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 858

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	ABELL 773	139.3092	51.8461	138.434684	52.055757	124.471508	34.139728	165.95348434	43.2527698	276.9988	55684.9096412037	2011-05-03 21:49:53	55685.7363541667	2011-05-04 17:40:21	806027040	49.8691	50	49.8805	49.8771	0	49.8691	2	2	0	2	1	0	0	44.1285	44.1285	71.422	1	PROCESSED	57601.942962963	2016-08-01 22:37:52	55652	2011-04-01 00:00:00	55697.3061458333	2011-05-16 07:20:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806027040/	Quick Look
2	COMA CLUSTER OFFSET	194.6939	27.9466	194.090146	28.216217	181.281218	31.269541	60.06105128	88.1791818	318.0815	53885.0996412037	2006-05-30 02:23:29	53886.8384722222	2006-05-31 20:07:24	801044010	79.172	80	79.172	79.172	79.172	79.172	2	2	2	2	1	0	0	75.2282	75.2282	150.2049	2	PROCESSED	57534.5195949074	2016-05-26 12:28:13	54394	2007-10-21 00:00:00	53926.7587384259	2006-07-10 18:12:35	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010091	In order to determine the distribution of O of the intracluster medium of the Coma cluster, we propose to observe the central region with a 40ks exposure and the offset region with a 80ks exposure. The most important in studying the history of nucleosynthesis by SN II is the O mass in the intracluster medium. Especially, the hot cluster contains most of the metals synthesized in the past.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	1	AO1	THE DETERMINATION OF O ABUNDANCE OF THE INTRACLUSTER MEDIUM OF THE COMA CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801044010/	Quick Look
3	HYDRA A-2	139.672	-11.9467	139.069416	-11.735403	146.240414	-26.215979	242.89463155	25.29884455	94.9986	55509.1804861111	2010-11-09 04:19:54	55510.3008680556	2010-11-10 07:13:15	805008010	41.8231	40	41.8311	41.8231	0	41.8311	2	2	0	2	1	0	0	34.5896	34.5896	96.7898	2	PROCESSED	57554.050162037	2016-06-15 01:12:14	55890	2011-11-25 00:00:00	55524.1344791667	2010-11-24 03:13:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050012	X-ray observations of cluster outskirts give us valuable information about star-formation and metal-enrichment histories in clusters. Here, we propose surveys of two regular clusters of galaxies, Hydra A cluster	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KYOKO MATSUSHITA		JAP	5	AO5	DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM UP TO 0.7R180	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805008010/	Quick Look
4	COMA SUBHALO2	194.5069	27.3689	193.901795	27.638743	181.411119	30.679028	42.63932899	88.51577103	315.0001	56452.5504976852	2013-06-09 13:12:43	56453.0265046296	2013-06-10 00:38:10	808020010	21.1563	20	21.1563	21.1563	0	21.1563	1	1	0	1	1	0	0	17.608	17.608	41.1199	1	PROCESSED	57611.5058564815	2016-08-11 12:08:26	56872	2014-08-03 00:00:00	56506.7547222222	2013-08-02 18:06:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080023	We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NOBUHIRO OKABE		JAP	8	AO8	SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808020010/	Quick Look
5	A3376 NORTH	90.6541	-39.7108	90.244762	-39.708634	91.122885	-63.149983	246.26196714	-25.85404299	80.8001	56553.3109143518	2013-09-18 07:27:43	56554.8453935185	2013-09-19 20:17:22	808029010	57.6912	57	57.6912	57.6992	0	57.7072	2	2	0	2	1	0	0	50.8185	50.8185	132.57	0	PROCESSED	57612.703275463	2016-08-12 16:52:43	56956	2014-10-26 00:00:00	56588.7436689815	2013-10-23 17:50:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080037	Abell 3376 (z=0.046) is a peculiar merging cluster with giant double radio relics. High sensitivity of the XIS will enable us (i) to determine the temperature and density distributions around the shock accompanying the east relic, and (ii) to examine how thermal and non-thermal energies separate and go into the respective particles. Wide coverage will allow us to compare the ICM properties along the shock and non-shock directions. The low redshift of the source will allow XIS data to resolve detailed shock-related structures.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKAYA OHASHI		JAP	8	AO8	SUZAKU OBSERVATION OF THE EAST MERGER SHOCK AND RADIO RELIC IN ABELL 3376	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808029010/	Quick Look
6	A1689-OFFSET3	197.7048	-1.4241	197.062246	-1.158416	196.866357	5.631394	312.98436439	61.06880263	289.9992	54672.423599537	2008-07-25 10:09:59	54673.474525463	2008-07-26 11:23:19	803026010	44.0942	40	44.0942	44.0942	0	44.0942	2	2	0	2	1	0	0	37.7063	37.7063	90.7878	1	PROCESSED	57543.149537037	2016-06-04 03:35:20	55076	2009-09-02 00:00:00	54707.1173263889	2008-08-29 02:48:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030100	We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NOBUHIRO OKABE		JAP	3	AO3	UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803026010/	Quick Look
7	NGC 5044 OFFSET1	198.8505	-16.143	198.184446	-15.87899	203.499232	-7.562902	311.28196707	46.33985641	290.0004	53919.3604398148	2006-07-03 08:39:02	53920.9599305556	2006-07-04 23:02:18	801047010	54.6204	60	54.6204	54.6204	54.6204	54.6204	2	2	2	2	1	0	0	45.8033	45.8033	138.1899	1	PROCESSED	57534.8941203704	2016-05-26 21:27:32	54394	2007-10-21 00:00:00	53942.4615740741	2006-07-26 11:04:40	3.0.22.43	6	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010092	We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	1	AO1	THE METAL DISTRIBUTION OF THE NGC 5044 GROUP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801047010/	Quick Look
8	ABELL1835 OFFSET2	210.2863	2.6798	209.652404	2.920968	207.209815	14.079845	340.21334307	60.40388756	306.816	55384.1224884259	2010-07-07 02:56:23	55385.4667939815	2010-07-08 11:12:11	805038010	45.6036	50	45.6036	45.6276	0	45.6116	2	2	0	2	1	0	0	41.2826	41.2826	116.1298	0	PROCESSED	57552.5623611111	2016-06-13 13:29:48	55801	2011-08-28 00:00:00	55434.3364930556	2010-08-26 08:04:33	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050040	We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	NOBUHIRO OKABE		JAP	5	AO5	UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805038010/	Quick Look
9	NGC 253	11.9272	-25.3509	11.313264	-25.623648	0.061683	-27.85028	97.52826827	-88.03578801	242.9951	56643.3716203704	2013-12-17 08:55:08	56645.502962963	2013-12-19 12:04:16	808053010	99.6864	100	99.6864	99.6864	0	99.6864	2	2	0	2	1	0	0	98.5642	98.5642	184.1038	0	PROCESSED	57613.6331481482	2016-08-13 15:11:44	57031	2015-01-09 00:00:00	56664.7662962963	2014-01-07 18:23:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080070	We propose the observation of edge-on starburst galaxies NGC253 and NGC 2146 for 150 ks and 100 ks, respectively. One of the mechanisms that promote the chemical evolution of the universe, starburst outflows have been studied from both aspects of multi-wavelength observations and theory so far. Suzaku original attempts focusing on the abundance patterns has given new insights for a starburst-driven outflow scenario. In AO8, we try to extract the abundance pattern from the south region in NGC 253 and the central region in NGC 2146.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TOSHIKI SATO		JAP	8	AO8	OBSERVATION OF EDGE-ON STARBURST GALAXIES NGC 253 & NGC 2146	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808053010/	Quick Look
10	A2163SE	244.1024	-6.3096	243.434314	-6.186546	243.31547	14.764116	6.72311865	30.24259241	94.6291	57074.4179282407	2015-02-21 10:01:49	57075.8002662037	2015-02-22 19:12:23	809009010	43.2945	50	43.2945	51.0623	0	51.0943	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6399421296	2016-08-17 15:21:31	57453	2016-03-06 00:00:00	57087.4694212963	2015-03-06 11:15:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090032	Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	9	AO9	SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809009010/	Quick Look
11	RBS1066	181.3063	39.3578	180.66961	39.636099	163.015077	36.071469	158.19944471	74.44309108	133.5252	56973.6795486111	2014-11-12 16:18:33	56973.8890277778	2014-11-12 21:20:12	809105010	10.2376	12	10.2376	10.5256	0	10.5256	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7665509259	2016-08-16 18:23:50	57358	2015-12-02 00:00:00	56992.4200810185	2014-12-01 10:04:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809105010/	Quick Look
12	M82 N2	148.2738	70.273	147.216273	70.508377	118.122269	52.466944	140.95732372	40.02876632	282.8972	57162.9827546296	2015-05-20 23:35:10	57164.434224537	2015-05-22 10:25:17	810043010	59.8084	60	59.8084	61.9021	0	61.9021	2	2	0	2	0	0	0	0	0	34.13	0	PROCESSED	57618.7218287037	2016-08-18 17:19:26	57548	2016-06-09 00:00:00	57177.3762847222	2015-06-04 09:01:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101442	We propose to carry out Suzaku observations of the starburst galaxy M82. We will search for X-ray emission from winds and shock heated clouds out to its possible outer boundary of ~45 kpc. We will also constrain the density and temperature profiles of the gas/wind emission out to large radii. These data can place important constraints on theoretical models of starburst galaxies and their environments. We will test models such as the Chevalier & Clegg adiabatic wind model, shocked clouds in a wind, etc. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	10	AO10	SEARCH FOR THE OUTER BOUNDARY OF THE STARBURST GALAXY: M82	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/810043010/	Quick Look
13	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
14	A1914_OFFSET4	216.4138	37.6152	215.900162	37.839927	196.47734	48.33006	66.75628519	67.60183749	330.9949	55365.2958333333	2010-06-18 07:06:00	55366.115462963	2010-06-19 02:46:16	805094010	27.2904	40	27.2904	27.3001	0	27.2944	2	2	0	2	1	0	0	25.4203	25.4203	70.816	0	PROCESSED	57552.407037037	2016-06-13 09:46:08	55769	2011-07-27 00:00:00	55403.4672106482	2010-07-26 11:12:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	053087	We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA	ERIC MILLER	JUS	5	AO5	THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805094010/	Quick Look
15	A1831	209.8007	27.9693	209.233208	28.211522	195.74505	37.218341	40.05378223	74.96810077	288.1207	53937.1181828704	2006-07-21 02:50:11	53937.5106481482	2006-07-21 12:15:20	801077010	18.0796	18	18.0796	18.0796	18.0796	18.0796	2	2	2	2	1	0	0	17.0891	17.0891	33.8979	1	PROCESSED	57535.0011805556	2016-05-27 00:01:42	54401	2007-10-28 00:00:00	53943.553599537	2006-07-27 13:17:11	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801077010/	Quick Look
16	A1750S	202.5548	-2.1063	201.910476	-1.848597	201.643103	6.819901	322.18359807	59.30814244	293.521	55751.0328009259	2011-07-09 00:47:14	55753.0002314815	2011-07-11 00:00:20	806097010	80.1668	80	80.1668	80.1668	0	80.1668	2	2	0	2	1	0	0	67.0448	67.0448	169.9618	3	PROCESSED	57602.5725578704	2016-08-02 13:44:29	56148	2012-08-09 00:00:00	55778.4321412037	2011-08-05 10:22:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	063019	We observe Abell 1750 which has three clusters of galaxies in a filamentary structure of the large-scale structure, with 4 pointing observations (80 x 3 + 40 ks). We reveal global spatial structures of temperature, density, and entropy in Abell 1750 for the first time. By a correlation with a galaxy map obtained from SDSS, and a comparison between thermal pressure and total pressure required by the total mass derived from weal lensing analysis, we explore the inflow of matter and evolutionary process in this system.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA	SCOTT RANDALL	JUS	6	AO6	SUZAKU OBSERVATION OF ABELL 1750 IN THE LARGE-SCALE STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806097010/	Quick Look
17	A1914_OFFSET1	216.5507	38.0175	216.039339	38.24183	196.32687	48.734523	67.63121502	67.35438204	324.9943	55362.5248148148	2010-06-15 12:35:44	55363.4724768518	2010-06-16 11:20:22	805091010	32.2034	40	32.2034	32.2034	0	32.2034	2	2	0	2	1	0	0	27.5086	27.5086	81.876	1	PROCESSED	57552.3572569445	2016-06-13 08:34:27	55766	2011-07-24 00:00:00	55399.2609722222	2010-07-22 06:15:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	053087	We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA	ERIC MILLER	JUS	5	AO5	THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805091010/	Quick Look
18	1RXJ0603	90.7832	42.2686	89.889602	42.270241	90.61448	18.829705	170.16927881	9.72454424	80.0992	56207.7131828704	2012-10-07 17:06:59	56210.6307986111	2012-10-10 15:08:21	807001010	124.3416	120	124.3511	124.3439	0	124.3416	2	2	0	2	1	0	0	125.1948	125.1948	252.0559	1	PROCESSED	57607.7803009259	2016-08-07 18:43:38	56595	2013-10-30 00:00:00	56226.6645717593	2012-10-26 15:56:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070025	We propose to 120 ks + 30 ks (background) Suzaku observations of a new cluster scale shock front candiate in merger cluster of galaxies 1RXJ0603. 1RXJ0603 has irregular shape radio relic with remarkable steep radio spectrum index, which indicate the existence of shock fronts with mach number M ~ 4.5. The temperature and density of Intra ClusterMedium across radio relics will provide the nature of shock front. Our study will shed new light on the origin of the cluster scale shock fronts.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	HIROKI AKAMATSU		JAP	7	AO7	SUZAKU OBSERVATION OF A NEW CLUSTER SCALE SHOCK FRONT CANDIATE IN MERGING CLUSTER OF GALAXIES 1RXJ0603	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807001010/	Quick Look
19	A1674	195.9676	67.5471	195.510877	67.814977	143.551001	62.83408	121.10331631	49.53698634	114.9985	54085.1434837963	2006-12-16 03:26:37	54087.0426388889	2006-12-18 01:01:24	801062010	68.4138	100	68.4218	68.4218	0	68.4138	2	2	0	2	1	0	0	109.0131	109.0131	164.064	2	PROCESSED	57536.3777546296	2016-05-28 09:03:58	54750	2008-10-11 00:00:00	54094.6003935185	2006-12-25 14:24:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010156	A1674 is a nearby (z=0.106) richness class 3 clsuter with Abell galaxy count of 165, while its X-ray luminsity is as low as 6e43erg/s. We have observed this cluster with ASCA and XMM-Newton, and found iregular extended X-ray emission. The X-ray spectrum can be fitted with a thin thermal model of kT ~ 3keV, but the metal abundance is 0.07 with upper limit of 0.2. We assume this cluster may be a cluster under construction. Utilizing the low background level and high sensitivity of Suzaku XIS, we aim to obtain accurate X-ray spectrum of this cluster to constrain the metal abndance of each species. We also examine possible contribution of diffuse non-thermal emission in cluster scale.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KIYOSHI HAYASHIDA		JAP	1	AO1	METAL DEFICIENT GAS OR NON THERMAL EMISSION? DIFFUSE X-RAYS IN A1674	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801062010/	Quick Look
20	FORNAX A W-LOBE W	50.2219	-37.0341	49.742698	-37.213173	32.331063	-52.814253	239.92107074	-57.06786371	27.0759	54990.6810763889	2009-06-08 16:20:45	54991.75375	2009-06-09 18:05:24	804036010	60.3625	50	60.3625	60.3625	0	60.3625	2	2	0	2	1	0	0	56.3965	56.3965	92.6519	1	PROCESSED	57547.532974537	2016-06-08 12:47:29	55367	2010-06-20 00:00:00	55001.0562615741	2009-06-19 01:21:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040073	We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MAKOTO TASHIRO		JAP	4	AO4	X-RAY MAPPING OF THE FORNAX A WEST LOBE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804036010/	Quick Look
