Quick Look
169	THE KEPLER SNR	262.6745	-21.5044	261.925136	-21.467093	263.174286	1.76325	4.50818409	6.8092486	272.4561	55469.9826736111	2010-09-30 23:35:03	55470.368287037	2010-10-01 08:50:20	505092010	17.7141	620	17.7221	17.7301	0	17.7141	2	2	0	2	1	0	0	17.8694	17.8694	33.3079	0	PROCESSED	57553.595	2016-06-14 14:16:48	55287	2010-04-01 00:00:00	55482.4747453704	2010-10-13 11:23:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092010/	Quick Look
170	G272.2-3.2	136.7114	-52.1231	136.316281	-51.921066	170.818449	-63.077248	272.22308022	-3.18374401	297.1287	55709.5476041667	2011-05-28 13:08:33	55711.9009490741	2011-05-30 21:37:22	506060010	130.0782	150	130.0862	130.0942	0	130.0782	2	2	0	2	1	0	0	121.8303	121.8303	203.3058	3	PROCESSED	57602.216087963	2016-08-02 05:11:10	55652	2011-04-01 00:00:00	55735.3493171296	2011-06-23 08:23:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506060010/	Quick Look
171	GRXE_E_5	268.0495	-26.6011	267.269457	-26.589728	268.243808	-3.171982	2.75089625	-0.04390767	105.4995	56373.3059722222	2013-03-22 07:20:36	56375.3646990741	2013-03-24 08:45:10	507072010	101.2435	100	101.2435	101.2435	0	101.2435	2	2	0	2	1	0	0	102.6676	102.6676	177.8658	1	PROCESSED	57610.9241087963	2016-08-10 22:10:43	56018	2012-04-01 00:00:00	56384.595787037	2013-04-02 14:17:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507072010/	Quick Look
172	VIRGO W6	186.0979	11.4464	185.462989	11.723363	180.971644	12.912849	279.57270772	73.07967034	99.9988	56274.3472685185	2012-12-13 08:20:04	56274.8098726852	2012-12-13 19:26:13	807099010	22.4217	19	22.4217	22.4217	0	22.4217	2	2	0	2	1	0	0	19.182	19.182	39.9499	1	PROCESSED	57608.269224537	2016-08-08 06:27:41	56018	2012-04-01 00:00:00	56342.6277893518	2013-02-19 15:04:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807099010/	Quick Look
173	VIRGO W11	184.734	10.623	184.097417	10.900554	180.060818	11.617697	276.51178499	71.80735655	99.9988	56276.9834143518	2012-12-15 23:36:07	56277.5397337963	2012-12-16 12:57:13	807104010	24.3087	24	24.3087	24.311	0	24.3127	2	2	0	2	1	0	0	23.5095	23.5095	48.0381	0	PROCESSED	57608.2867361111	2016-08-08 06:52:54	56018	2012-04-01 00:00:00	56338.5029050926	2013-02-15 12:04:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807104010/	Quick Look
174	VIRGO N6	187.706	14.8589	187.074932	15.134961	181.007785	16.666841	280.53999282	76.82590701	310.9995	56104.4640740741	2012-06-26 11:08:16	56104.8946296296	2012-06-26 21:28:16	807111010	20.488	15	20.488	20.496	0	20.496	2	2	0	2	1	0	0	19.9025	19.9025	37.198	1	PROCESSED	57606.4880555556	2016-08-06 11:42:48	56018	2012-04-01 00:00:00	56117.9917361111	2012-07-09 23:48:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807111010/	Quick Look
175	VIRGO S2	187.7262	11.7827	187.093118	12.058753	182.329563	13.867553	284.50264567	73.91527115	308.5008	56111.5319791667	2012-07-03 12:46:03	56111.8286805556	2012-07-03 19:53:18	807116010	14.0408	10	14.0488	14.0408	0	14.0568	1	1	0	1	1	0	0	13.1631	13.1631	25.6319	0	PROCESSED	57606.5448611111	2016-08-06 13:04:36	56018	2012-04-01 00:00:00	56139.1771180556	2012-07-31 04:15:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807116010/	Quick Look
176	VIRGO S3	187.7051	11.4733	187.071794	11.749367	182.439346	13.576413	284.74763768	73.61284119	308.498	56111.8292013889	2012-07-03 19:54:03	56112.2224189815	2012-07-04 05:20:17	807117010	15.063	10	15.063	15.063	0	15.063	2	2	0	2	1	0	0	13.396	13.396	33.9619	0	PROCESSED	57606.5537384259	2016-08-06 13:17:23	56018	2012-04-01 00:00:00	56139.230787037	2012-07-31 05:32:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807117010/	Quick Look
177	VIRGO S9	187.5697	9.5888	186.935063	9.864954	183.095212	11.799058	286.04491696	71.76339412	306.8996	56115.2917361111	2012-07-07 07:00:06	56115.6641319444	2012-07-07 15:56:21	807123010	18.9179	14	18.9339	18.9179	0	18.9339	2	2	0	2	1	0	0	18.6185	18.6185	32.168	0	PROCESSED	57606.5741087963	2016-08-06 13:46:43	56018	2012-04-01 00:00:00	56142.0874884259	2012-08-03 02:05:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807123010/	Quick Look
178	VIRGO S14	187.4376	7.6823	186.801678	7.958538	183.753215	10.000828	287.13089499	69.88593318	122	56270.8466666667	2012-12-09 20:19:12	56271.2320717593	2012-12-10 05:34:11	807128010	15.4204	12	15.4364	15.4204	0	15.4444	1	1	0	1	1	0	0	16.7417	16.7417	33.2879	0	PROCESSED	57608.2246643518	2016-08-08 05:23:31	56018	2012-04-01 00:00:00	56291.692349537	2012-12-30 16:36:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807128010/	Quick Look