21	COMA_45OFF	194.2558	27.5714	193.650381	27.84154	181.073902	30.760176	52.91406039	88.6829823	127.9482	54436.4228703704	2007-12-02 10:08:56	54437.2085185185	2007-12-03 05:00:16	802047010	31.6151	30	31.6151	31.6151	0	31.6151	2	2	0	2	1	0	0	26.1691	26.1691	67.824	0	PROCESSED	57540.7702083333	2016-06-01 18:29:06	54814	2008-12-14 00:00:00	54445.1600925926	2007-12-11 03:50:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020149	With XIS and HXD onboard Suzaku, we propose a scanning observation along the large-scale filament structure connecting the Coma cluster outskirts and the radio relic 1253+275. The scientific aims are: 1) to verify and delineate the spatial extent of the hard X-ray excess reported by BeppoSAX and RXTE, 2) to constrain the spatial distribution of large-scale magnetic fields, 3) to probe nonthermal processes associated with structure formation, such as ultra-high-energy particle acceleration at the cluster accretion shock, and 4) to provide complementary data in connection with observations in other wavebands, especially GeV-TeV gamma-rays.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	SUSUMU INOUE		JAP	2	AO2	EXPLORING PARTICLE ACCELERATION AND MAGNETIC FIELDS IN A LARGE-SCALE FILAMENT STRUCTURE ASSOCIATED WITH THE COMA CLUSTER	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802047010/	Quick Look
22	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
23	A1800	207.3618	28.0973	206.789109	28.345144	193.256107	36.394356	40.59651819	77.12066844	302.3644	53936.635625	2006-07-20 15:15:18	53937.1140509259	2006-07-21 02:44:14	801078010	20.0437	17	20.0473	20.0553	20.0553	20.0437	2	2	2	2	1	0	0	19.0003	19.0003	41.3319	0	PROCESSED	57535.0036458333	2016-05-27 00:05:15	54401	2007-10-28 00:00:00	53943.5299652778	2006-07-27 12:43:09	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801078010/	Quick Look
24	AWM7 NW2	42.4678	42.1132	41.659195	41.906559	53.004907	24.584739	145.29354682	-15.55850289	257.0018	56705.8674421296	2014-02-17 20:49:07	56706.6667824074	2014-02-18 16:00:10	808024010	35.333	35	35.341	35.333	0	35.349	2	2	0	2	1	0	0	30.0596	30.0596	69.0559	0	PROCESSED	57613.8687268518	2016-08-13 20:50:58	57130	2015-04-18 00:00:00	56764.8062847222	2014-04-17 19:21:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080034	We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	8	AO8	METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808024010/	Quick Look
25	URSA MINOR	227.2517	67.2307	227.099638	67.419875	158.023499	73.538029	104.9865755	44.80382561	40.7921	54195.7731944444	2007-04-05 18:33:24	54196.7557175926	2007-04-06 18:08:14	802052010	70.8823	67	70.8903	70.8823	0	70.8903	2	2	0	2	1	0	0	59.5872	59.5872	84.876	1	PROCESSED	57538.0737731482	2016-05-30 01:46:14	54695	2008-08-17 00:00:00	54203.3200462963	2007-04-13 07:40:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021405	We propose 50 ksec Suzaku observations of the Ursa Minor and Draco dwarf spheroidal galaxies. These dense, dark-matter-dominated systems are carefully selected as the strongest potential sources of line emission from radiatively decaying keV dark matter of any astrophysical object. The low-level, stable Suzaku background makes it the most sensitive instrument to-date for this purpose. At the very least, constraints that enter a significant new regime are derived: non-detections are still of great importance. In the best case, the long sought-after identity of dark matter will be discovered, pointing the way to physics beyond the Standard Model.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MICHAEL LOEWENSTEIN		USA	2	AO2	SEARCH FOR WARM DARK MATTER WITH SUZAKU OBSERVATIONS OF DWARF SPHEROIDAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802052010/	Quick Look
26	BOOTES GROUP 1	218.7136	35.7235	218.197903	35.941461	200.235171	47.529275	60.71261374	66.41229506	153.2269	54440.1222106482	2007-12-06 02:55:59	54441.2015972222	2007-12-07 04:50:18	802054010	42.2242	38	42.2242	42.2242	0	42.2242	2	2	0	2	1	0	0	41.3023	41.3023	93.254	0	PROCESSED	57540.8293518518	2016-06-01 19:54:16	54815	2008-12-15 00:00:00	54448.2273842593	2007-12-14 05:27:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021424	We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MARSHALL BAUTZ		USA	2	AO2	SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802054010/	Quick Look
27	ABELL2244	255.6885	34.0502	255.230084	34.120069	248.255538	56.413781	56.77689495	36.30222985	232.8204	54392.7992013889	2007-10-19 19:10:51	54394.3959953704	2007-10-21 09:30:14	802078010	71.3811	63	71.3891	71.3971	0	71.3811	2	2	0	2	1	0	0	69.1077	69.1077	137.9498	3	PROCESSED	57540.332337963	2016-06-01 07:58:34	54771	2008-11-01 00:00:00	54403.2516666667	2007-10-30 06:02:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022036	In order to use clusters as cosmological probes, accurate mass determinations are needed. The ICM is an ideal candidate since it provides a map of the DM potential. Measuring the gas properties to the virial radius is imperative for determining the proper cluster mass, since a large part of the cluster mass resides beyond 1/2 r_vir. Current discrepancies in outer cluster kT profiles are due to large uncertainties due to the high background in Chandra and XMM-Newton. With its lower background, Suzaku is able to make this measurement. We propose a 50 ks observation of A2244. A2244 is an ideal candidate to make this measurement; at a redshift of z~0.1, the virial radius can be fit inside Suzaku's field of view, moreover A2244 is an unusual example of a relaxed cluster without a cool core.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DANIEL HUDSON		EUR	2	AO2	A2244 - MEASURING CLUSTER GAS TEMPERATURE TO THE VIRIAL RADIUS IN A RELAXED ISOTHERMAL CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802078010/	Quick Look
28	A2665	357.7161	6.1352	357.076736	5.857083	0.350497	6.536022	96.94047732	-53.65177278	245.9817	54078.2252893518	2006-12-09 05:24:25	54078.562037037	2006-12-09 13:29:20	801076010	13.944	15	13.944	13.944	0	13.944	2	2	0	2	1	0	0	11.6073	11.6073	29.0879	0	PROCESSED	57536.2715393518	2016-05-28 06:31:01	54695	2008-08-17 00:00:00	54089.271412037	2006-12-20 06:30:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801076010/	Quick Look
29	FJ1	238.114	22.5674	237.571568	22.715547	229.271734	41.603316	36.86878642	48.89749971	115.0005	56698.0557638889	2014-02-10 01:20:18	56701.0001851852	2014-02-13 00:00:16	808041010	111.8457	100	111.8537	111.8457	0	111.8537	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57613.8229166667	2016-08-13 19:45:00	57130	2015-04-18 00:00:00	56765.6012152778	2014-04-18 14:25:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080054	Filament Junctions are known to be the most active regions in structure formation in the Universe. These regions can be identified using our original method based on galaxy distribution. In AO8, we try to detect (1) a galaxy-scale halo with a radio relic structure often observed after merger and (2) a galaxy-scale halo just before merger at the Filament Junction.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	IKUYUKI MITSUISHI		JAP	8	AO8	EXPLORING EVOLUTION OF GROUPS AT FILAMENT JUNCTIONS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808041010/	Quick Look
30	A1689-OFFSET4	197.7965	-1.1735	197.154302	-0.90795	196.855647	5.897997	313.25406527	61.301843	290	54673.475	2008-07-26 11:24:00	54674.5091898148	2008-07-27 12:13:14	803027010	42.0199	40	42.0279	42.0279	0	42.0199	2	2	0	2	1	0	0	36.8505	36.8505	89.354	2	PROCESSED	57543.1496527778	2016-06-04 03:35:30	55076	2009-09-02 00:00:00	54707.0673032407	2008-08-29 01:36:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030100	We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NOBUHIRO OKABE		JAP	3	AO3	UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803027010/	Quick Look
31	A3112	49.3542	-44.4494	48.920816	-44.631605	25.154749	-59.092558	253.34888003	-56.10584592	209.0003	57003.8439467593	2014-12-12 20:15:17	57006.6182407407	2014-12-15 14:50:16	809116020	97.989	200	97.989	97.989	0	97.989	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.5061458333	2016-08-17 12:08:51	57387	2015-12-31 00:00:00	57017.4238425926	2014-12-26 10:10:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	094527	The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ESRA BULBUL		USJ	9	AO9	A DETAILED STUDY OF CHEMICAL ENRICHMENT OF A3112 OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809116020/	Quick Look
32	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
33	FILAMENT OF GALAXIES	238.2847	27.6247	237.767937	27.772087	227.420415	46.484967	44.49442625	49.89393343	305.997	55408.8620833333	2010-07-31 20:41:24	55410.6883101852	2010-08-02 16:31:10	805030010	61.7703	80	61.7703	61.7703	0	61.7703	2	2	0	2	1	0	0	55.5833	55.5833	157.7518	0	PROCESSED	57552.8205671296	2016-06-13 19:41:37	55793	2011-08-20 00:00:00	55427.2133449074	2010-08-19 05:07:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050032	Warm Hot Intergalactic Medium (WHIM) is the most promising candidate for the cosmic missing baryons. Nevertheless, no concrete evidence of the presence of the WHIM has been unveiled yet. We propose a SUZAKU observation of a filament discovered through a systematic analysis of the SDSS galaxy catalogue. The observation toward a 10 Mpc long section of this filament aligned with the line of sight will provide the redshifted OVII and OVIII emission lines from the WHIM or much stronger constraint on the overdensity of the WHIM.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	HAJIME KAWAHARA		JAP	5	AO5	SEARCHING FOR MISSING BARYONS ALONG A FILAMENT OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805030010/	Quick Look
34	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
35	CENA LOBE 2	201.7888	-39.7615	201.063878	-39.502282	215.867885	-28.246306	310.35736359	22.59471631	296.9216	56141.4611921296	2012-08-02 11:04:07	56143.2779861111	2012-08-04 06:40:18	807041030	65.8666	65	65.8746	65.8746	0	65.8666	2	2	0	2	1	0	0	57.8659	57.8659	156.9538	2	PROCESSED	57606.7677893518	2016-08-06 18:25:37	56018	2012-04-01 00:00:00	56162.2467013889	2012-08-23 05:55:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070106	Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LUKASZ STAWARZ		JAP	7	AO7	STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807041030/	Quick Look
36	COMA SUBHALO1 S	195.2527	28.7629	194.651674	29.031827	181.36326	32.219878	71.19878606	87.32773157	296.8003	56452.0686458333	2013-06-09 01:38:51	56452.5459490741	2013-06-09 13:06:10	808019010	20.4808	20	20.4888	20.4808	0	20.4968	1	1	0	1	1	0	0	21.4968	21.4968	41.2319	0	PROCESSED	57611.4938541667	2016-08-11 11:51:09	56869	2014-07-31 00:00:00	56503.6109606482	2013-07-30 14:39:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080023	We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NOBUHIRO OKABE		JAP	8	AO8	SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808019010/	Quick Look
37	A3376 SOUTH	90.6172	-40.196	90.211877	-40.194003	91.07062	-63.635447	246.775776	-26.0046965	124.8629	56580.8395486111	2013-10-15 20:08:57	56582.2918055556	2013-10-17 07:00:12	808030010	66.5346	57	66.5347	66.5346	0	66.5346	3	2	0	2	1	0	0	56.9771	56.9771	125.45	1	PROCESSED	57613.0188541667	2016-08-13 00:27:09	57004	2014-12-13 00:00:00	56637.6639351852	2013-12-11 15:56:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080037	Abell 3376 (z=0.046) is a peculiar merging cluster with giant double radio relics. High sensitivity of the XIS will enable us (i) to determine the temperature and density distributions around the shock accompanying the east relic, and (ii) to examine how thermal and non-thermal energies separate and go into the respective particles. Wide coverage will allow us to compare the ICM properties along the shock and non-shock directions. The low redshift of the source will allow XIS data to resolve detailed shock-related structures.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKAYA OHASHI		JAP	8	AO8	SUZAKU OBSERVATION OF THE EAST MERGER SHOCK AND RADIO RELIC IN ABELL 3376	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808030010/	Quick Look
38	ABELL 3571	206.8624	-32.8524	206.14186	-32.603207	216.960537	-20.284209	316.31343933	28.55973438	103.8412	56666.0275	2014-01-09 00:39:36	56666.7772453704	2014-01-09 18:39:14	808094010	38.279	60	38.279	38.279	0	38.279	2	2	0	2	1	0	0	39.0047	39.0047	64.776	0	PROCESSED	57613.7763425926	2016-08-13 18:37:56	57096	2015-03-15 00:00:00	56730.4916435185	2014-03-14 11:47:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081531	Abell 3571 is one of the brightest cluster in the X-ray sky and one of the main clusters in the Shapley supercluster. We have recently found evidence that it may be passing through a violent (~2000 km/s) merger in the line of sight (los). If corroborated it would be the closest template for the systems of this kind allowing us to study and characterize los mergers. We request a short observation of 60 ksec to corroborate the velocity gradients found with Chandra for this cluster, using the improved spectral resolution and gain stability of Suzaku s XISs.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	RENATO DUPKE		USA	8	AO8	ABELL 3571. THE CLOSEST LINE OF SIGHT MERGER?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808094010/	Quick Look
39	A262 E3	29.2513	35.7586	28.51426	35.514871	40.102333	22.236821	137.59731231	-25.23895106	250.0003	56701.0116319444	2014-02-13 00:16:45	56701.8717939815	2014-02-13 20:55:23	808114010	38.5681	40	38.5761	38.5681	0	38.5761	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57613.8129861111	2016-08-13 19:30:42	57080	2015-02-27 00:00:00	56714.7407986111	2014-02-26 17:46:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	083002	We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA	NORBERT WERNER	JUS	8	AO8	OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808114010/	Quick Look
40	A2163BGD1	244.2972	-6.0675	243.630135	-5.945298	243.467732	15.036983	7.08170195	30.23063611	97.9997	57078.1207523148	2015-02-25 02:53:53	57078.9737384259	2015-02-25 23:22:11	809010010	28.6539	30	28.6539	28.6619	0	28.6699	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6666782407	2016-08-17 16:00:01	57454	2016-03-07 00:00:00	57087.4740393518	2015-03-06 11:22:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090032	Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	9	AO9	SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809010010/	Quick Look
41	PKS 2356-61	359.7661	-60.908	359.120501	-61.186478	324.284485	-53.222548	314.02525269	-55.07790138	249.6445	54075.7140740741	2006-12-06 17:08:16	54078.21625	2006-12-09 05:11:24	801016010	100.8372	100	100.8452	100.8372	0	100.8532	2	2	0	2	1	0	0	92.1255	92.1255	216.1579	3	PROCESSED	57536.3143171296	2016-05-28 07:32:37	54456	2007-12-22 00:00:00	54088.6546759259	2006-12-19 15:42:44	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010059	We propose a 100 ksec Suzaku observation of the radio galaxy PKS 2356-61. PKS 2356-61 is reported to reside in a group of galaxies, and a sign of a diffuse X-ray emission with a possibly high temperature surrounding PKS 2356-61 was suggested with ASCA. Our objective is the determination of the origin of the diffuse emission to evaluate AGN heating of the intragroup gas by PKS 2356-61.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	SOOJING HONG		JAP	1	AO1	HIGH TEMPERATURE GROUP OF GALAXIES SURROUNDING THE RADIO GALAXY PKS 2356-61	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801016010/	Quick Look