179	VIRGO S15	187.3986	7.3548	186.762452	7.631062	183.850325	9.685273	287.25281516	69.55887671	122.0016	56271.2325925926	2012-12-10 05:34:56	56271.6272106482	2012-12-10 15:03:11	807129010	18.2136	16	18.2296	18.2136	0	18.2296	1	1	0	1	1	0	0	17.3218	17.3218	34.056	0	PROCESSED	57608.2302430556	2016-08-08 05:31:33	56018	2012-04-01 00:00:00	56291.7069328704	2012-12-30 16:57:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807129010/	Quick Look
180	ABELL 426 W7.5	47.1647	41.6449	46.344371	41.454202	56.483409	23.060639	148.68932505	-14.26285782	94.0006	55431.5082175926	2010-08-23 12:11:50	55431.8251967593	2010-08-23 19:48:17	805117010	15.0656	15	15.0896	15.0656	0	15.0896	1	1	0	1	1	0	0	10.992	10.992	27.3839	0	PROCESSED	57553.174525463	2016-06-14 04:11:19	55287	2010-04-01 00:00:00	55446.2098263889	2010-09-07 05:02:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805117010/	Quick Look
181	ABELL 426 SE5	51.1493	40.4958	50.325207	40.319644	59.246759	21.114379	151.9309414	-13.59719782	89.5614	55799.1762268518	2011-08-26 04:13:46	55799.6029861111	2011-08-26 14:28:18	806118010	16.4382	15	16.4462	16.4382	0	16.4538	2	2	0	2	1	0	0	13.2539	13.2539	36.8699	0	PROCESSED	57602.9664814815	2016-08-02 23:11:44	55652	2011-04-01 00:00:00	55855.1847685185	2011-10-21 04:26:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806118010/	Quick Look
182	VIRGO E7	189.7478	13.5221	189.118223	13.796711	183.461681	16.259141	290.25286309	76.08652265	285.0003	56483.2548842593	2013-07-10 06:07:02	56483.6994560185	2013-07-10 16:47:13	808122010	18.1665	17	18.1665	18.1905	0	18.1745	2	2	0	2	1	0	0	15.6917	15.6917	38.4039	2	PROCESSED	57611.7926273148	2016-08-11 19:01:23	56383	2013-04-01 00:00:00	56496.6013657407	2013-07-23 14:25:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808122010/	Quick Look
183	VIRGO N7	187.7068	15.1871	187.075953	15.46316	180.867336	16.966208	280.02627988	77.13302603	311	56104.895150463	2012-06-26 21:29:01	56105.2924768518	2012-06-27 07:01:10	807112010	18.1828	16	18.1828	18.2059	0	18.1908	2	2	0	2	1	0	0	16.604	16.604	34.3279	0	PROCESSED	57606.4965393518	2016-08-06 11:55:01	56018	2012-04-01 00:00:00	56117.9967013889	2012-07-09 23:55:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807112010/	Quick Look
184	A2199 OFFSET8	247.7871	40.0108	247.362763	40.116965	233.730787	60.681855	63.58609445	43.22438175	270.3665	55796.7271180556	2011-08-23 17:27:03	55797.4578703704	2011-08-24 10:59:20	806154010	30.7084	30	30.7084	30.7084	0	30.7084	2	2	0	2	1	0	0	25.6487	25.6487	63.134	2	PROCESSED	57602.9315046296	2016-08-02 22:21:22	55652	2011-04-01 00:00:00	55806.3170138889	2011-09-02 07:36:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806154010/	Quick Look
185	ABELL 426 SE6	51.3915	40.2857	50.568134	40.110458	59.377203	20.862689	152.21004388	-13.66501615	96.5621	55799.9192708333	2011-08-26 22:03:45	55800.1515856482	2011-08-27 03:38:17	806120010	10.1455	10	10.1455	10.1695	0	10.1535	1	1	0	1	1	0	0	8.8587	8.8587	20.0639	0	PROCESSED	57602.969212963	2016-08-02 23:15:40	55652	2011-04-01 00:00:00	55865.0772569444	2011-10-31 01:51:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806120010/	Quick Look
186	ABELL 426 NE2	50.5182	41.8628	49.686815	41.684269	59.152818	22.559001	150.73800989	-12.73403508	89.4986	55808.6745949074	2011-09-04 16:11:25	55808.8752314815	2011-09-04 21:00:20	806124010	10.2106	10	10.2426	10.2346	0	10.2106	1	1	0	1	1	0	0	11.6835	11.6835	17.3279	0	PROCESSED	57603.0596412037	2016-08-03 01:25:53	55652	2011-04-01 00:00:00	55865.9664467593	2011-10-31 23:11:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806124010/	Quick Look
187	ABELL 426 NE3	50.8162	42.0347	49.982827	41.857279	59.43466	22.663828	150.82784183	-12.4676031	89.4977	55809.0721412037	2011-09-05 01:43:53	55809.4029513889	2011-09-05 09:40:15	806126010	10.5666	10	10.5666	10.5906	0	10.5746	2	2	0	2	1	0	0	10.704	10.704	28.5759	0	PROCESSED	57603.0680902778	2016-08-03 01:38:03	55652	2011-04-01 00:00:00	55866.0158333333	2011-11-01 00:22:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806126010/	Quick Look