42	A3376 WEST RELIC	90.0363	-39.9917	89.629297	-39.992531	90.071049	-63.433501	246.43145562	-26.38385089	126.3601	54034.3950231482	2006-10-26 09:28:50	54035.9176388889	2006-10-27 22:01:24	800011020	62.2648	60	62.2648	62.2648	62.2648	62.2648	2	2	2	2	1	0	0	55.5629	55.5629	131.5378	2	PROCESSED	57535.9705902778	2016-05-27 23:17:39	54694	2008-08-16 00:00:00	54090.2671643518	2006-12-21 06:24:43	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001039	We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA		JAP	0	SWG	SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800011020/	Quick Look
43	HYDRA A-1	139.3695	-11.9475	138.767154	-11.737163	145.930071	-26.316597	242.69436566	25.06487811	95	55508.1097569444	2010-11-08 02:38:03	55509.1800115741	2010-11-09 04:19:13	805007010	42.5647	40	42.5727	42.5647	0	42.5727	2	2	0	2	1	0	0	35.2072	35.2072	92.4558	1	PROCESSED	57554.0434143518	2016-06-15 01:02:31	55890	2011-11-25 00:00:00	55524.1752430556	2010-11-24 04:12:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050012	X-ray observations of cluster outskirts give us valuable information about star-formation and metal-enrichment histories in clusters. Here, we propose surveys of two regular clusters of galaxies, Hydra A cluster	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KYOKO MATSUSHITA		JAP	5	AO5	DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM UP TO 0.7R180	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805007010/	Quick Look
44	FILAMENT JUNCTION 3	151.4159	39.7399	150.662748	39.98344	138.765722	26.114357	181.90509124	53.56333781	291.576	55672.3023611111	2011-04-21 07:15:24	55673.6362268518	2011-04-22 15:16:10	806005010	55.0232	60	55.0232	55.0312	0	55.0392	2	2	0	2	1	0	0	49.8669	49.8669	115.2299	2	PROCESSED	57601.5861921296	2016-08-01 14:04:07	56061	2012-05-14 00:00:00	55692.3338425926	2011-05-11 08:00:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060015	Haloes, such as galaxy clusters or groups have been considered to form at intersections of cosmological filaments. Nevertheless, there are a lot of junctions of galaxy filaments without X-ray strong signal from massive clusters. We propose a SUZAKU observation of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey using a new method. The SUZAKU observation of high sensitivity in low energy will reveal nature of faint haloes growing in the large filament junctions.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HAJIME KAWAHARA		JAP	6	AO6	EXPLORING JUNCTIONS OF GALAXY FILAMENTS BY SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806005010/	Quick Look
45	NGC 2300 GROUP	112.8158	85.6965	108.675805	85.795148	93.626997	62.54508	127.72434362	27.79082708	339.9138	55235.7626388889	2010-02-08 18:18:12	55236.5002893518	2010-02-09 12:00:25	804030010	37.0591	100	37.0591	37.0591	0	37.0591	2	2	0	2	1	0	0	34.4534	34.4534	63.7299	1	PROCESSED	57550.5366666667	2016-06-11 12:52:48	55619	2011-02-27 00:00:00	55251.1588310185	2010-02-24 03:48:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040055	We propose to observe the NGC 2300 group for 100 ks and a offset pointing for 200 ks to evaluate the background emission from the Galaxy. The purpose of the observations are to measure O, Mg, Si and Fe abundances of intragaractic medium to study metal synthesis in this small group of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KYOKO MATSUSHITA		JAP	4	AO4	O, MG, S AND FE ABUNDANCES OF INTRAGROUP MEDIUM IN THE NGC 2300 GROUP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804030010/	Quick Look
46	RCS212414-6325.8	321.0509	-63.4275	320.054735	-63.642547	299.532953	-45.130077	330.62476764	-40.84164156	79.2319	55691.4113541667	2011-05-10 09:52:21	55691.979375	2011-05-10 23:30:18	806082010	36.3224	35	36.3304	36.3304	0	36.3224	2	2	0	2	1	0	0	26.914	26.914	49.0679	1	PROCESSED	57602.0065046296	2016-08-02 00:09:22	56068	2012-05-21 00:00:00	55701.1927546296	2011-05-20 04:37:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061533	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AMALIA HICKS		USA	6	AO6	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806082010/	Quick Look
47	ABELL 1795 Far North	207.223	26.9995	206.646903	27.247656	193.71055	35.352954	35.63943573	77.21561208	130.4264	53715.3208796296	2005-12-11 07:42:04	53715.9730092593	2005-12-11 23:21:08	800012030	30.6406	30	30.6486	30.6406	30.6639	30.6566	2	2	2	2	1	0	0	27.8833	27.8833	56.3379	1	PROCESSED	57532.4195833333	2016-05-24 10:04:12	54247	2007-05-27 00:00:00	54039.1003703704	2006-10-31 02:24:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012030/	Quick Look
48	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
49	A133_S	15.6819	-22.1029	15.071421	-22.371383	5.125588	-26.4157	150.58121257	-84.35810156	44.9946	55355.2966203704	2010-06-08 07:07:08	55356.727974537	2010-06-09 17:28:17	805022010	51.128	50	51.128	51.128	0	51.128	2	2	0	2	1	0	0	42.8599	42.8599	123.6558	1	PROCESSED	57551.9312962963	2016-06-12 22:21:04	55737	2011-06-25 00:00:00	55370.2538310185	2010-06-23 06:05:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050019	We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KOSUKE SATO		JAP	5	AO5	METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805022010/	Quick Look
50	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
51	A1914_OFFSET1	216.5784	38.0421	216.067238	38.26635	196.337734	48.766613	67.66951456	67.3249966	134.001	55565.4188194445	2011-01-04 10:03:06	55565.728599537	2011-01-04 17:29:11	805091020	11.393	10	11.401	11.393	0	11.401	2	2	0	2	1	0	0	11.3763	11.3763	25.4979	0	PROCESSED	57600.5573263889	2016-07-31 13:22:33	55995	2012-03-09 00:00:00	55627.1165625	2011-03-07 02:47:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	053087	We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA	RYO NAGINO	JUS	5	AO5	THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805091020/	Quick Look
52	A1914_OFFSET3	216.2252	37.8719	215.712166	38.097165	196.093912	48.482824	67.5271644	67.6467927	330.9949	55364.3811805556	2010-06-17 09:08:54	55365.2953587963	2010-06-18 07:05:19	805093010	28.5066	40	28.5066	28.5066	0	28.5066	2	2	0	2	1	0	0	26.3813	26.3813	78.9679	1	PROCESSED	57552.3531018518	2016-06-13 08:28:28	55769	2011-07-27 00:00:00	55400.3084375	2010-07-23 07:24:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	053087	We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA	ERIC MILLER	JUS	5	AO5	THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805093010/	Quick Look
53	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
54	NGC 5044 OFFSET2	199.1117	-16.388	198.444886	-16.124395	203.827071	-7.694393	311.59229028	46.06278821	290.7836	53920.9609143518	2006-07-04 23:03:43	53922.7598842593	2006-07-06 18:14:14	801048010	62.451	60	62.451	62.451	62.451	62.451	2	2	2	2	1	0	0	57.1102	57.1102	155.3149	2	PROCESSED	57534.8962615741	2016-05-26 21:30:37	54422	2007-11-18 00:00:00	54034.2926736111	2006-10-26 07:01:27	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010092	We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	1	AO1	THE METAL DISTRIBUTION OF THE NGC 5044 GROUP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801048010/	Quick Look
55	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
56	FORNAX OFFSET3	55.0322	-35.1579	54.552305	-35.31846	39.454432	-52.642961	236.21473388	-53.30533318	63.6008	54664.1800810185	2008-07-17 04:19:19	54665.2009143518	2008-07-18 04:49:19	803008010	41.2795	30	41.2875	41.2795	0	41.2955	2	2	0	2	1	0	0	35.0699	35.0699	88.1898	0	PROCESSED	57543.0818055556	2016-06-04 01:57:48	55055	2009-08-12 00:00:00	54689.4341087963	2008-08-11 10:25:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030036	We proposeto observe 5 offset pointings of the Fornax cluster for 160 ks with Suzaku. The purpose of the observation is to determine O, Mg and Fe distribution of the intracluster medium up to 0.15-0.2 r180 and to study the origin of the metals.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	3	AO3	METAL DISTRIBUTION OF THE FORNAX CLUSTER UP TO 0.2R180.	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803008010/	Quick Look
57	PERSEUS OFFSET-F	49.9431	41.79	49.113812	41.609338	58.684902	22.607146	150.41345254	-13.03211324	269.9991	55609.6649305556	2011-02-17 15:57:30	55610.152974537	2011-02-18 03:40:17	805046010	20.7197	25	20.7197	20.7197	0	20.7197	1	1	0	1	1	0	0	18.813	18.813	42.1599	0	PROCESSED	57600.9628125	2016-07-31 23:06:27	55990	2012-03-04 00:00:00	55621.2476967593	2011-03-01 05:56:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050093	We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKAYUKI TAMURA		JAP	5	AO5	MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805046010/	Quick Look
58	A2495	342.5777	10.9124	341.95313	10.647232	348.269753	16.897696	81.20126485	-41.9387619	237.1467	54061.4694097222	2006-11-22 11:15:57	54062.0787037037	2006-11-23 01:53:20	801080010	18.0313	18	18.0313	18.3673	0	18.1193	2	2	0	2	1	0	0	16.3891	16.3891	52.6339	3	PROCESSED	57536.1381365741	2016-05-28 03:18:55	54695	2008-08-17 00:00:00	54088.9563194444	2006-12-19 22:57:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080010/	Quick Look
59	NGC 4382	186.3492	18.1851	185.718232	18.461926	178.313661	19.153245	267.72488674	79.23166289	294.1787	54638.1652199074	2008-06-21 03:57:55	54640.4481944444	2008-06-23 10:45:24	803005010	99.0682	90	99.0682	99.0682	0	99.0682	2	2	0	2	1	0	0	93.4447	93.4447	197.2038	3	PROCESSED	57542.911412037	2016-06-03 21:52:26	55020	2009-07-08 00:00:00	54651.2282291667	2008-07-04 05:28:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030033	We proposeto observe a S0 galaxy, NGC 4382 for 90 ks with Suzaku. The purpose of the observation is to study abundance pattern of O/Ne/Mg/Si/Fe of S0 galaxies and to study history of S0 galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	3	AO3	THE ISM ABUNDANCE OF A S0 GALAXY, NGC 4382	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803005010/	Quick Look
60	FORNAX A W-LOBE S	50.3569	-37.3111	49.879649	-37.489667	32.298971	-53.110795	240.40306132	-56.92864271	79.0007	55065.4424189815	2009-08-22 10:37:05	55066.6731365741	2009-08-23 16:09:19	804038020	45.5693	42	45.5693	45.5693	0	45.5693	3	2	0	2	1	0	0	38.9534	38.9534	106.2599	0	PROCESSED	57548.3175347222	2016-06-09 07:37:15	55444	2010-09-05 00:00:00	55078.0721064815	2009-09-04 01:43:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040073	We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MAKOTO TASHIRO		JAP	4	AO4	X-RAY MAPPING OF THE FORNAX A WEST LOBE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804038020/	Quick Look
61	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
62	FG25	234.9579	30.7058	234.452539	30.866616	221.876556	48.458584	48.772653	53.18955534	294.6599	56136.7541898148	2012-07-28 18:06:02	56137.0821875	2012-07-29 01:58:21	807049010	10.6393	10	10.6393	10.6393	0	10.6393	2	2	0	2	1	0	0	11.074	11.074	28.3281	0	PROCESSED	57606.6807523148	2016-08-06 16:20:17	56527	2013-08-23 00:00:00	56161.2376736111	2012-08-22 05:42:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071511	Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ELENA D'ONGHIA		USA	7	AO7	SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807049010/	Quick Look
63	A 2218 OFFSETB	249.9091	65.2119	249.835523	65.307656	180.044789	81.713752	96.37864193	38.09205953	233.3309	53670.1916319444	2005-10-27 04:35:57	53670.4620833333	2005-10-27 11:05:24	800020010	14.9215	15	14.9375	14.9335	14.9215	14.9415	2	2	2	2	1	0	0	14.1931	14.1931	23.3561	0	PROCESSED	57527.6596180556	2016-05-19 15:49:51	54247	2007-05-27 00:00:00	54036.8343981482	2006-10-28 20:01:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001096	To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI		JAP	0	SWG	SEARCH FOR OXYGEN LINES FROM WARM IGM		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800020010/	Quick Look
64	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
65	THE MOON	131.4647	12.9515	130.775529	13.134573	130.365878	-4.869219	213.82172975	31.16197152	285.4003	56783.5475578704	2014-05-06 13:08:29	56783.6842361111	2014-05-06 16:25:18	809001010	4.6424	45	4.6464	4.6424	0	4.6504	2	2	0	2	1	0	0	4.5647	4.5647	11.806	0	PROCESSED	57615.0366898148	2016-08-15 00:52:50	57162	2015-05-20 00:00:00	56793.5228125	2014-05-16 12:32:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001010/	Quick Look
66	FORNAX A HOST GALAXY	50.6684	-37.2029	50.191244	-37.380302	32.749558	-53.117138	240.15407206	-56.69497357	218.3809	54091.6179976852	2006-12-22 14:49:55	54092.8689699074	2006-12-23 20:51:19	801015010	48.7217	50	48.7217	48.7217	0	48.7217	2	2	0	2	1	0	0	48.3987	48.3987	108.0839	1	PROCESSED	57536.4184837963	2016-05-28 10:02:37	54735	2008-09-26 00:00:00	54132.9200347222	2007-02-01 22:04:51	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010029	We propose Suzaku observations of the Fornax A west radio lobe and the host galaxy. By measuring the inverse-Compton X-ray spectrum from the radio lobe precisely up to 20 keV and comparing with radio observation results, we are able to determine the electron energy spectrum and to derive magnetic field without any assumptions. This will be an important sample to measure the kinetic energy outflow from an active galactic nucleus.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO TASHIRO		JAP	1	AO1	RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801015010/	Quick Look
67	COMA NW5	194.3037	29.1454	193.700799	29.41548	180.283789	32.183117	91.00313756	87.61452721	319.9965	55733.4693865741	2011-06-21 11:15:55	55734.0682407407	2011-06-22 01:38:16	806042010	21.0972	20	21.1201	21.1132	0	21.0972	2	2	0	2	1	0	0	20.4401	20.4401	51.724	0	PROCESSED	57602.3799537037	2016-08-02 09:07:08	55652	2011-04-01 00:00:00	55768.342025463	2011-07-26 08:12:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806042010/	Quick Look
68	COMA SW5.5	193.6448	27.0863	193.037174	27.357142	180.762937	30.083449	29.67661506	89.29968791	314.5983	55735.866400463	2011-06-23 20:47:37	55736.3037037037	2011-06-24 07:17:20	806048010	15.2345	15	15.245	15.2345	0	15.2345	2	2	0	2	1	0	0	16.4375	16.4375	37.776	0	PROCESSED	57602.4025347222	2016-08-02 09:39:39	55652	2011-04-01 00:00:00	55794.9965625	2011-08-21 23:55:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806048010/	Quick Look
69	3C390.3_VICINITY_1	276.9861	79.7253	277.865171	79.689308	84.608267	76.703493	111.37115096	27.70478895	240.0064	56607.4234953704	2013-11-11 10:09:50	56608.4910648148	2013-11-12 11:47:08	808046010	57.71	50	57.71	57.72	0	57.7141	2	2	0	2	1	0	0	52.9408	52.9408	92.2319	1	PROCESSED	57613.2938425926	2016-08-13 07:03:08	56991	2014-11-30 00:00:00	56625.6961458333	2013-11-29 16:42:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080060	We propose for observations of the vicinities of 3C 390.3 and Fairall 9, in order to constrain the origins of 'excess' emission in the soft X-ray diffuse background observed with Suzaku and to confirm its possible relation to high velocity clouds (HVCs). We have been observing blank-skies in many directions and studying a oxygen emission from the Galactic halo. Intensities of the emission show a uniform value in most of directions; however in some directions we can see an excess, which possibly originate to a blob-like high density gas and/or a distribution of HVCs. By conducting a joint analysis of absorption and emission lines, we can characterize the roots of the excess emission. Moreover, the joint analysis even constraints a density of the origins, which has never been done until now.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KAZUHIRO SAKAI		JAP	8	AO8	DO HIGH VELOCITY CLOUDS HEAT THE HALO OF OUR GALAXY?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808046010/	Quick Look