188	ABELL 426 NE7	52.033	42.7019	51.191639	42.529059	60.569296	23.064384	151.19797458	-11.40826829	89.5003	55811.3970486111	2011-09-07 09:31:45	55811.6487384259	2011-09-07 15:34:11	806134010	11.079	10	11.0908	11.087	0	11.079	3	2	0	2	1	0	0	10.7886	10.7886	21.7361	0	PROCESSED	57603.0933449074	2016-08-03 02:14:25	55652	2011-04-01 00:00:00	55868.9251967593	2011-11-03 22:12:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806134010/	Quick Look
189	ABELL 426 NNE2	50.087	42.0498	49.255577	41.869667	58.874503	22.827107	150.35811431	-12.75634017	60.4956	55804.0547916667	2011-08-31 01:18:54	55804.3098726852	2011-08-31 07:26:13	806136010	10.686	10	10.686	10.686	0	10.686	1	1	0	1	1	0	0	6.899	6.899	22.0319	1	PROCESSED	57603.0180208333	2016-08-03 00:25:57	55652	2011-04-01 00:00:00	55830.1908333333	2011-09-26 04:34:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806136010/	Quick Look
190	ABELL 426 NNE3	50.1707	42.3226	49.337205	42.142774	59.021278	23.072073	150.2566965	-12.4946686	60.4975	55804.5824189815	2011-08-31 13:58:41	55804.7849768518	2011-08-31 18:50:22	806138010	9.859	10	9.859	9.859	0	9.859	3	2	0	2	1	0	0	10.125	10.125	17.4719	0	PROCESSED	57603.0234606482	2016-08-03 00:33:47	55652	2011-04-01 00:00:00	55871.8708680556	2011-11-06 20:54:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806138010/	Quick Look
191	VIRGO W1	187.5107	12.2426	186.877692	12.518786	181.938422	14.202058	283.26919479	74.29186005	291.9999	56110.6712847222	2012-07-02 16:06:39	56110.9370138889	2012-07-02 22:29:18	807094010	12.7859	10	12.7939	12.7939	0	12.7859	1	1	0	1	1	0	0	10.5429	10.5429	22.9519	0	PROCESSED	57606.5451157407	2016-08-06 13:04:58	56018	2012-04-01 00:00:00	56127.137662037	2012-07-19 03:18:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807094010/	Quick Look
192	VIRGO W7	185.8245	11.2655	185.18923	11.542594	180.795697	12.638786	278.94638045	72.81351487	99.9999	56274.8104398148	2012-12-13 19:27:02	56275.3217013889	2012-12-14 07:43:15	807100010	23.4449	20	23.4529	23.4529	0	23.4449	2	2	0	2	1	0	0	25.0353	25.0353	44.1699	0	PROCESSED	57608.2724652778	2016-08-08 06:32:21	56018	2012-04-01 00:00:00	56338.5069560185	2013-02-15 12:10:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807100010/	Quick Look
193	VIRGO W8	185.551	11.0911	184.915383	11.368319	180.616918	12.370601	278.32881118	72.55156974	99.4998	56275.3224074074	2012-12-14 07:44:16	56275.8078240741	2012-12-14 19:23:16	807101010	22.1703	21	22.1783	22.1703	0	22.1863	2	2	0	2	1	0	0	18.8585	18.8585	41.918	0	PROCESSED	57608.2782291667	2016-08-08 06:40:39	56018	2012-04-01 00:00:00	56315.5145023148	2013-01-23 12:20:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807101010/	Quick Look
194	VIRGO N1	187.7027	13.2607	187.070564	13.536766	181.686135	15.207962	282.74012713	75.31771863	314.0012	56097.8290740741	2012-06-19 19:53:52	56098.0419328704	2012-06-20 01:00:23	807106010	9.9319	10	9.9319	9.9399	0	9.9399	1	1	0	1	1	0	0	9.542	9.542	18.3839	0	PROCESSED	57605.7042592593	2016-08-05 16:54:08	56018	2012-04-01 00:00:00	56225.4789699074	2012-10-25 11:29:43	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807106010/	Quick Look
195	VIRGO N2	187.703	13.5671	187.071067	13.843165	181.556537	15.487683	282.35217615	75.60823465	313.9984	56098.0424074074	2012-06-20 01:01:04	56098.2606828704	2012-06-20 06:15:23	807107010	10.7068	10	10.7068	10.7308	0	10.7148	1	1	0	1	1	0	0	8.659	8.659	18.848	1	PROCESSED	57605.7127777778	2016-08-05 17:06:24	56018	2012-04-01 00:00:00	56214.9560763889	2012-10-14 22:56:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807107010/	Quick Look
196	VIRGO N8	187.7075	15.4944	187.076861	15.770459	180.735378	17.246403	279.52276063	77.41962086	310.9997	56105.2930439815	2012-06-27 07:01:59	56105.7028703704	2012-06-27 16:52:08	807113010	18.7018	18	18.7057	18.7018	0	18.7097	2	2	0	2	1	0	0	18.7504	18.7504	35.4	0	PROCESSED	57606.4979050926	2016-08-06 11:56:59	56018	2012-04-01 00:00:00	56118.0144097222	2012-07-10 00:20:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807113010/	Quick Look
197	VIRGO N9	187.7056	15.8164	187.075176	16.092459	180.594255	17.538861	278.95935226	77.71791573	310.4995	56106.6618171296	2012-06-28 15:53:01	56107.1398611111	2012-06-29 03:21:24	807114010	22.9788	19	22.9788	23.0059	0	22.9788	1	1	0	1	1	0	0	20.6819	20.6819	41.2959	1	PROCESSED	57606.5125578704	2016-08-06 12:18:05	56018	2012-04-01 00:00:00	56118.0912037037	2012-07-10 02:11:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807114010/	Quick Look