70	BULLET-BKG	105.498	-55.9182	105.253708	-55.844379	132.076188	-77.080913	266.15428465	-20.7753384	287.5121	56422.4617592593	2013-05-10 11:04:56	56424.0029976852	2013-05-12 00:04:19	808057010	51.0907	50	51.0987	51.0907	0	51.1067	2	2	0	2	1	0	0	46.6938	46.6938	133.1496	0	PROCESSED	57611.3081365741	2016-08-11 07:23:43	56799	2014-05-22 00:00:00	56433.6980208333	2013-05-21 16:45:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080080	We propose two offset pointings of the bullet cluster with one adjacent blank-sky pointing. By detecting a very hot component in the ICM and mapping temperature/entropy out to the outskirts, we study thermodynamical evolution of the ICM in the course of cluster merger. More specifically, we estimate the fraction of energy injected to the ICM from the energy released by the merger, and the amount of energy heating the ICM through the shock, irreversible process.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	8	AO8	THERMODYNAMICAL EVOLUTION OF THE ICM IN THE BULLET CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808057010/	Quick Look
71	A262 E4	29.5568	35.6351	28.819272	35.392091	40.300853	22.029449	137.89892988	-25.28797491	250	56701.8723148148	2014-02-13 20:56:08	56702.5974652778	2014-02-14 14:20:21	808115010	31.9389	30	31.9469	31.9389	0	31.9549	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57613.8117361111	2016-08-13 19:28:54	57080	2015-02-27 00:00:00	56714.739525463	2014-02-26 17:44:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	083002	We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA	NORBERT WERNER	JUS	8	AO8	OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808115010/	Quick Look
72	RXCJ0605	91.7111	-35.2772	91.267409	-35.26998	92.696732	-58.702768	241.82465393	-23.81756849	309.9841	55323.0313194444	2010-05-07 00:45:06	55323.8550810185	2010-05-07 20:31:19	805065030	42.4239	40	42.4319	42.4319	0	42.4239	2	2	0	2	1	0	0	39.146	39.146	71.1619	0	PROCESSED	57551.4298263889	2016-06-12 10:18:57	55287	2010-04-01 00:00:00	55341.5040393518	2010-05-25 12:05:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805065030/	Quick Look
73	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
74	NGC 2300 GROUP	112.834	85.6974	108.693645	85.79613	93.629136	62.546385	127.72312729	27.79205873	339.9186	55237.1794907407	2010-02-10 04:18:28	55238.2502777778	2010-02-11 06:00:24	804030020	52.5611	100	52.5611	52.5611	0	52.5611	2	2	0	2	1	0	0	47.712	47.712	92.498	0	PROCESSED	57550.5807986111	2016-06-11 13:56:21	55633	2011-03-13 00:00:00	55266.3365625	2010-03-11 08:04:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040055	We propose to observe the NGC 2300 group for 100 ks and a offset pointing for 200 ks to evaluate the background emission from the Galaxy. The purpose of the observations are to measure O, Mg, Si and Fe abundances of intragaractic medium to study metal synthesis in this small group of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KYOKO MATSUSHITA		JAP	4	AO4	O, MG, S AND FE ABUNDANCES OF INTRAGROUP MEDIUM IN THE NGC 2300 GROUP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804030020/	Quick Look
75	A3526	191.1432	-39.6142	190.459557	-39.340673	207.301582	-31.717062	301.49310157	23.23836897	110.0059	55944.2688078704	2012-01-18 06:27:05	55944.754375	2012-01-18 18:06:18	806090010	18.3702	16	18.3782	18.3702	0	18.3857	2	2	0	2	1	0	0	14.795	14.795	41.9499	2	PROCESSED	57604.405775463	2016-08-04 09:44:19	56352	2013-03-01 00:00:00	55985.1138310185	2012-02-28 02:43:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806090010/	Quick Look
76	J2218.8-0258	334.694	-2.9598	334.046783	-3.210826	335.453457	7.033577	59.75779093	-46.24852305	49.9996	56072.7972685185	2012-05-25 19:08:04	56073.7370833333	2012-05-26 17:41:24	807086010	38.3981	35	38.4061	38.3981	0	38.4061	2	2	0	2	1	0	0	36.9739	36.9739	81.1958	1	PROCESSED	57605.5228703704	2016-08-05 12:32:56	56500	2013-07-27 00:00:00	56134.0402199074	2012-07-26 00:57:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072018	We propose to observe the three clusters of galaxies J2218.2-0350, J2218.6-0346 and J2218.8-0258 with exposure times of 15, 25 and 35 ks respectively. These clusters are part of a structure of four linearly aligned clusters, separated from each other by 4 to 10 Mpc. We will accurately determine their masses and orientation. This will allow us to fully map the tidal force field of the structure, which is the prime force behind the formation of filaments in the cosmic web. We will study the effects of cluster mass, separation and mutual orientation on the filamentary structure of the cosmic web and on the evolution of galaxies therein.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	E.G. PATRICK BOS		EUR	7	AO7	CLUSTERS AND THE COSMIC WEB	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807086010/	Quick Look
77	A 2218 CENTER	249.0052	66.205	248.955095	66.304813	172.75657	81.615548	97.72589248	38.11630228	233.3294	53669.4904050926	2005-10-26 11:46:11	53670.1905555556	2005-10-27 04:34:24	800019010	31.9354	35	31.9434	31.9434	31.9354	31.9434	2	2	2	2	1	0	0	28.9371	28.9371	60.4879	1	PROCESSED	57527.6471990741	2016-05-19 15:31:58	54247	2007-05-27 00:00:00	54036.9596990741	2006-10-28 23:01:58	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001096	To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI		JAP	0	SWG	SEARCH FOR OXYGEN LINES FROM WARM IGM		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800019010/	Quick Look
78	ABELL 2259	260.1834	27.7413	259.686949	27.789931	256.20097	50.711544	50.50845469	31.05916058	109.9997	57082.4117476852	2015-03-01 09:52:55	57083.6002199074	2015-03-02 14:24:19	809081020	42.5928	42.5	42.5928	43.0168	0	43.0568	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.687650463	2016-08-17 16:30:13	57465	2016-03-18 00:00:00	57097.407037037	2015-03-16 09:46:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091526	Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	9	AO9	REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809081020/	Quick Look
79	SPT-CL J0000-5748	0.2511	-57.8123	359.609856	-58.090789	327.861661	-51.025666	315.62746494	-58.05556131	46.7517	55694.989849537	2011-05-13 23:45:23	55696.1169097222	2011-05-15 02:48:21	806074010	50.3986	50	50.3986	50.3986	0	50.3986	2	2	0	2	1	0	0	42.4563	42.4563	97.3498	0	PROCESSED	57602.0636921296	2016-08-02 01:31:43	56072	2012-05-25 00:00:00	55705.1979166667	2011-05-24 04:45:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061531	We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ERIC MILLER		USA	6	AO6	THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806074010/	Quick Look
80	Z235	10.9622	24.4059	10.298374	24.132304	19.875378	18.073678	120.72614401	-38.43334342	59.0539	53944.0060185185	2006-07-28 00:08:40	53944.6148032407	2006-07-28 14:45:19	801083010	20.0335	20	20.0415	20.0415	20.0415	20.0335	2	2	2	2	1	0	0	19.5263	19.5263	52.5899	1	PROCESSED	57535.0666782407	2016-05-27 01:36:01	54401	2007-10-28 00:00:00	53955.6800925926	2006-08-08 16:19:20	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801083010/	Quick Look
81	ABELL 262 CENTER	28.1922	36.1591	27.457024	35.91293	39.406526	22.931602	136.56609466	-25.08359968	69.9979	54329.1761921296	2007-08-17 04:13:43	54330.0446643518	2007-08-18 01:04:19	802001010	37.1645	36	37.1645	37.1645	0	37.1645	2	2	0	2	1	0	0	34.1304	34.1304	75.0299	1	PROCESSED	57539.6070949074	2016-05-31 14:34:13	54730	2008-09-21 00:00:00	54350.5576851852	2007-09-07 13:23:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020004	We propose to observe Abell 262. The temperature of the intracluster mediums of the cluster is 2 keV and therefore this cluster is between groups of galaxies and clusters of galaxies. The purpuse of the observation is to determine the distribution of O, Mg, Si and Fe f the intracluster medium upto 0.3 r180. The exposures are 30 ks for the central pointing and 40 ks for two offset pointings and the total exposure is 110ks.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	2	AO2	O AND MG ABUNDANCES OF THE INTRACLUSTER MEDIUMS OF ABELL 262	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802001010/	Quick Look
82	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
83	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
84	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
85	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
86	A1689-OFFSET2	197.956	-1.5158	197.313284	-1.250483	197.134748	5.642151	313.46570539	60.93832198	289.9994	54671.3493518518	2008-07-24 08:23:04	54672.423125	2008-07-25 10:09:18	803025010	43.5468	40	43.5468	43.5468	0	43.5468	2	2	0	2	1	0	0	36.5486	36.5486	92.7159	2	PROCESSED	57543.1297685185	2016-06-04 03:06:52	55076	2009-09-02 00:00:00	54707.2585763889	2008-08-29 06:12:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030100	We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NOBUHIRO OKABE		JAP	3	AO3	UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803025010/	Quick Look
87	A2061_1	229.9941	30.5295	229.479101	30.70939	216.056203	46.759039	47.89500096	57.43543483	120.6365	56306.3817939815	2013-01-14 09:09:47	56307.4847800926	2013-01-15 11:38:05	807029010	42.2923	40	42.3006	42.2991	0	42.2923	2	2	0	2	1	0	0	38.1838	38.1838	95.294	0	PROCESSED	57608.511087963	2016-08-08 12:15:58	56703	2014-02-15 00:00:00	56337.5472222222	2013-02-14 13:08:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070070	We propose to conduct multi-pointing observations to cover the entire region of A2061 hosting radio relic. We discovered that the radio relic is located in the cluster outskirts of the opposite side of the filamentary large-scale structure. We found the same trend for 3 relic clusters compiling NVSS radio and SDSS optical data-sets, though the sample number is small. It suggests that an universal process to form radio relic potentially exists. We therefore aim to map out the temperature, density, pressure, and entropy of the intra-cluster medium (ICM) to understand the interplays among the large-scale structure, the ICM and radio relic. Our study provides us a comprehensive picture of the ICM in the radio relic cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NOBUHIRO OKABE		JAP	7	AO7	SUZAKU OBSERVATION OF THE OUTSKIRTS IN RADIO RELIC CLUSTER A2061	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807029010/	Quick Look
88	BULLET-OFFSET1	104.8831	-55.8434	104.638861	-55.772465	130.550899	-77.176368	265.96507608	-21.0808269	287.0003	56416.3315277778	2013-05-04 07:57:24	56419.0787037037	2013-05-07 01:53:20	808055010	102.9172	100	102.9412	102.9172	0	102.9412	2	2	0	2	1	0	0	93.4395	93.4395	237.3167	4	PROCESSED	57611.2833564815	2016-08-11 06:48:02	56795	2014-05-18 00:00:00	56429.7533101852	2013-05-17 18:04:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080080	We propose two offset pointings of the bullet cluster with one adjacent blank-sky pointing. By detecting a very hot component in the ICM and mapping temperature/entropy out to the outskirts, we study thermodynamical evolution of the ICM in the course of cluster merger. More specifically, we estimate the fraction of energy injected to the ICM from the energy released by the merger, and the amount of energy heating the ICM through the shock, irreversible process.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	8	AO8	THERMODYNAMICAL EVOLUTION OF THE ICM IN THE BULLET CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808055010/	Quick Look
89	A3376 WEST RELIC	90.0415	-39.9946	89.634521	-39.995405	90.079962	-63.436398	246.43569548	-26.38071178	132.0018	53681.5938078704	2005-11-07 14:15:05	53684.7883912037	2005-11-10 18:55:17	800011010	126.9969	150	126.9969	127.1809	127.0769	127.0289	2	2	2	2	1	0	0	112.9113	112.9113	230.9397	3	PROCESSED	57528.0013541667	2016-05-20 00:01:57	54247	2007-05-27 00:00:00	54037.6050231482	2006-10-29 14:31:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001039	We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA		JAP	0	SWG	SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800011010/	Quick Look
90	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
91	A2163NW	243.7926	-5.9349	243.126237	-5.810502	242.931845	15.076918	6.85972512	30.71314923	93.93	57075.8011574074	2015-02-22 19:13:40	57077.0558333333	2015-02-24 01:20:24	809008010	48.0634	50	48.0634	49.7339	0	49.7194	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6490046296	2016-08-17 15:34:34	57454	2016-03-07 00:00:00	57087.4664467593	2015-03-06 11:11:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090032	Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	9	AO9	SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809008010/	Quick Look
92	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
93	A2572B	349.6066	18.7294	348.98329	18.45586	358.210513	21.259827	94.21850787	-38.90117923	59.1565	53922.7742939815	2006-07-06 18:34:59	53923.3002199074	2006-07-07 07:12:19	801073010	24.0595	21	24.0755	24.0595	24.0675	24.0755	2	2	2	2	1	0	0	21.4951	21.4951	45.3979	1	PROCESSED	57534.8583912037	2016-05-26 20:36:05	54401	2007-10-28 00:00:00	53930.6043055556	2006-07-14 14:30:12	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801073010/	Quick Look
94	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
95	1RXJ0603 OFFSET	92.2783	42.2687	91.384795	42.277603	91.783385	18.842189	170.6889541	10.70559867	80.0991	56214.8308564815	2012-10-14 19:56:26	56215.5314236111	2012-10-15 12:45:15	807002010	26.8334	30	26.8334	26.8574	0	26.8414	2	2	0	2	1	0	0	28.3531	28.3531	60.5159	1	PROCESSED	57607.7719907407	2016-08-07 18:31:40	56690	2014-02-02 00:00:00	56323.4936574074	2013-01-31 11:50:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070025	We propose to 120 ks + 30 ks (background) Suzaku observations of a new cluster scale shock front candiate in merger cluster of galaxies 1RXJ0603. 1RXJ0603 has irregular shape radio relic with remarkable steep radio spectrum index, which indicate the existence of shock fronts with mach number M ~ 4.5. The temperature and density of Intra ClusterMedium across radio relics will provide the nature of shock front. Our study will shed new light on the origin of the cluster scale shock fronts.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	HIROKI AKAMATSU		JAP	7	AO7	SUZAKU OBSERVATION OF A NEW CLUSTER SCALE SHOCK FRONT CANDIATE IN MERGING CLUSTER OF GALAXIES 1RXJ0603	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807002010/	Quick Look
96	CENA LOBE BGD1	205.3783	-39.3349	204.641576	-39.082547	218.514411	-26.72025	313.38854271	22.51794697	286.0001	56122.4603125	2012-07-14 11:02:51	56123.1043634259	2012-07-15 02:30:17	807042010	22.2455	20	22.2455	22.2455	0	22.2455	2	2	0	2	1	0	0	18.8556	18.8556	55.616	1	PROCESSED	57606.6151157407	2016-08-06 14:45:46	56018	2012-04-01 00:00:00	56142.2381597222	2012-08-03 05:42:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070106	Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LUKASZ STAWARZ		JAP	7	AO7	STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807042010/	Quick Look