198	VIRGO S6	187.6479	10.5513	187.013944	10.827404	182.769907	12.710704	285.44540552	72.71150131	308.4999	56112.7686574074	2012-07-04 18:26:52	56113.0799421296	2012-07-05 01:55:07	807120010	12.7014	10	12.7014	12.7014	0	12.7014	1	1	0	1	1	0	0	10.5005	10.5005	26.8879	1	PROCESSED	57606.5642361111	2016-08-06 13:32:30	56018	2012-04-01 00:00:00	56141.2151388889	2012-08-02 05:09:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807120010/	Quick Look
199	VIRGO S10	187.554	9.2735	186.919151	9.549665	183.210349	11.504238	286.25782629	71.4549429	121.999	56269.421712963	2012-12-08 10:07:16	56269.7570717593	2012-12-08 18:10:11	807124010	16.098	16	16.098	16.098	0	16.098	1	1	0	1	1	0	0	13.413	13.413	28.952	0	PROCESSED	57608.2049074074	2016-08-08 04:55:04	56018	2012-04-01 00:00:00	56336.4667824074	2013-02-13 11:12:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807124010/	Quick Look
200	VIRGO E2	188.3405	12.688	187.708685	12.963651	182.515676	14.938652	285.71074231	74.9520878	284.9998	56481.5631944444	2013-07-08 13:31:00	56481.9592824074	2013-07-08 23:01:22	808117010	10.6598	10	10.6598	10.6598	0	10.6598	2	2	0	2	1	0	0	10.6982	10.6982	34.22	0	PROCESSED	57611.7227199074	2016-08-11 17:20:43	56383	2013-04-01 00:00:00	56524.654212963	2013-08-20 15:42:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808117010/	Quick Look
201	VIRGO E4	188.894	12.9933	188.263024	13.268562	182.897357	15.437334	287.44169131	75.38588793	285.0007	56482.2160069445	2013-07-09 05:11:03	56482.4926157407	2013-07-09 11:49:22	808119010	12.9687	11	12.9927	12.9847	0	12.9687	1	1	0	1	1	0	0	9.283	9.283	23.8959	0	PROCESSED	57611.7741319444	2016-08-11 18:34:45	56383	2013-04-01 00:00:00	56496.5935185185	2013-07-23 14:14:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808119010/	Quick Look
202	VIRGO E9	190.3236	13.8446	189.694982	14.118738	183.856818	16.782028	292.32223865	76.50695206	284.9995	56484.1924305556	2013-07-11 04:37:06	56484.6162268518	2013-07-11 14:47:22	808124010	18.8719	18	18.8951	18.8879	0	18.8719	2	2	0	2	1	0	0	15.3674	15.3674	36.6119	0	PROCESSED	57611.8197106482	2016-08-11 19:40:23	56383	2013-04-01 00:00:00	56498.6214930556	2013-07-25 14:54:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808124010/	Quick Look
203	VIRGO E11	190.8574	14.15	190.229706	14.423674	184.22049	17.272492	294.34392528	76.88802661	285	56485.1965162037	2013-07-12 04:42:59	56485.8154513889	2013-07-12 19:34:15	808126010	23.3591	21	23.3671	23.3591	0	23.3737	2	2	0	2	1	0	0	19.9937	19.9937	53.4699	1	PROCESSED	57611.8143171296	2016-08-11 19:32:37	56383	2013-04-01 00:00:00	56498.6447106482	2013-07-25 15:28:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808126010/	Quick Look
204	1RXS J1708-4009	257.2032	-40.2034	256.333623	-40.139657	259.789477	-17.214031	346.44001394	-0.00188973	266.4021	55066.6841203704	2009-08-23 16:25:08	55067.9466898148	2009-08-24 22:43:14	404080010	60.8869	60	60.8869	60.8949	0	60.9046	3	2	0	2	1	0	0	51.5313	51.5313	109.0758	1	PROCESSED	57548.350150463	2016-06-09 08:24:13	54922	2009-04-01 00:00:00	55078.1751851852	2009-09-04 04:12:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	4	AO4	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404080010/	Quick Look
205	GX 1+4	263.0071	-24.816	262.238766	-24.780248	263.643916	-1.529018	1.87675865	4.75818757	273.1727	55471.2801273148	2010-10-02 06:43:23	55473.5140509259	2010-10-04 12:20:14	405077010	99.67	100	99.6704	99.67	0	99.6704	3	2	0	2	1	0	0	96.5259	96.5259	192.6091	0	PROCESSED	57553.6626967593	2016-06-14 15:54:17	55287	2010-04-01 00:00:00	55487.4199537037	2010-10-18 10:04:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056002	We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	5	AO5	A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405077010/	Quick Look
206	ABELL 426 S4.5	49.6359	40.2959	48.817105	40.114123	57.998946	21.235515	151.06094801	-14.4070178	87.9989	55426.0734375	2010-08-18 01:45:45	55426.4037037037	2010-08-18 09:41:20	805110010	9.1793	10	9.1793	9.1793	0	9.1793	2	2	0	2	1	0	0	6.7459	6.7459	28.53	0	PROCESSED	57553.1162384259	2016-06-14 02:47:23	55287	2010-04-01 00:00:00	55439.1536342593	2010-08-31 03:41:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805110010/	Quick Look
207	THE KEPLER SNR	262.6706	-21.4823	261.92136	-21.444974	263.169538	1.785137	4.52493262	6.82424916	102.5027	55615.8474421296	2011-02-23 20:20:19	55616.8174768518	2011-02-24 19:37:10	505092030	34.2015	150	34.2095	34.2015	0	34.2095	2	2	0	2	1	0	0	29.1199	29.1199	83.7958	0	PROCESSED	57601.0436342593	2016-08-01 01:02:50	55287	2010-04-01 00:00:00	55628.1747569444	2011-03-08 04:11:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092030/	Quick Look
208	MBM16	49.7645	11.5821	49.080902	11.401011	50.440387	-6.505796	170.59989958	-37.2737153	77.5997	56511.9409027778	2013-08-07 22:34:54	56513.916875	2013-08-09 22:00:18	508078010	82.3246	80	82.3246	82.3246	0	82.3246	2	2	0	2	1	0	0	79.0718	79.0718	170.6898	2	PROCESSED	57612.2763541667	2016-08-12 06:37:57	56383	2013-04-01 00:00:00	56587.6759490741	2013-10-22 16:13:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086002	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	8	AO8	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508078010/	Quick Look
209	MBM36	238.3853	-4.8926	237.724645	-4.745297	237.254427	15.02643	3.92555744	35.61619893	279.5456	56531.6987268518	2013-08-27 16:46:10	56533.8883333333	2013-08-29 21:19:12	508079020	79.6067	80	79.6067	79.6067	0	79.6067	2	2	0	2	1	0	0	67.717	67.717	189.166	2	PROCESSED	57612.4621064815	2016-08-12 11:05:26	56383	2013-04-01 00:00:00	56603.7246875	2013-11-07 17:23:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086002	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	8	AO8	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508079020/	Quick Look
210	SN1006_BGD3	226.4731	-42.5186	225.649158	-42.32537	236.222692	-24.044133	327.77356316	13.77561257	286.5156	56888.6466550926	2014-08-19 15:31:11	56889.2084606482	2014-08-20 05:00:11	509085010	31.65	30	31.65	31.65	0	31.65	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5050115741	2016-08-16 12:07:13	56748	2014-04-01 00:00:00	56910.6423611111	2014-09-10 15:25:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096004	We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		USA	9	AO9	THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509085010/	Quick Look
211	ABELL 426 S1	49.8666	41.2611	49.040997	41.080162	58.466927	22.114789	150.66369426	-13.50507569	88	55424.9920601852	2010-08-16 23:48:34	55425.2995138889	2010-08-17 07:11:18	805096010	8.4343	10	8.4423	8.4503	0	8.4343	2	2	0	2	1	0	0	7.8611	7.8611	26.5499	0	PROCESSED	57553.0919675926	2016-06-14 02:12:26	55287	2010-04-01 00:00:00	55439.0952662037	2010-08-31 02:17:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805096010/	Quick Look
212	ABELL 426 S6	49.5399	39.884	48.723938	39.701875	57.801339	20.859927	151.23166434	-14.79141746	87.9993	55426.858900463	2010-08-18 20:36:49	55427.3321759259	2010-08-19 07:58:20	805101010	16.4888	15	16.5048	16.5048	0	16.4888	2	2	0	2	1	0	0	13.4845	13.4845	40.8879	1	PROCESSED	57553.1336342593	2016-06-14 03:12:26	55287	2010-04-01 00:00:00	55439.1815625	2010-08-31 04:21:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805101010/	Quick Look
213	ABELL 426 W3	48.8462	41.5856	48.021362	41.400926	57.770933	22.640736	149.82172461	-13.64958161	93.9989	55428.9659722222	2010-08-20 23:11:00	55429.3022916667	2010-08-21 07:15:18	805105010	11.1661	10	11.1901	11.1821	0	11.1661	2	2	0	2	1	0	0	9.1647	9.1647	29.036	0	PROCESSED	57553.1487962963	2016-06-14 03:34:16	55287	2010-04-01 00:00:00	55445.2284143518	2010-09-06 05:28:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805105010/	Quick Look
214	ABELL 426 W5	48.1001	41.6131	47.277233	41.425733	57.199753	22.826654	149.32075885	-13.92405492	94.0016	55429.7828125	2010-08-21 18:47:15	55429.9946296296	2010-08-21 23:52:16	805107010	9.2192	10	9.2192	9.2192	0	9.2192	2	2	0	2	1	0	0	7.8166	7.8166	18.2979	0	PROCESSED	57553.1586689815	2016-06-14 03:48:29	55287	2010-04-01 00:00:00	55445.231087963	2010-09-06 05:32:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805107010/	Quick Look
215	THE KEPLER SNR	262.6712	-21.4826	261.921958	-21.445277	263.170111	1.784866	4.52498243	6.82361728	97.9009	55634.5331712963	2011-03-14 12:47:46	55635.5759606482	2011-03-15 13:49:23	505092060	46.4961	100	46.6401	46.4961	0	46.6401	2	2	0	2	1	0	0	38.6118	38.6118	90.05	1	PROCESSED	57601.1934143518	2016-08-01 04:38:31	55287	2010-04-01 00:00:00	55648.2987731482	2011-03-28 07:10:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	5	AO5	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092060/	Quick Look