97	COMA W SHOCK1	194.1832	28.2738	193.578654	28.544023	180.637957	31.358455	77.58391557	88.36116739	275.406	56475.3084143518	2013-07-02 07:24:07	56475.66125	2013-07-02 15:52:12	808090010	16.692	15	16.692	16.716	0	16.7	2	2	0	2	1	0	0	13.638	13.638	30.4759	1	PROCESSED	57611.6582407407	2016-08-11 15:47:52	56897	2014-08-28 00:00:00	56524.6518518518	2013-08-20 15:38:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081529	Our analysis of Suzaku data of the Coma Cluster revealed an intriguing correlation between the outer edge of its radio halo and the thermodynamic properties of the gas. This correlation seems to be the most pronounced in the western direction where the temperature drops from about 10keV in the annulus spanning 35'-41' to only 1.7keV in the annulus spanning 50'-60'. The Planck Collaboration found a marked local steepening of the radial gradient of the SZ signal at this location and interpret this feature as a shock with a Mach number of about 2. Unfortunately, we currently lack X-ray coverage towards the W in this critical range of 41'-50'. We therefore propose two additional pointings with a total exposure time of 30ks, that will allow us to resolve the temperature gradient in this region.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AURORA SIMIONESCU		USA	8	AO8	THE MISSING PUZZLE PIECE IN THE COMA SHOCK FRONT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808090010/	Quick Look
98	A478 OFFSET A	63.4449	10.2053	62.759891	10.079352	63.389046	-10.816509	182.72704568	-28.38203256	259.1008	55600.4642361111	2011-02-08 11:08:30	55601.5488194444	2011-02-09 13:10:18	805001010	44.3964	45	44.3964	44.3964	0	44.3964	2	2	0	2	1	0	0	35.2374	35.2374	93.6998	1	PROCESSED	57600.8998148148	2016-07-31 21:35:44	55983	2012-02-26 00:00:00	55617.4093981482	2011-02-25 09:49:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050008	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 a representative regular cluster, Abell 478	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA	ANDREW FABIAN	JAP	5	AO5	DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805001010/	Quick Look
99	THE MOON	337.3918	-5.9294	336.739564	-6.185815	336.879419	3.286876	58.6068568	-50.1809823	252.3009	56990.3496643518	2014-11-29 08:23:31	56990.483587963	2014-11-29 11:36:22	809001320	6.3868	45	6.3868	6.3868	0	6.3868	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.4101851852	2016-08-17 09:50:40	57415	2016-01-28 00:00:00	57006.395	2014-12-15 09:28:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001320/	Quick Look
100	A133_N	15.6732	-21.6726	15.062059	-21.941094	5.322246	-26.023104	148.68503798	-83.97324559	44.9987	55352.9000347222	2010-06-05 21:36:03	55354.0974768518	2010-06-07 02:20:22	805020010	50.2334	50	50.2334	50.2334	0	50.2334	1	1	0	1	1	0	0	44.176	44.176	103.416	1	PROCESSED	57551.8040740741	2016-06-12 19:17:52	55765	2011-07-23 00:00:00	55393.4422916667	2010-07-16 10:36:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050019	We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KOSUKE SATO		JAP	5	AO5	METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805020010/	Quick Look
101	FJ1145+6430	176.4302	64.5188	175.749504	64.796472	138.22089	54.839324	134.11889935	51.15827028	157.0241	56940.8652199074	2014-10-10 20:45:55	56941.847337963	2014-10-11 20:20:10	809036010	44.5555	45	44.5555	44.9155	0	44.9235	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6416435185	2016-08-16 15:23:58	57345	2015-11-19 00:00:00	56979.4120949074	2014-11-18 09:53:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090090	Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	IKUYUKI MITSUISHI		JAP	9	AO9	EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809036010/	Quick Look
102	CIZA J1358.9-4750	209.651	-47.7758	208.860998	-47.532845	225.745985	-33.169178	314.45332941	13.58776424	104.5762	56313.755	2013-01-21 18:07:12	56315.4835648148	2013-01-23 11:36:20	807037010	61.6899	60	61.7299	61.6899	0	61.731	2	2	0	2	1	0	0	58.9497	58.9497	149.3318	1	PROCESSED	57608.595162037	2016-08-08 14:17:02	56718	2014-03-02 00:00:00	56351.6358680556	2013-02-28 15:15:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070101	We propose a Suzaku observation of newly found merging cluster in the Zone of Avoidance, CIZA J1358.9-4750. The cluster has double core, and apparently in an early phase of merging. Targets with this phase is rare. With this observation, we want to obtain the temperature map of the bridge region and identify the existence of heating, to understand the merging phase of this cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TERUKAZU NISHIDA		JAP	7	AO7	OBSERVATION OF THE NEWLY DISCOVERED MERGING CLUSTER NEAR THE GALACTIC DISC; CIZA J1358.9-4750	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807037010/	Quick Look
103	CENTAURUS CLUSTER N	192.2138	-40.9141	191.523743	-40.64159	208.863601	-32.495572	302.40583252	21.95501054	115.2417	55961.0060763889	2012-02-04 00:08:45	55962.6667939815	2012-02-05 16:00:11	806011010	54.0496	50	54.0496	54.0496	0	54.0496	2	2	0	2	1	0	0	48.6109	48.6109	143.4758	2	PROCESSED	57604.5565972222	2016-08-04 13:21:30	56360	2013-03-09 00:00:00	55992.1577546296	2012-03-06 03:47:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060035	We propose to observe two fields at 0.1-0.2r180 of the Centaurus cluster for total 90 ks exposures with Suzaku. The purpose of the observations is to determine Mg and Fe distributions of the intracluster medium up to 0.2 r180 and to study origin of metals in the intracluster medium.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KYOKO MATSUSHITA		JAP	6	AO6	MG AND FE ABUNDANCES OF THE ICM IN THE CENTAURUS CLUSTER UP TO 0.2R180	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806011010/	Quick Look
104	ABELL2801	9.6433	-29.1188	9.027926	-29.393572	356.054774	-30.312746	357.12193154	-86.53506096	232.0377	53701.3547106482	2005-11-27 08:30:47	53702.1668865741	2005-11-28 04:00:19	800008010	34.89	25	34.89	34.89	34.89	34.89	2	2	2	2	1	0	0	30.1636	30.1636	70.1639	1	PROCESSED	57528.0891898148	2016-05-20 02:08:26	54247	2007-05-27 00:00:00	54038.3717361111	2006-10-30 08:55:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001025	We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYUKI TAMURA		JAP	0	SWG	THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800008010/	Quick Look
105	ABELL 1795 Near North	207.2221	26.7993	206.645445	27.047459	193.815884	35.172187	34.737463	77.20142043	130.7334	53714.7756481482	2005-12-10 18:36:56	53715.3203587963	2005-12-11 07:41:19	800012020	24.4106	25	24.4266	24.4106	24.4426	24.4346	1	1	1	1	1	0	0	25.1798	25.1798	47.0559	2	PROCESSED	57532.404375	2016-05-24 09:42:18	54247	2007-05-27 00:00:00	54038.8804166667	2006-10-30 21:07:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012020/	Quick Look
106	ABELL 1795 Near South	207.2228	26.4007	206.645046	26.648859	194.026663	34.812966	32.94964182	77.16185549	129.833	53715.9739467593	2005-12-11 23:22:29	53716.5355787037	2005-12-12 12:51:14	800012040	26.074	25	26.098	26.0919	26.074	26.086	2	2	2	2	1	0	0	25.7986	25.7986	48.522	1	PROCESSED	57532.4329282407	2016-05-24 10:23:25	54247	2007-05-27 00:00:00	54039.0706018518	2006-10-31 01:41:40	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012040/	Quick Look
107	NGC4388	186.4461	12.6674	185.812197	12.944186	180.780806	14.166666	279.11809751	74.34084148	119.622	53728.3779976852	2005-12-24 09:04:19	53731.250162037	2005-12-27 06:00:14	800017010	123.6341	100	123.9249	125.8143	123.6341	124.1523	2	2	2	2	1	0	0	111.8209	111.8209	248.128	3	PROCESSED	57532.5484143518	2016-05-24 13:09:43	54247	2007-05-27 00:00:00	54039.5984375	2006-10-31 14:21:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001077	Large-scale X-ray nebulae up to a few tens of kpc have been often found in starburst galaxies, which is thermally heated up by the superwind from the starburst nucleus. Iwasawa et al. (2003) found a large X-ray nebula up to 16kpc around NGC4388, which is photoiionized by Seyfert nucleus. Thus, this result suggests that the hard X-ray emission from active galactic nucleus could be a prime heat source of nebula. The goals of this observation are (1) to see how far the X-ray nebula is extended, (2) to obtain its precise X-ray spectrum, (3) to determine what is the X-ray emission mechanism, and (4) to exam if the photoionization by AGN could be a prime heat source of the galactic halo. We determine the photon index and the high energy cut-off of the power-law component from the HXD spectrum.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKESHI TSURU		JAP	0	SWG	VERY EXTENDED PHOTOIONIZED X-RAY NEBULA AROUND THE SEYFERT GALAXY NGC4388	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800017010/	Quick Look
108	A2104W	234.9146	-3.2969	234.261116	-3.135581	233.381893	15.795133	2.73337641	39.30878407	117.9077	54121.3401388889	2007-01-21 08:09:48	54121.8960532407	2007-01-21 21:30:19	801001010	19.9269	20	19.9269	19.9269	0	19.9269	1	1	0	1	1	0	0	17.2001	17.2001	48.0079	2	PROCESSED	57536.8971875	2016-05-28 21:31:57	54735	2008-09-26 00:00:00	54137.0936805556	2007-02-06 02:14:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010012	We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO HATTORI		JAP	1	AO1	TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801001010/	Quick Look
109	RX J1347.5-1145	206.8558	-11.8095	206.189394	-11.560383	209.147012	-0.679812	323.97878779	48.76095676	291.7151	53931.2858333333	2006-07-15 06:51:36	53933.2551388889	2006-07-17 06:07:24	801013020	79.1105	75	79.1265	79.1105	79.1265	79.1345	2	2	2	2	1	0	0	69.567	69.567	170.1098	2	PROCESSED	57534.9865393518	2016-05-26 23:40:37	54394	2007-10-21 00:00:00	53942.463587963	2006-07-26 11:07:34	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010014	We propose to obtain broad-band spectra of the most X-ray luminous cluster of galaxies RXJ1347.5-1145 at z=0.45. Our previous high-resolution Sunyaev-Zel'dovich obvervations of this cluster revealed that it exhibits an unusually violent merger activity. Its high X-ray luminosity ensures the unprecedented high-quality spectra with Suzaku. It is indeed a unique target to probe gas physics and particle acceleration mechanism associated with the violent mergers at high redshift. The continuum observations with HXD and XIS as well as the iron line spectroscopy will specify the physical states of both thermal and non-thermal components of the ICM. Combined with the Chandra and our SZ data, the Suzaku data will accomplish the first comprehensive modeling of a violent merger in distant clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	NAOMI OTA		JAP	1	AO1	BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801013020/	Quick Look
110	OPHIUCHUS CLUSTER 0	258.0174	-23.3865	257.259196	-23.326891	259.005066	-0.401441	0.50702706	9.33401192	88.8366	54183.0313078704	2007-03-24 00:45:05	54183.5648726852	2007-03-24 13:33:25	801021010	16.6411	15	16.6411	16.6411	0	16.6411	2	2	0	2	1	0	0	13.5209	13.5209	46.0959	0	PROCESSED	57537.9746643518	2016-05-29 23:23:31	54736	2008-09-27 00:00:00	54209.5175462963	2007-04-19 12:25:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010065	The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUTAKA FUJITA		JAP	1	AO1	PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801021010/	Quick Look
111	OPHIUCHUS CLUSTER 8	258.0175	-23.6665	257.257716	-23.606887	259.028283	-0.680466	0.2749393	9.17298979	88.8988	54182.4897337963	2007-03-23 11:45:13	54183.0308333333	2007-03-24 00:44:24	801029010	23.7389	15	23.7469	23.7389	0	23.7469	2	2	0	2	1	0	0	21.678	21.678	46.746	0	PROCESSED	57537.9753240741	2016-05-29 23:24:28	54736	2008-09-27 00:00:00	54209.5725231482	2007-04-19 13:44:26	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010065	The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUTAKA FUJITA		JAP	1	AO1	PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801029010/	Quick Look
112	M87 50' SE	188.2678	11.8367	187.635305	12.112401	182.806232	14.132107	286.30035277	74.11241529	119.899	54071.127650463	2006-12-02 03:03:49	54072.312037037	2006-12-03 07:29:20	801039010	53.6374	50	53.6374	53.6581	0	53.6454	2	2	0	2	1	0	0	46.1394	46.1394	102.309	1	PROCESSED	57536.2354861111	2016-05-28 05:39:06	54735	2008-09-26 00:00:00	54088.5776736111	2006-12-19 13:51:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010084	The black hole at the center of M87 is one of the most heaviest in the universe. Recently TeV-gamma ray emission from M87 was found. M87 is thus a very strong candidate for an accelerator of ultra-high energy cosmic rays. We aim at the detection of non-thermal hard X-rays from M87 to clarify the mechanism of the particle acceleration. The giant elliptical galaxy M87 is at the center of the Virgo cluster of galaxies, which is the nearest cluster. We can investigate the distribution of various metal elements. We will clarify how the metals, especially oxygen, diffuse to the intracluster space from the galaxy M87.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	HIRONORI MATSUMOTO		JAP	1	AO1	NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801039010/	Quick Look
113	PERSEUS CL OFFSET	49.2788	41.3719	48.454118	41.188803	58.04223	22.344257	150.2212005	-13.65398882	65.9966	53980.7676273148	2006-09-02 18:25:23	53981.4543287037	2006-09-03 10:54:14	801049020	32.4646	30	32.4806	32.4646	32.4966	32.4886	1	1	1	1	1	0	0	28.2912	28.2912	59.3199	1	PROCESSED	57535.422025463	2016-05-27 10:07:43	54526	2008-03-01 00:00:00	54021.2712731482	2006-10-13 06:30:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010097	We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	1	AO1	MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049020/	Quick Look
114	ABELL 2199 OFFSET 4	247.0296	39.3161	246.598828	39.425672	233.044127	59.841273	62.60481799	43.78660639	250.4756	54012.6800462963	2006-10-04 16:19:16	54013.3044444444	2006-10-05 07:18:24	801060010	24.4546	25	24.4706	24.4626	24.4546	24.4775	2	2	2	2	1	0	0	25.811	25.811	53.9399	0	PROCESSED	57535.7612615741	2016-05-27 18:16:13	54735	2008-09-26 00:00:00	54024.6738888889	2006-10-16 16:10:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010138	Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	1	AO1	PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801060010/	Quick Look
115	Z8276	266.0474	32.9693	265.586798	32.989586	263.998981	56.326696	57.88393681	27.65216461	308.1365	53961.1406134259	2006-08-14 03:22:29	53961.4723958333	2006-08-14 11:20:15	801079010	14.9374	14	14.9374	14.9374	14.9374	14.9374	1	1	1	1	1	0	0	15.462	15.462	28.658	0	PROCESSED	57535.267962963	2016-05-27 06:25:52	54391	2007-10-18 00:00:00	54018.6023842593	2006-10-10 14:27:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801079010/	Quick Look
116	A3667_CENTER	303.141	-56.7974	302.14092	-56.947599	291.656641	-35.82366	340.90266514	-33.39955413	74.263	53861.7363078704	2006-05-06 17:40:17	53862.3843055556	2006-05-07 09:13:24	801096010	20.8805	20	20.8885	20.8885	20.8965	20.8805	1	1	1	1	1	0	0	8.425	8.425	55.9439	1	PROCESSED	57533.6497337963	2016-05-25 15:35:37	54394	2007-10-21 00:00:00	53913.7840509259	2006-06-27 18:49:02	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	013080	We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA	CRAIG SARAZIN	JUS	1	AO1	SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801096010/	Quick Look