216	MBM16	49.7705	11.5801	49.086905	11.399033	50.445581	-6.509248	170.60706006	-37.27124926	254.3335	56691.5957175926	2014-02-03 14:17:50	56693.5209953704	2014-02-05 12:30:14	508078020	87.8509	80	87.8509	87.8589	0	87.8589	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57613.7866782407	2016-08-13 18:52:49	56383	2013-04-01 00:00:00	56706.5234375	2014-02-18 12:33:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086002	Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions.	GALACTIC DIFFUSE EMISSION	5	A	MASSIMILIANO GALEAZZI		USA	8	AO8	CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508078020/	Quick Look
217	ABELL 426 SE7	51.6308	40.0717	50.808198	39.897364	59.505151	20.607904	152.49041219	-13.73591885	87.5626	55800.376875	2011-08-27 09:02:42	55800.6418055556	2011-08-27 15:24:12	806122010	10.3288	10	10.3288	10.3288	0	10.3288	2	2	0	2	1	0	0	9.822	9.822	22.8839	0	PROCESSED	57602.977337963	2016-08-02 23:27:22	55652	2011-04-01 00:00:00	55865.0862731482	2011-10-31 02:04:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806122010/	Quick Look
218	ABELL 426 NE5	51.4212	42.371	50.583845	42.195846	60.001331	22.866197	151.01253218	-11.93716766	89.4976	55810.0456481482	2011-09-06 01:05:44	55810.5418287037	2011-09-06 13:00:14	806130010	17.5276	15	17.5276	17.5356	0	17.5356	2	2	0	2	1	0	0	17.7802	17.7802	42.862	0	PROCESSED	57603.0838888889	2016-08-03 02:00:48	55652	2011-04-01 00:00:00	55866.1625925926	2011-11-01 03:54:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806130010/	Quick Look
219	ABELL 426 NE6.5	51.8822	42.6245	51.041802	42.451087	60.430729	23.019323	151.15044966	-11.53522591	89.4983	55811.0317939815	2011-09-07 00:45:47	55811.396712963	2011-09-07 09:31:16	806133010	10.2804	10	10.2959	10.2879	0	10.2804	2	2	0	2	1	0	0	13.7277	13.7277	31.5259	0	PROCESSED	57603.0893634259	2016-08-03 02:08:41	55652	2011-04-01 00:00:00	55866.233587963	2011-11-01 05:36:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806133010/	Quick Look
220	VIRGO W3	186.9593	11.946	186.325534	12.222509	181.555181	13.711892	281.75004157	73.83934761	99.9993	56273.4086921296	2012-12-12 09:48:31	56273.6403472222	2012-12-12 15:22:06	807096010	10.8424	10	10.8504	10.8504	0	10.8424	1	1	0	1	1	0	0	9.0921	9.0921	20.0079	0	PROCESSED	57608.2529282407	2016-08-08 06:04:13	56018	2012-04-01 00:00:00	56342.4989699074	2013-02-19 11:58:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807096010/	Quick Look
221	VIRGO S7	187.6096	10.2244	186.9754	10.500529	182.869873	12.396474	285.61941254	72.38660135	308.5009	56113.0805092593	2012-07-05 01:55:56	56113.4293518518	2012-07-05 10:18:16	807121010	14.9979	13	14.9979	14.9979	0	14.9979	2	2	0	2	1	0	0	15.746	15.746	30.1359	0	PROCESSED	57606.5659606482	2016-08-06 13:34:59	56018	2012-04-01 00:00:00	56141.9783101852	2012-08-02 23:28:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807121010/	Quick Look
222	VIRGO E3	188.6166	12.8387	187.985199	13.11416	182.706731	15.185969	286.56417369	75.16845975	284.999	56481.9598032407	2013-07-08 23:02:07	56482.2154861111	2013-07-09 05:10:18	808118010	12.3275	10	12.3355	12.3355	0	12.3275	1	1	0	1	1	0	0	10.334	10.334	22.0879	0	PROCESSED	57611.7501851852	2016-08-11 18:00:16	56383	2013-04-01 00:00:00	56495.6160185185	2013-07-22 14:47:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086003	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	8	AO8	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808118010/	Quick Look
223	ZWCL0008.8+5215 EAST	3.1134	52.6387	2.455083	52.360692	29.755774	45.738765	116.94843434	-9.77955026	65.9987	56844.7667939815	2014-07-06 18:24:11	56847.5876273148	2014-07-09 14:06:11	809118010	117.8473	120	117.8473	119.9094	0	119.9334	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.3793518518	2016-08-15 09:06:16	56748	2014-04-01 00:00:00	56859.7336111111	2014-07-21 17:36:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	096003	Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROKI AKAMATSU		EUR	9	AO9	EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809118010/	Quick Look
224	KES 79	283.1953	0.6959	282.557686	0.633849	284.399792	23.479242	33.70438491	0.01846016	73.5801	55674.9437152778	2011-04-23 22:38:57	55676.4716782407	2011-04-25 11:19:13	506059010	50.897	50	50.897	50.897	0	50.897	2	2	0	2	1	0	0	40.8978	40.8978	131.96	2	PROCESSED	57601.597025463	2016-08-01 14:19:43	55652	2011-04-01 00:00:00	55697.1427083333	2011-05-16 03:25:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066001	Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	6	AO6-KP	NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506059010/	Quick Look
225	KEPLER_BG_GN	261.9141	-20.2308	261.17196	-20.189852	262.396131	2.997058	5.199252	8.09662946	270.3619	55105.4689699074	2009-10-01 11:15:19	55107.4279976852	2009-10-03 10:16:19	504103010	68.6043	60	68.6043	68.6043	0	68.6123	2	2	0	2	1	0	0	55.8014	55.8014	169.2279	1	PROCESSED	57548.7547800926	2016-06-09 18:06:53	54922	2009-04-01 00:00:00	55125.6331828704	2009-10-21 15:11:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046004	The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	4	AO4	A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504103010/	Quick Look
226	ABELL 426 SE1	50.1688	41.3334	49.341889	41.153578	58.72404	22.121633	150.81714435	-13.31934713	89.5646	55797.4683912037	2011-08-24 11:14:29	55797.7113194444	2011-08-24 17:04:18	806111010	10.8099	10	10.8099	10.8099	0	10.8099	1	1	0	1	1	0	0	10.3733	10.3733	20.9879	0	PROCESSED	57602.9312268518	2016-08-02 22:20:58	55652	2011-04-01 00:00:00	55855.1291550926	2011-10-21 03:05:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806111010/	Quick Look
227	ABELL 426 NNE2.5	50.1251	42.1872	49.292647	42.007206	58.945293	22.951312	150.30450115	-12.62617945	60.4949	55804.3102083333	2011-08-31 07:26:42	55804.5820833333	2011-08-31 13:58:12	806137010	10.5444	10	10.5444	10.5444	0	10.5444	2	2	0	2	1	0	0	9.962	9.962	23.4721	0	PROCESSED	57603.0188773148	2016-08-03 00:27:11	55652	2011-04-01 00:00:00	55830.2163888889	2011-09-26 05:11:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806137010/	Quick Look
228	ABELL 426 NNE5.5	50.3796	43.0058	49.54083	42.82674	59.388281	23.686025	150.00098645	-11.84054635	60.4963	55806.8935300926	2011-09-02 21:26:41	55807.3024074074	2011-09-03 07:15:28	806143010	16.4506	15	16.4727	16.4666	0	16.4506	1	1	0	1	1	0	0	11.6975	11.6975	35.3199	1	PROCESSED	57603.0430208333	2016-08-03 01:01:57	55652	2011-04-01 00:00:00	55845.2820486111	2011-10-11 06:46:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806143010/	Quick Look
229	ABELL 426 SE2	50.4145	41.1258	49.588274	40.946892	58.854329	21.871316	151.09363465	-13.389164	89.5623	55797.7118402778	2011-08-24 17:05:03	55797.9342824074	2011-08-24 22:25:22	806112010	10.8343	10	10.8383	10.8343	0	10.8423	2	2	0	2	1	0	0	10.6496	10.6496	19.21	0	PROCESSED	57602.9407175926	2016-08-02 22:34:38	55652	2011-04-01 00:00:00	55855.1191782407	2011-10-21 02:51:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806112010/	Quick Look
230	A2199 OFFSET12	246.9232	39.9293	246.496885	40.039337	232.503258	60.398142	63.45171294	43.88430519	267.9996	55820.7013657407	2011-09-16 16:49:58	55821.2488078704	2011-09-17 05:58:17	806158010	23.5902	20	23.5902	23.5902	0	23.5902	2	2	0	2	1	0	0	22.1544	22.1544	47.2919	0	PROCESSED	57603.1801851852	2016-08-03 04:19:28	55652	2011-04-01 00:00:00	55865.2446412037	2011-10-31 05:52:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066024	Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	AURORA SIMIONESCU	JAP	6	AO6-KP	DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806158010/	Quick Look
231	ABELL 426 S3	49.7347	40.7118	48.913	40.530382	58.200048	21.614452	150.88956259	-14.01841244	87.9998	55425.5951273148	2010-08-17 14:16:59	55425.804375	2010-08-17 19:18:18	805098010	11.0308	10	11.0548	11.0468	0	11.0308	1	1	0	1	1	0	0	7.7896	7.7896	18.0719	0	PROCESSED	57553.1040162037	2016-06-14 02:29:47	55287	2010-04-01 00:00:00	55439.0928935185	2010-08-31 02:13:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805098010/	Quick Look
232	G348.5+0.1	258.6301	-38.5295	257.772536	-38.472556	260.783274	-15.450832	348.44223752	0.09652262	91.401	55247.6321180556	2010-02-20 15:10:15	55248.7592476852	2010-02-21 18:13:19	504097010	53.8106	50	53.8106	53.8106	0	53.8106	2	2	0	2	1	0	0	46.3929	46.3929	97.3598	1	PROCESSED	57550.6723842593	2016-06-11 16:08:14	54922	2009-04-01 00:00:00	55257.0343287037	2010-03-02 00:49:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	4	AO4	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504097010/	Quick Look
233	GALACTIC_BULGE18	269.3126	-34.5716	268.480017	-34.566233	269.41346	-11.131891	356.40349802	-4.99577293	70.9023	55633.4308101852	2011-03-13 10:20:22	55634.5273263889	2011-03-14 12:39:21	505087010	51.4284	50	51.4684	51.4284	0	51.4755	1	1	0	1	1	0	0	44.2072	44.2072	94.7279	1	PROCESSED	57601.1565046296	2016-08-01 03:45:22	55287	2010-04-01 00:00:00	55649.0417824074	2011-03-29 01:00:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056001	We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505087010/	Quick Look