117	CEN45	192.5119	-41.3865	191.819775	-41.11429	209.359018	-32.811033	302.65166747	21.4844922	104.7288	54458.1467939815	2007-12-24 03:31:23	54459.2294444444	2007-12-25 05:30:24	802008010	58.2226	53	58.2226	58.2365	0	58.2306	2	2	0	2	1	0	0	64.5171	64.5171	93.5218	2	PROCESSED	57540.9525810185	2016-06-01 22:51:43	54854	2009-01-23 00:00:00	54486.1941087963	2008-01-21 04:39:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020011	We propose to obtain high-quality X-ray spectra of the subcluster region in the Centaurus cluster, Cen45, aiming at the first reliable detection of a supersonic motion of the intracluster gas. Previous optical and X-ray observations suggest that Cen45 is indeed in the process of merging and has a high velocity relative to the main cluster. Utilizing the high-sensitivity Suzaku/XIS spectroscopy, the line-of-sight velocity of the X-ray emitting gas can be accurately measured from the Doppler shift of iron-K lines. With our proposed 40ks observation, we can put a strong constraint on the gas motion in the subcluster region. This will also have great impacts on our understanding of dynamical state of clusters and their evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	NAOMI OTA		JAP	2	AO2	MEASURING GAS MOTIONS OF THE INFALLING SUBCLUSTER CEN45	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802008010/	Quick Look
118	A963N	154.2645	39.1732	153.523641	39.42315	141.268932	26.461753	182.34163859	55.82043448	108.9136	54428.4751041667	2007-11-24 11:24:09	54429.0522453704	2007-11-25 01:15:14	802010010	29.1318	25	29.1318	29.1413	0	29.1358	2	2	0	2	1	0	0	27.8843	27.8843	49.8381	0	PROCESSED	57540.5914351852	2016-06-01 14:11:40	54804	2008-12-04 00:00:00	54434.2199305556	2007-11-30 05:16:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020018	We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 10% precision in a few arcmin scale, which has not been done before to any cluster. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO HATTORI		JAP	2	AO2	TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802010010/	Quick Look
119	FORNAX_GALACTIC_1	48.2958	-37.68	47.815673	-37.866142	29.586545	-52.740717	241.51144521	-58.49700193	45.4419	54279.8103240741	2007-06-28 19:26:52	54280.3335532407	2007-06-29 08:00:19	802037010	20.4175	20	20.4175	20.4175	0	20.4175	1	1	0	1	1	0	0	16.1912	16.1912	45.184	0	PROCESSED	57539.0539814815	2016-05-31 01:17:44	54695	2008-08-17 00:00:00	54322.4346064815	2007-08-10 10:25:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020119	We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YOH TAKEI		JAP	2	AO2	DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802037010/	Quick Look
120	OPHIUCHUS CLUSTER	258.1093	-23.379	257.351096	-23.319827	259.088514	-0.387026	0.56233145	9.26925896	277.7852	54367.8835069444	2007-09-24 21:12:15	54370.5939351852	2007-09-27 14:15:16	802046010	100.525	100	100.525	100.525	0	100.525	2	2	0	2	1	0	0	82.9495	82.9495	234.1619	3	PROCESSED	57540.1576041667	2016-06-01 03:46:57	54770	2008-10-31 00:00:00	54402.5613194444	2007-10-29 13:28:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020143	The verification of the resonance scattering effect to resonance lines in an intracluster medium (ICM) is a big problem that has been carried over from ASCA. Though two interpretations for abnormality of intensity ratio of Fe-Kalpha/Fe Kbeta line, "resonance scattering effect" and "Ni overabundance", have been proposed, a determinate result has not been obtained. Both interpretations give a very big impact to the understanding of chemical evolution of ICM that has been obtained so far. To solve the problem, we propose the measurement of Ni and Fe lines with high precision for Ophiuchus cluster which is bright and hot enough for measuring the K lines. Moreover, this cluster is suggested the existence of non-thermal radiation from observations with Beppo-SAX, INTEGRAL, Swift.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AKIHIRO FURUZAWA		JAP	2	AO2	APPROCHING RESONANCE SCATTERING/NI-OVERABUNDANCE PROBLEM IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802046010/	Quick Look
121	COMA_60OFF	194.0251	27.4252	193.418894	27.695609	180.937501	30.537759	49.19228369	88.92228234	126.7582	54438.1998726852	2007-12-04 04:47:49	54439.1946990741	2007-12-05 04:40:22	802048010	36.6669	30	36.6669	36.6669	0	36.6669	2	2	0	2	1	0	0	31.6962	31.6962	85.9219	1	PROCESSED	57540.8231365741	2016-06-01 19:45:19	54814	2008-12-14 00:00:00	54445.3011689815	2007-12-11 07:13:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020149	With XIS and HXD onboard Suzaku, we propose a scanning observation along the large-scale filament structure connecting the Coma cluster outskirts and the radio relic 1253+275. The scientific aims are: 1) to verify and delineate the spatial extent of the hard X-ray excess reported by BeppoSAX and RXTE, 2) to constrain the spatial distribution of large-scale magnetic fields, 3) to probe nonthermal processes associated with structure formation, such as ultra-high-energy particle acceleration at the cluster accretion shock, and 4) to provide complementary data in connection with observations in other wavebands, especially GeV-TeV gamma-rays.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	SUSUMU INOUE		JAP	2	AO2	EXPLORING PARTICLE ACCELERATION AND MAGNETIC FIELDS IN A LARGE-SCALE FILAMENT STRUCTURE ASSOCIATED WITH THE COMA CLUSTER	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802048010/	Quick Look
122	BOOTES GROUP 26	219.0541	33.7727	218.530502	33.989642	201.885156	45.915481	55.78379271	66.53529007	323.2958	54265.160787037	2007-06-14 03:51:32	54266.3092476852	2007-06-15 07:25:19	802055010	43.6657	38	43.6737	43.6817	0	43.6657	2	2	0	2	1	0	0	38.8727	38.8727	99.2108	0	PROCESSED	57538.9553703704	2016-05-30 22:55:44	54695	2008-08-17 00:00:00	54271.4809837963	2007-06-20 11:32:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021424	We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MARSHALL BAUTZ		USA	2	AO2	SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802055010/	Quick Look
123	PKS 0745-191	116.8852	-19.2901	116.331446	-19.165404	123.663194	-39.639458	236.4397894	3.03527791	293.9994	54231.0124884259	2007-05-11 00:17:59	54231.8216898148	2007-05-11 19:43:14	802062010	32.0065	30	32.0065	32.0305	0	32.0145	2	2	0	2	1	0	0	27.7016	27.7016	69.9099	0	PROCESSED	57538.6154976852	2016-05-30 14:46:19	54695	2008-08-17 00:00:00	54238.8868518518	2007-05-18 21:17:04	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021440	PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ANDREW YOUNG		USA	2	AO2	PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062010/	Quick Look
124	FILAMENT JUNCTION 1	204.175	43.8307	203.643106	44.085146	179.610846	48.837733	97.2080472	70.96687365	328.3601	55706.688900463	2011-05-25 16:32:01	55707.984224537	2011-05-26 23:37:17	806003010	52.5091	60	52.5091	52.5171	0	52.5171	2	2	0	2	1	0	0	50.1339	50.1339	111.8899	0	PROCESSED	57602.1515509259	2016-08-02 03:38:14	56093	2012-06-15 00:00:00	55725.311412037	2011-06-13 07:28:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060015	Haloes, such as galaxy clusters or groups have been considered to form at intersections of cosmological filaments. Nevertheless, there are a lot of junctions of galaxy filaments without X-ray strong signal from massive clusters. We propose a SUZAKU observation of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey using a new method. The SUZAKU observation of high sensitivity in low energy will reveal nature of faint haloes growing in the large filament junctions.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HAJIME KAWAHARA		JAP	6	AO6	EXPLORING JUNCTIONS OF GALAXY FILAMENTS BY SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806003010/	Quick Look
125	PKS 0745-191	117.1155	-19.3739	116.561976	-19.248204	123.963107	-39.669924	236.62179243	3.1809503	294.0002	54233.2263773148	2007-05-13 05:25:59	54234.0369675926	2007-05-14 00:53:14	802062040	32.9092	30	32.9092	32.9092	0	32.9092	1	1	0	1	1	0	0	31.0085	31.0085	69.9999	0	PROCESSED	57538.6488541667	2016-05-30 15:34:21	54695	2008-08-17 00:00:00	54245.5354861111	2007-05-25 12:51:06	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021440	PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ANDREW YOUNG		USA	2	AO2	PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062040/	Quick Look
126	ABELL 262 OFFSET1	28.5344	36.2686	27.797773	36.023209	39.729024	22.927942	136.82832457	-24.90547123	69.9996	54318.8941898148	2007-08-06 21:27:38	54320.0772337963	2007-08-08 01:51:13	802079010	54.5894	48	54.5974	54.5894	0	54.6029	2	2	0	2	1	0	0	50.9123	50.9123	102.2038	1	PROCESSED	57539.4485416667	2016-05-31 10:45:54	54730	2008-09-21 00:00:00	54347.4244791667	2007-09-04 10:11:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	023004	We propose to observe Abell 262. The temperature of the intracluster mediums of the cluster is 2 keV and therefore this cluster is between groups of galaxies and clusters of galaxies. The purpuse of the observation is to determine the distribution of O, Mg, Si and Fe f the intracluster medium upto 0.3 r180. The exposures are 30 ks for the central pointing and 40 ks for two offset pointings and the total exposure is 110ks.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	Fabio Gastaldello	JUS	2	AO2	O AND MG ABUNDANCES OF THE INTRACLUSTER MEDIUMS OF ABELL 262	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802079010/	Quick Look
127	IKT25	16.5704	-72.153	16.175469	-72.420209	314.528049	-65.245772	301.32642461	-44.92895011	33.6181	54601.2130208333	2008-05-15 05:06:45	54603.3675810185	2008-05-17 08:49:19	803002010	107.3223	100	107.3303	107.3303	0	107.3223	2	2	0	2	1	0	0	124.1064	124.1064	186.1339	1	PROCESSED	57542.58375	2016-06-03 14:00:36	54981	2009-05-30 00:00:00	54613.1905439815	2008-05-27 04:34:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030016	In order for the white dwarf, the progenitor of SN Ia, to increase its mass to the Chandrasekhar limit, stellar wind driven by Fe contained in the accreting matter needs to be strong enough. For this reason, SN Ia is difficult to take place in the galaxy with low metallicity. We propose the observation on IKT 25, a type Ia SNR candidate in SMC, in order to decide its origin. Since the Fe abundance of SMC (0.2 solar) is lower than that of any other galaxys where SN Ia (or its remnant) had already been discovered, this observation will give the strongest restriction to the theory of the white dwarf evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROYA YAMAGUCHI		JAP	3	AO3	IKT25: TYPE IA SNR CANDIDATE IN SMALL MAGELLANIC CLOUD	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803002010/	Quick Look
128	ZWCL_0823_FILAMENT-1	126.4596	4.2515	125.801978	4.415646	127.752151	-14.538767	220.17063425	22.90045491	284.0603	54603.3781944444	2008-05-17 09:04:36	54604.4551388889	2008-05-18 10:55:24	803009010	41.3573	40	41.3573	41.3619	0	41.3619	2	2	0	2	1	0	0	35.9369	35.9369	93.0059	1	PROCESSED	57542.5603472222	2016-06-03 13:26:54	54979	2009-05-28 00:00:00	54613.0757060185	2008-05-27 01:49:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030039	We propose Suzaku X-ray follow-up observations of dark matter (DM) halo "sub-clumps" detected by the Subaru weak-lens survey. The sub-clumps we are interested in are the smaller DM halo associated with large scale structures. According to the CDM hierarchical structure formation scenario, they are the elemental component of the universe. Since the barion component associated to the clumps are supposed to be very faint, the X-ray follow-up requires the highest sensitivity for diffuse sources, i.e. the Suzaku XIS detectors. Our aim is to detect barion signals and reveal the history/nature of these sub-clumps. A total of four pointing, two aiming at A222/223 filament and another two at ZwCl0823--A664 filament are proposed.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KAZUHIRO NAKAZAWA		JAP	3	AO3	SUZAKU X-RAY FOLLOW-UP OF DARK MATTER SUB-CLUMPS DETECTED WITH SUBARU WEAK-LENS SURVEY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803009010/	Quick Look
129	NGC1961BACKGROUND	85.5048	67.8763	84.182746	67.851301	87.633372	44.47331	145.2497599	18.81010884	72.0206	54748.602962963	2008-10-09 14:28:16	54749.1197222222	2008-10-10 02:52:24	803041010	24.1435	20	24.1435	24.1435	0	24.1435	2	2	0	2	1	0	0	20.099	20.099	44.6399	1	PROCESSED	57544.0915393518	2016-06-05 02:11:49	55148	2009-11-13 00:00:00	54780.6911342593	2008-11-10 16:35:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031401	Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio. The Milky Way is missing at least 70% of its baryons while lower mass galaxies retain less than 10% of their baryons. Theory suggests that these baryons were expelled by intense galactic winds during the primary star formation period. These galactic winds carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding the very massive spiral galaxy, NGC 1961, which has 10 times the stellar content of M31 and with v_rot = 450 km/sec. If successful, we will detect a significant fraction of the 5E11 Msun of its missing baryons.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	3	AO3	THE BARYONS CONTENT OF THE MOST MASSIVE SPIRAL GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803041010/	Quick Look
130	ABELL S753 RELIC	211.0241	-34.0331	210.287956	-33.79356	220.862622	-20.093047	319.70505054	26.46102153	102.5257	54838.0480555556	2009-01-07 01:09:12	54841.6668287037	2009-01-10 16:00:14	803053010	137.5275	120	137.5355	137.5275	0	137.5355	3	3	0	3	1	0	0	99.5992	99.5992	312.6056	3	PROCESSED	57545.2410069444	2016-06-06 05:47:03	55328	2010-05-12 00:00:00	54851.4730787037	2009-01-20 11:21:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031432	The cluster radio relic PKS B1400-33 in the poor cluster Abell S753 will be observed with the HXD/PIN to detect and characterize the nonthermal Inverse Compton emission. This is one of the brightest cluster radio relics known. Remarkably, it is associated with a relatively poor, cool cluster. Although it has many properties similar to other cluster radio relics, it is possible that it is an old radio lobe, displaced by motions or buoyancy. The HXD/PIN data will be a strong test of merger shock acceleration processes. The XIS observations will constrain the low energy nonthermal spectrum and determine the thermal gas properties near the relic, and allow a merger shock to be detected. The long exposure with the XIS will also provide accurate abundances for the gas in this cool cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CRAIG SARAZIN		USA	3	AO3	PKS B1400-33 AND ABELL S753: A VERY BRIGHT RADIO RELIC IN A POOR CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803053010/	Quick Look
131	A3112	49.4785	-44.2477	49.044044	-44.429449	25.501128	-58.962889	252.95565297	-56.08416767	11.0983	54609.240162037	2008-05-23 05:45:50	54611.0557638889	2008-05-25 01:20:18	803054010	67.4982	60	67.4982	67.4982	0	67.4982	2	2	0	2	1	0	0	59.0658	59.0658	156.8578	0	PROCESSED	57542.6456365741	2016-06-03 15:29:43	54988	2009-06-06 00:00:00	54620.3684490741	2008-06-03 08:50:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031434	We propose to perform spatially resolved spectroscopy on the X-ray bright relaxed galaxy cluster Abell 3112, in order to characterize its soft/hard X-ray excess component. Abell 3112 is one of two clusters with very strong soft excess emission (the other being Abell S1101, observed in AO1). The indications provided by this observation will be crucial in order to assess, beyond doubt, the reality of the soft excess emission, previously observed by all soft X-ray missions since EUVE. The proposed observation will constrain the nature of the excess emitter, and address outstanding questions in observational cosmology: the {it missing baryon} problem, the density of matter in the universe and the non-thermal energy in galaxy clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MASSIMILIANO BONAMENTE		USA	3	AO3	SOFT EXCESS, HARD EXCESS AND THERMAL EMISSION IN ABELL 3112	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803054010/	Quick Look