234	ABELL 426 SE6.5	51.5164	40.175	50.693426	40.000231	59.444153	20.730657	152.35568667	-13.7013792	87.5613	55800.1546990741	2011-08-27 03:42:46	55800.3765856482	2011-08-27 09:02:17	806121010	10.1899	10	10.1979	10.1899	0	10.2055	1	1	0	1	1	0	0	7.353	7.353	19.1679	0	PROCESSED	57602.9755324074	2016-08-02 23:24:46	55652	2011-04-01 00:00:00	55865.0897569444	2011-10-31 02:09:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806121010/	Quick Look
235	VIRGO S8	187.5886	9.916	186.954186	10.192142	182.977842	12.105979	285.82444468	72.08390522	307.999	56113.4301041667	2012-07-05 10:19:21	56113.7523148148	2012-07-05 18:03:20	807122010	16.053	13	16.053	16.053	0	16.053	1	1	0	1	1	0	0	15.15	15.15	27.8319	1	PROCESSED	57606.5675578704	2016-08-06 13:37:17	56018	2012-04-01 00:00:00	56226.5896296296	2012-10-26 14:09:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807122010/	Quick Look
236	ABELL 426 W6	47.7251	41.6255	46.903246	41.436792	56.912386	22.919663	149.06845077	-14.06119334	94.0002	55430.3630324074	2010-08-22 08:42:46	55430.696724537	2010-08-22 16:43:17	805108010	15.3996	15	15.4076	15.3996	0	15.4076	1	1	0	1	1	0	0	13.6106	13.6106	28.8239	0	PROCESSED	57553.1647569444	2016-06-14 03:57:15	55287	2010-04-01 00:00:00	55446.1712384259	2010-09-07 04:06:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805108010/	Quick Look
237	ABELL 426 SE4	50.9063	40.7039	50.081498	40.526831	59.116004	21.364386	151.65332772	-13.52999243	89.5612	55798.708912037	2011-08-25 17:00:50	55798.9210300926	2011-08-25 22:06:17	806116010	10.8357	10	10.8406	10.8446	0	10.8357	2	2	0	2	1	0	0	10.8394	10.8394	18.32	0	PROCESSED	57602.9537615741	2016-08-02 22:53:25	55652	2011-04-01 00:00:00	55855.1658449074	2011-10-21 03:58:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	6	AO6-KP	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806116010/	Quick Look
238	ABELL 426 S7.5	49.4444	39.4701	48.631245	39.287629	57.603638	20.482404	151.40364882	-15.177571	87.9989	55428.0734375	2010-08-20 01:45:45	55428.5321180556	2010-08-20 12:46:15	805113010	14.87	15	14.87	14.87	0	14.87	2	2	0	2	1	0	0	13.0723	13.0723	39.628	0	PROCESSED	57553.1466898148	2016-06-14 03:31:14	55287	2010-04-01 00:00:00	55439.2152546296	2010-08-31 05:09:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056005	We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	5	AO5	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805113010/	Quick Look
239	GRXE_E_9	268.0849	-26.1545	267.307554	-26.143306	268.269555	-2.725006	3.15134991	0.15632851	103.0998	56385.8984490741	2013-04-03 21:33:46	56388.2085648148	2013-04-06 05:00:20	507074010	98.6516	100	98.6596	98.6596	0	98.6516	2	2	0	2	1	0	0	83.0269	83.0269	199.5757	2	PROCESSED	57611.012650463	2016-08-11 00:18:13	56018	2012-04-01 00:00:00	56401.6405092593	2013-04-19 15:22:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076002	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	7	AO7	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507074010/	Quick Look
240	GRXE_E_7	268.3325	-26.1696	267.555037	-26.159608	268.492207	-2.737339	3.2513581	-0.04270444	86.7249	56716.5321296296	2014-02-28 12:46:16	56718.7084953704	2014-03-02 17:00:14	508076010	102.6848	100	102.6978	102.6868	0	102.6848	2	2	0	2	1	0	0	96.4539	96.4539	188.0198	3	PROCESSED	57613.9520486111	2016-08-13 22:50:57	56383	2013-04-01 00:00:00	56727.7217013889	2014-03-11 17:19:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	086001	We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	8	AO8	ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508076010/	Quick Look
241	VIRGO S18	187.3413	6.4206	186.704552	6.696898	184.175793	8.806296	287.72310531	68.63810092	122.5021	56272.526400463	2012-12-11 12:38:01	56272.9307175926	2012-12-11 22:20:14	807132010	19.8676	18	19.8756	19.8676	0	19.8836	2	2	0	2	1	0	0	18.8251	18.8251	34.9319	0	PROCESSED	57608.2443055556	2016-08-08 05:51:48	56018	2012-04-01 00:00:00	56291.7121296296	2012-12-30 17:05:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	076004	We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	7	AO7	WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807132010/	Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE SUBSTRING(proposal_id,3,1) = '6'

Your request has been accepted.
The download will start soon automatically.

Go to top of this page ⏏