132	SHAPLEY OFF-FILAMENT	201.0894	-30.5701	200.390777	-30.309695	211.196223	-20.080758	311.26734846	31.76827748	298.8248	54666.4273958333	2008-07-19 10:15:27	54670.1905439815	2008-07-23 04:34:23	803068010	143.4669	140	143.4749	143.4749	0	143.4669	2	2	0	2	1	0	0	110.8111	110.8111	325.0858	2	PROCESSED	57543.1803240741	2016-06-04 04:19:40	55073	2009-08-30 00:00:00	54707.3575694444	2008-08-29 08:34:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031451	It is, in principle, possible to search for the signature of the Warm-Hot Intergalactic Medium (WHIM) in regions between clusters, where WHIM filaments are expected. However, the complexity of the filament network and the distance between clusters makes this approach very difficult (if not impossible), except in few cases where several clusters are sufficiently close together, such as within a supercluster. We propose an investigation using Suzaku of a region within the Shapley Supercluster where, following the cluster network, a filament is expected and a ROSAT PSPC investigation has found excess emission. Suzaku s characteristics will allow a clear detection and characterization of the filament. A second observation in an empty region nearby will be used as control field.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MASSIMILIANO GALEAZZI		USA	3	AO3	FILAMENTARY X-RAY STRUCTURE IN THE SHAPLEY SUPERCLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803068010/	Quick Look
133	DEM L 205	82.0576	-67.4229	82.080975	-67.461346	340.764256	-86.78514	277.64219696	-32.8462006	9.9744	55005.3430092593	2009-06-23 08:13:56	55006.4578472222	2009-06-24 10:59:18	804010010	41.3433	40	41.3492	41.3492	0	41.3433	2	2	0	2	1	0	0	37.3829	37.3829	96.3078	3	PROCESSED	57547.6717361111	2016-06-08 16:07:18	55381	2010-07-04 00:00:00	55015.1437268518	2009-07-03 03:26:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040009	The combined actions of fast stellar winds and core-collapse supernova explosions of the massive stars create large shell-like structures, called superbubbles (SBs), by sweeping up the ambient medium. Large tenuous cavities created inside the SB walls allow that the blast shocks of the interior supernova remnants (SNRs) expand rapidly without decelerating for a long time. Therefore, the timescale of efficient cosmic-ray acceleration can be much longer than that of most isolated SNRs. We propose the observations on DEM L 192 and DEM L 205, which are the SBs in the Large Magellanic Cloud, in order to search the large non-thermal SNR shells hidden inside the SBs. They are the strong candidates of the accelerators of the "knee energy" particles.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROYA YAMAGUCHI		JAP	4	AO4	DEM L 192 AND DEM L 205: SUPERBUBBLES IN THE LARGE MAGELLANIC CLOUD	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804010010/	Quick Look
134	A2390	328.3984	17.7035	327.804289	17.467151	337.435653	28.529496	73.96308198	-27.80512015	79.9886	54955.5395486111	2009-05-04 12:56:57	54957.6939583333	2009-05-06 16:39:18	804012010	96.4645	90	96.4645	96.473	0	96.4725	2	2	0	2	1	0	0	85.5386	85.5386	186.1119	1	PROCESSED	57546.5371990741	2016-06-07 12:53:34	55343	2010-05-27 00:00:00	54976.1695023148	2009-05-25 04:04:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040011	We propose Suzaku observations of two massive clusters with different radio morphologies, A2219 and A2390, to search for extremely hot (~25 keV) thermal gas. Because of the presence of hot regions indicated in X-ray temperature maps as well as extended radio halo emission, they are the best candidates hosting strongly heated gas due to the past mergers. With the Suzaku broad-band spectroscopy, we can examine properties of very hot gas with high accuracy, and also put constraints on non-thermal emission. This study can only be achieved by the Suzaku's excellent sensitivity to spectral observations over the wide band, and will bring us new insights into physics of gas heating in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NAOMI OTA		JAP	4	AO4	SEARCH FOR EXTREMELY HOT GAS IN TWO MASSIVE GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804012010/	Quick Look
135	FERMI_0265	187.8001	-14.1665	187.150388	-13.890445	192.786887	-9.914495	295.53023761	48.41419063	294.2648	55020.9540277778	2009-07-08 22:53:48	55021.5418981482	2009-07-09 13:00:20	804017010	26.3115	80	26.3115	26.3115	0	26.3115	2	2	0	2	1	0	0	22.8463	22.8463	50.7879	1	PROCESSED	57547.7938773148	2016-06-08 19:03:11	55422	2010-08-14 00:00:00	55034.2333217593	2009-07-22 05:35:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040014	We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JUN KATAOKA		JAP	4	AO4	SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804017010/	Quick Look
136	FERMI_0459	304.3461	6.0496	303.729476	5.893761	308.253181	25.044638	48.6197877	-16.02859504	257.4741	55131.4269097222	2009-10-27 10:14:45	55132.2224189815	2009-10-28 05:20:17	804020010	32.8128	30	32.8128	32.8128	0	32.8128	2	2	0	2	1	0	0	28.6251	28.6251	68.7259	0	PROCESSED	57549.0265046296	2016-06-10 00:38:10	55513	2010-11-13 00:00:00	55149.4269791667	2009-11-14 10:14:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040014	We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JUN KATAOKA		JAP	4	AO4	SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804020010/	Quick Look
137	A2029_4	228.0053	5.6496	227.385284	5.836972	223.833276	22.612919	6.60771448	50.27207577	112.9543	55225.6146180556	2010-01-29 14:45:03	55226.2501388889	2010-01-30 06:00:12	804024040	25.6584	22	25.6584	25.6824	0	25.6664	2	2	0	2	1	0	0	19.446	19.446	54.9019	0	PROCESSED	57550.4263657407	2016-06-11 10:13:58	55637	2011-03-17 00:00:00	55271.0446064815	2010-03-16 01:04:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040030	Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUZURU TAWARA		JAP	4	AO4	TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024040/	Quick Look
138	NGC 669	26.8113	35.5683	26.082401	35.319076	38.038857	22.814409	135.52840833	-25.9346715	67.5273	55017.2207523148	2009-07-05 05:17:53	55018.4377777778	2009-07-06 10:30:24	804049010	50.2528	50	50.2608	50.2528	0	50.2608	1	1	0	1	1	0	0	45.4023	45.4023	105.1199	11	PROCESSED	57547.7727430556	2016-06-08 18:32:45	55395	2010-07-18 00:00:00	55029.2656944444	2009-07-17 06:22:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041504	Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio: the Milky Way retained only 30% of its baryons while lower mass galaxies retain less than 10%. Probably, these baryons were expelled by intense galactic winds during the early star formation period at z = 1-3. These galactic winds can carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding two extremely massive spiral galaxies, with 6-8 times the stellar content of M31 and with v_rot = 370, 420 km/s. If successful, we will detect a significant fraction of the 3-4E11 Msun of the missing baryons as hot gas.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JOEL BREGMAN		USA	4	AO4	THE BARYON CONTENT OF MASSIVE SPIRAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804049010/	Quick Look
139	RXJ1159+5531	179.953	55.611	179.309735	55.889319	149.803846	49.191232	137.55848692	60.02702904	317.8793	54953.4172222222	2009-05-02 10:00:48	54955.52875	2009-05-04 12:41:24	804051010	85.4892	75	85.4972	85.4892	0	85.4972	2	2	0	2	1	0	0	82.4128	82.4128	182.4218	2	PROCESSED	57546.517974537	2016-06-07 12:25:53	55343	2010-05-27 00:00:00	54976.1055439815	2009-05-25 02:31:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041514	We propose a 75ks observation of the galaxy group RXJ1159+5531 to place definitive constraints on its gas out to the virial radius (Rvir). These unprecedented measurements will enable us to study the entropy profile at scales near the region in which accretion shocks become important, and will reveal whether its flattening outside the core of the group extends as far as Rvir. Furthermore, we will obtain the mass profile and test the validity of the NFW model in the outer parts of the halo. Due to its high surface brightness and favourable distance, RXJ1159+5531 is the ideal target with which to carry out this study. It will constitute a textbook case for constraining the feedback and other nongravitational processes which shape the distribution of hot gas in galaxy groups.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	PHILIP HUMPHREY		USA	4	AO4	GAS IN A GALAXY GROUP AT THE VIRIAL RADIUS: RXJ1159+5531, A TEXTBOOK EXAMPLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804051010/	Quick Look
140	NGC741MOSAICE_P1	29.7199	5.461	29.066489	5.218433	29.574235	-6.258595	152.014798	-53.55912322	71.7248	55053.8433796296	2009-08-10 20:14:28	55054.0834837963	2009-08-11 02:00:13	804052010	10.8302	10	10.8342	10.8302	0	10.8381	2	2	0	2	1	0	0	7.8627	7.8627	20.74	0	PROCESSED	57548.1137847222	2016-06-09 02:43:51	55448	2010-09-09 00:00:00	55081.2096875	2009-09-07 05:01:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052010/	Quick Look
141	NGC741MOSAICS_P4	29.2193	5.0492	28.567063	4.805449	28.959637	-6.470888	151.55342081	-54.14565062	71.7599	55053.1534259259	2009-08-10 03:40:56	55053.3759143518	2009-08-10 09:01:19	804054040	10.589	10	10.597	10.589	0	10.589	1	1	0	1	1	0	0	9.9689	9.9689	19.1919	0	PROCESSED	57548.09625	2016-06-09 02:18:36	55451	2010-09-12 00:00:00	55084.9935763889	2009-09-10 23:50:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054040/	Quick Look
142	ABELL 426 E1	50.3027	41.5257	49.474155	41.346372	58.885391	22.278944	150.79331238	-13.10366228	89.0025	55041.5144560185	2009-07-29 12:20:49	55041.7141666667	2009-07-29 17:08:24	804056010	9.696	10	9.696	9.696	0	9.696	1	1	0	1	1	0	0	7.856	7.856	17.2479	0	PROCESSED	57547.9587268518	2016-06-08 23:00:34	55419	2010-08-11 00:00:00	55050.256400463	2009-08-07 06:09:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804056010/	Quick Look
143	ABELL 426 E5	51.7975	41.5108	50.964978	41.337079	60.044403	21.962427	151.74947693	-12.48443224	87.0002	55042.7485069444	2009-07-30 17:57:51	55043.2932175926	2009-07-31 07:02:14	804060010	21.649	20	21.649	21.9423	0	21.929	3	2	0	2	1	0	0	22.1391	22.1391	47.0481	0	PROCESSED	57548.0130208333	2016-06-09 00:18:45	55427	2010-08-19 00:00:00	55060.702349537	2009-08-17 16:51:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804060010/	Quick Look
144	ABELL 426 N3	49.4023	42.2033	48.571812	42.020646	58.391407	23.116315	149.83616068	-12.90614214	59.9986	55062.4722106482	2009-08-19 11:19:59	55062.7542708333	2009-08-19 18:06:09	804065010	12.2498	10	12.2498	12.2498	0	12.2498	1	1	0	1	1	0	0	11.8582	11.8582	24.3619	0	PROCESSED	57548.2751157407	2016-06-09 06:36:10	55441	2010-09-02 00:00:00	55074.9931597222	2009-08-31 23:50:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804065010/	Quick Look
145	ABELL 426 N7	48.6285	43.1676	47.793828	42.98212	58.096043	24.202758	148.81295674	-12.39950143	59.9993	55064.6340509259	2009-08-21 15:13:02	55065.4329166667	2009-08-22 10:23:24	804069010	36.4901	30	36.4901	36.5101	0	36.5021	2	2	0	2	1	0	0	30.3696	30.3696	69.018	0	PROCESSED	57548.3120486111	2016-06-09 07:29:21	55441	2010-09-02 00:00:00	55075.0667708333	2009-09-01 01:36:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804069010/	Quick Look
146	RCS0928+3646	142.0898	36.7798	141.319732	36.998258	132.498761	20.704213	186.98438508	46.37223207	116.6063	55148.3222800926	2009-11-13 07:44:05	55149.1064699074	2009-11-14 02:33:19	804080010	36.5167	30	36.5327	36.5167	0	36.5327	2	2	0	2	1	0	0	27.0584	27.0584	67.7439	1	PROCESSED	57549.3099652778	2016-06-10 07:26:21	55546	2010-12-16 00:00:00	55180.0365972222	2009-12-15 00:52:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041525	Understanding relationships between baryons in galaxy clusters and the underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a cluster sample chosen independently of X-ray properties. We propose to study 14 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Chandra observations of 8 high-dispersion, low-z targets. Suzaku s superior throughput is required to probe the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 6 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AMALIA HICKS		USA	4	AO4	DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804080010/	Quick Look
147	A1795_FAR_NORTHEAST	207.4803	26.8793	206.904436	27.126887	194.02783	35.343989	35.17669327	76.97815393	300.5693	55010.6105439815	2009-06-28 14:39:11	55011.5556712963	2009-06-29 13:20:10	804082010	40.0263	35	40.0263	40.0263	0	40.0263	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57547.6967476852	2016-06-08 16:43:19	55395	2010-07-18 00:00:00	55026.4466087963	2009-07-14 10:43:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041528	The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	4	AO4	ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804082010/	Quick Look
148	A1795_FAR_WEST	206.824	26.695	206.246184	26.94403	193.479611	34.924294	34.12189199	77.54661564	300.5663	55008.5840625	2009-06-26 14:01:03	55009.4634143518	2009-06-27 11:07:19	804084010	35.4763	35	35.4843	35.4763	0	35.4843	2	2	0	2	1	0	0	30.3466	30.3466	75.9378	1	PROCESSED	57547.7077662037	2016-06-08 16:59:11	55395	2010-07-18 00:00:00	55022.2936458333	2009-07-10 07:02:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041528	The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	4	AO4	ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804084010/	Quick Look
149	A478 OFFSET C	63.6328	10.5074	62.946361	10.382264	63.629527	-10.552687	182.59008129	-28.04907037	259.6787	55604.2488888889	2011-02-12 05:58:24	55605.3522685185	2011-02-13 08:27:16	805003010	47.1486	45	47.1646	47.1486	0	47.1646	2	2	0	2	1	0	0	39.9898	39.9898	95.3198	2	PROCESSED	57600.9430671296	2016-07-31 22:38:01	55983	2012-02-26 00:00:00	55617.4134490741	2011-02-25 09:55:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050008	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 a representative regular cluster, Abell 478	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA	ANDREW FABIAN	JAP	5	AO5	DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805003010/	Quick Look
150	RXCJ0013.2-4905	3.3206	-49.1017	2.696864	-49.379799	337.855034	-45.122753	318.93482177	-66.82406097	263.5597	55565.2569328704	2011-01-04 06:09:59	55565.4036689815	2011-01-04 09:41:17	805023010	8.432	10	8.432	8.432	0	8.432	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57600.5421875	2016-07-31 13:00:45	56016	2012-03-30 00:00:00	55627.5157638889	2011-03-07 12:22:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050021	We propose Suzaku observations of 5 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. Since some of the targets are to be observed in the AO4, we request an additional exposure for the remaining clusters to complete the program. With a short exposure time of 10 ks per cluster, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	5	AO5	LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805023010/	Quick Look
151	A2199 EAST OFFSET	246.7666	40.2374	246.342386	40.34813	232.073247	60.652123	63.87682573	44.00920476	240.0015	55458.2941666667	2010-09-19 07:03:36	55459.7155324074	2010-09-20 17:10:22	805042010	58.4398	60	58.4399	58.4398	0	58.4398	3	2	0	2	1	0	0	52.5076	52.5076	122.7919	1	PROCESSED	57553.4778935185	2016-06-14 11:28:10	55836	2011-10-02 00:00:00	55470.1049884259	2010-10-01 02:31:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050081	We propose to observe the virial radius region of the cluster of galaxies A2199 (z=0.0309) over the virial radius. This cluster lies in the Great Wall, and a cosmic filament runs from north to south. We aim to explore possible influence from the filament gives onto the formation process of the cluster, by comparing the hot-gas density and temperature around the virial radius in parallel and vertical directions to the filament. With the high sensitivity of XIS to faint extended emission, we expect to detect denser and hotter gas in the filement even outside the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	HIROKI AKAMATSU		JAP	5	AO5	TEMPERATURE OVER THE VIRIAL RADIUS OF ABELL 2199, AND INFLUENCE OF THE LARGE-SCALE STRUCTURE.	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805042010/	Quick Look
152	VIRGOHI 21	184.472	14.7597	183.83671	15.037342	178.086194	15.290258	268.97789082	75.3718003	123.3105	55535.5218518518	2010-12-05 12:31:28	55537.7911574074	2010-12-07 18:59:16	805054010	103.1915	100	103.3995	103.1915	0	103.3995	2	2	0	2	1	0	0	81.9209	81.9209	196.0168	4	PROCESSED	57554.4175694444	2016-06-15 10:01:18	55916	2011-12-21 00:00:00	55550.3035185185	2010-12-20 07:17:04	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050114	We propose a 100 ksec observation of "VIRGOHI 21" in the Virgo galaxy cluster. VIRGOHI 21 with no optical counterpart, is called a "dark galaxy" from the presence of velocity informed gas clouds with 21-cm observations somewhat like a disk galaxy. Origins are said to be traces of density fluctuation at cluster birth, or gas stripped from galaxies, but nothing clear is yet not introduced. Using the energy resolution of the XIS, we would like to explain the origin, deciding heavy element abundances of VIRGOHI 21. Extremely low abundance will give us the first "dark galaxy". Discovery of a "dark galaxy" with its information of prehistoric universe, will lead us to not just galaxy evolution, but also mighty mechanisms to understand cosmology, giving great impact to astrophysics itself.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	RYO IIZUKA		JAP	5	AO5	X-RAY SEARCH FOR A DARK GALAXY IN THE VIRGO CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805054010/	Quick Look
153	A2204_FIELD_2	248.1003	5.3993	247.484152	5.504515	245.364183	26.985557	20.85022945	33.23419381	260.9996	55435.6212615741	2010-08-27 14:54:37	55436.6744675926	2010-08-28 16:11:14	805057010	39.7312	40	39.7392	39.7312	0	39.7421	2	2	0	2	1	0	0	35.3157	35.3157	90.9818	1	PROCESSED	57553.2244444445	2016-06-14 05:23:12	55287	2010-04-01 00:00:00	55449.2310416667	2010-09-10 05:32:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805057010/	Quick Look
154	A1413_FIELD_1	178.851	23.2234	178.207267	23.50167	169.288709	20.757468	226.97411288	76.74388731	303.0003	55345.0808333333	2010-05-29 01:56:24	55346.139849537	2010-05-30 03:21:23	805059010	40.2041	40	40.2041	40.2041	0	40.2041	2	2	0	2	1	0	0	34.564	34.564	91.4919	1	PROCESSED	57551.6776041667	2016-06-12 16:15:45	55287	2010-04-01 00:00:00	55365.2529513889	2010-06-18 06:04:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805059010/	Quick Look
155	NGC5129 OFF-CENTER2	201.1253	13.7341	200.509035	13.994301	194.045924	20.91983	334.52733324	74.54035563	127.8098	55548.7900810185	2010-12-18 18:57:43	55549.42875	2010-12-19 10:17:24	805073010	30.7651	30	30.7811	30.7651	0	30.7811	2	2	0	2	1	0	0	25.2475	25.2475	55.168	0	PROCESSED	57554.4510416667	2016-06-15 10:49:30	55960	2012-02-03 00:00:00	55593.1036805556	2011-02-01 02:29:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051512	Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	XINYU DAI		USA	5	AO5	BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805073010/	Quick Look
156	NGC5129 BACKGROUND	201.7433	13.5725	201.127421	13.831619	194.704871	21.009611	336.16988197	74.1046924	116.4041	55547.7947106482	2010-12-17 19:04:23	55548.0397106482	2010-12-18 00:57:11	805074010	12.2767	10	12.2767	12.2847	0	12.2927	2	2	0	2	1	0	0	10.7811	10.7811	21.16	0	PROCESSED	57554.4321180556	2016-06-15 10:22:15	55960	2012-02-03 00:00:00	55592.9616435185	2011-01-31 23:04:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051512	Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	XINYU DAI		USA	5	AO5	BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805074010/	Quick Look
157	ESO3060170 OFFSET	85.0343	-41.2366	84.63691	-41.261684	81.30371	-64.529199	246.8664627	-30.36071331	321.0164	55326.497025463	2010-05-10 11:55:43	55327.7204166667	2010-05-11 17:17:24	805076010	78.6782	80	78.6782	78.6862	0	78.6862	2	2	0	2	1	0	0	69.7827	69.7827	105.6858	1	PROCESSED	57551.4828240741	2016-06-12 11:35:16	55707	2011-05-26 00:00:00	55341.5427893518	2010-05-25 13:01:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051513	We propose 30 and 80 ksec observations of the X-ray brightest fossil group, ESO 3060170. The target pointings will reach to 75% of the virial radius from the center of the galaxy, in order to determine the temperature and metal abundances of group gas at large radii. This will allow us to determine the radial profiles of the gaseous iron mass to stellar light ratio, the relative distributions of ejecta from SN Ia and SN II, the entropy, the total mass to light ratio, and the dark matter concentration for this fossil group. The energy resolution and low background of the XIS instrument are crucial for this study, which will help constrain the evolutional history of this fossil group and tell us how fossil groups relate to normal groups and clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YUANYUAN SU		USA	5	AO5	HOW DO FOSSIL GROUPS OF GALAXIES DIFFER FROM NORMAL GROUPS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805076010/	Quick Look
158	PKS 0745-191	116.7033	-18.9048	116.14781	-18.780899	123.330634	-39.304661	236.01965558	3.07990407	294.0011	55315.865462963	2010-04-29 20:46:16	55316.6418518518	2010-04-30 15:24:16	805084010	34.8356	35	34.8356	34.8356	0	34.8356	2	2	0	2	1	0	0	29.5067	29.5067	67.0759	1	PROCESSED	57551.3211458333	2016-06-12 07:42:27	55696	2011-05-15 00:00:00	55330.1469675926	2010-05-14 03:31:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051526	Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MATTHEW GEORGE		USA	5	AO5	BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805084010/	Quick Look
159	RCS2343-3517	355.9933	-35.2927	355.337628	-35.570369	340.879701	-30.492367	359.21699124	-73.45928386	237.6557	55523.8239930556	2010-11-23 19:46:33	55525.0418171296	2010-11-25 01:00:13	805088010	48.3167	61	48.3167	48.3167	0	48.3167	2	2	0	2	1	0	0	40.1454	40.1454	105.1859	1	PROCESSED	57554.2088078704	2016-06-15 05:00:41	55903	2011-12-08 00:00:00	55537.0179861111	2010-12-07 00:25:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051527	Understanding relationships between baryons in galaxy clusters and underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a sample chosen independently of X-ray properties. We propose to study 13 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Suzaku/Chandra observations of 11 high-dispersion, low-z targets. Suzaku's superior throughput is required to complete the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 2 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	5	AO5	DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805088010/	Quick Look
160	NGC 1332	51.5732	-21.333	51.017829	-21.507123	42.191625	-38.615675	212.17958034	-54.36451308	243.6482	55581.2509027778	2011-01-20 06:01:18	55584.0883333333	2011-01-23 02:07:12	805095010	101.423	100	101.423	101.423	0	101.423	2	2	0	2	1	0	0	89.9683	89.9683	245.1259	2	PROCESSED	57600.7603935185	2016-07-31 18:14:58	55965	2012-02-08 00:00:00	55599.216724537	2011-02-07 05:12:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	054502	Recent observations of relaxed galaxy groups have revealed ubiquitous abundance gradients. The broad peaks of Fe abundance indicate (turbulent) diffusion of metals possibly driven by AGN feedback. Exploiting the low background and good sensitivity of Suzaku XIS, we have found similar gradients in three lower mass (virial mass 5-10E12 Msun) elliptical galaxies, which has important implications for models of feedback and chemical enrichment. We propose to observe another two carefully chosen galaxies, thus starting to build a sample for determining the frequency and properties of such abundance gradients in early-type galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	PHILIP HUMPHREY	RYO NAGINO	USJ	5	AO5	ABUNDANCE GRADIENTS IN EARLY-TYPE GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805095010/	Quick Look
161	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
162	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
163	SNR B0532-675	83.0766	-67.535	83.105131	-67.568522	336.894388	-87.135778	277.71335978	-32.44457154	140.0497	55871.6295601852	2011-11-06 15:06:34	55874.1570601852	2011-11-09 03:46:10	806007010	82.4909	80	82.4909	82.4909	0	82.4909	2	2	0	2	1	0	0	77.4573	77.4573	218.3547	4	PROCESSED	57603.7734027778	2016-08-03 18:33:42	56257	2012-11-26 00:00:00	55890.6997337963	2011-11-25 16:47:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060025	Interstellar medium (ISM) heated by a forward shock of supernova remnants (SNRs) gives us a unique opportunity to study local metal abundance and density. Systematic study of the shock-heated ISM in a galaxy unveils its overall metal distribution and provides a key to understand its chemical evolution. On the basis of this idea, we have performed observations of SNRs in the Large Magellanic Cloud (LMC). We here propose to observe the LMC SNR B0532-675 for 80 ks. Since it locates near the star formation region LH76, we expect that we can study the process of metal diffusion from a star forming region by utilizing the result from another SNR DEM L241 near LH76 already observed.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KENTARO SOMEYA		JAP	6	AO6	STUDY OF CHEMICAL EVOLUTION OF THE LARGE MAGELLANIC CLOUD WITH SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806007010/	Quick Look
164	XMMU 2235.3-2557	338.8435	-25.9657	338.152793	-26.224773	330.62189	-15.821353	27.27021923	-59.64080614	244.5944	55878.6378125	2011-11-13 15:18:27	55881.5577777778	2011-11-16 13:23:12	806013010	101.1227	100	101.1227	101.1227	0	101.1227	2	2	0	2	1	0	0	90.6244	90.6244	252.2417	4	PROCESSED	57603.8656481482	2016-08-03 20:46:32	56257	2012-11-26 00:00:00	55890.7014583333	2011-11-25 16:50:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060038	Galaxy clusters at high redshift are useful as a cosmological probe that have a potential to constrain the inflation theory via its mass function. A massive cluster, XMMU 2235.3-2557 found at z=1.4 is especially important because the presence itself should be quite rare if the standard theory with the Gaussian random field is correct. However, there can be a lot of systematic errors of the mass estimates, that is, the temperature measurement of the cluster. Hence, we propose an independent measurement of X-ray spectroscopic temperature by SUZAKU.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	HAJIME KAWAHARA		JAP	6	AO6	TEMPERATURE MEASUREMENT OF A MASSIVE HIGH-Z CLUSTER XMMU 2235.3-2557 BY SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806013010/	Quick Look
165	ABELL 773	139.2619	51.6127	138.389122	51.822209	124.54102	33.911668	166.27594696	43.26641657	277.0001	55684.0736342593	2011-05-03 01:46:02	55684.909212963	2011-05-03 21:49:16	806027030	47.578	50	47.578	47.578	0	47.578	2	2	0	2	1	0	0	44.1095	44.1095	72.1819	0	PROCESSED	57601.9127083333	2016-08-01 21:54:18	55652	2011-04-01 00:00:00	55697.2793518518	2011-05-16 06:42:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806027030/	Quick Look
166	ABELL 1068	160.1718	40.1411	159.449793	40.402342	145.494968	29.227943	178.75085582	60.06234552	130.0011	55860.7020601852	2011-10-26 16:50:58	55861.8821527778	2011-10-27 21:10:18	806028010	51.9826	50	51.9906	51.9826	0	51.9826	2	2	0	2	1	0	0	44.5347	44.5347	101.9378	1	PROCESSED	57603.6168981482	2016-08-03 14:48:20	55652	2011-04-01 00:00:00	55874.1455324074	2011-11-09 03:29:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806028010/	Quick Look
167	ABELL 2667	358.0843	-26.1324	357.438238	-26.410641	347.261091	-23.090967	33.89369276	-76.76238411	64.8814	55725.7013773148	2011-06-13 16:49:59	55726.9814351852	2011-06-14 23:33:16	806029040	51.7936	50	51.7936	51.8161	0	51.8016	2	2	0	2	1	0	0	43.6427	43.6427	110.5818	1	PROCESSED	57602.3116319444	2016-08-02 07:28:45	55652	2011-04-01 00:00:00	55757.7024652778	2011-07-15 16:51:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806029040/	Quick Look
168	COMA OUTSKIRTS1	196.4834	28.9037	195.885803	29.171019	182.42683	32.834582	62.80265316	86.34142243	115.9997	55900.1880092593	2011-12-05 04:30:44	55901.4341203704	2011-12-06 10:25:08	806020010	48.334	50	48.334	48.334	0	48.334	2	2	0	2	1	0	0	42.2514	42.2514	107.6538	0	PROCESSED	57604.0541898148	2016-08-04 01:18:02	56282	2012-12-21 00:00:00	55914.2892013889	2011-12-19 06:56:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060099	In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKUYA SATO		JAP	6	AO6	STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806020010/	Quick Look
169	COMA OUTSKIRTS4	193.3444	28.9037	192.738609	29.174872	179.533604	31.586326	109.48887466	88.17367696	116.0002	55902.7178125	2011-12-07 17:13:39	55903.9105324074	2011-12-08 21:51:10	806023010	51.6563	50	51.6643	51.6563	0	51.6713	2	2	0	2	1	0	0	49.0198	49.0198	103.0419	1	PROCESSED	57604.0840972222	2016-08-04 02:01:06	56284	2012-12-23 00:00:00	55915.2433449074	2011-12-20 05:50:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060099	In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKUYA SATO		JAP	6	AO6	STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806023010/	Quick Look
170	COMA E4	196.1292	27.8947	195.52895	28.162497	182.637315	31.793754	48.48781449	87.00057059	279.9984	55729.6868287037	2011-06-17 16:29:02	55730.3355671296	2011-06-18 08:03:13	806033010	20.2023	20	20.2023	20.2103	0	20.2183	2	2	0	2	1	0	0	20.516	20.516	56.0419	1	PROCESSED	57602.3427199074	2016-08-02 08:13:31	55652	2011-04-01 00:00:00	55770.1680092593	2011-07-28 04:01:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806033010/	Quick Look
171	BEYOND VIRGO 1	187.7129	16.0953	187.082675	16.371354	180.479874	17.795652	278.48728746	77.9786094	118.4704	55905.1491666667	2011-12-10 03:34:48	55905.8431828704	2011-12-10 20:14:11	806060010	22.2598	20	22.2678	22.2678	0	22.2598	2	2	0	2	1	0	0	20.63	20.63	59.9539	1	PROCESSED	57604.1022569444	2016-08-04 02:27:15	56284	2012-12-23 00:00:00	55917.0698958333	2011-12-22 01:40:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061523	To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORBERT WERNER		USA	6	AO6	LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806060010/	Quick Look
172	BEYOND VIRGO 2	187.7135	16.3643	187.083459	16.640353	180.363309	18.040696	277.98453264	78.22684296	118.4711	55905.8436574074	2011-12-10 20:14:52	55906.3980439815	2011-12-11 09:33:11	806061010	21.4115	20	21.4275	21.4115	0	21.4335	1	1	0	1	1	0	0	19.1816	19.1816	47.872	1	PROCESSED	57604.0951041667	2016-08-04 02:16:57	56284	2012-12-23 00:00:00	55917.0723842593	2011-12-22 01:44:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061523	To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORBERT WERNER		USA	6	AO6	LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806061010/	Quick Look
173	BEYOND VIRGO 6	187.7152	17.4312	187.085892	17.70725	179.897096	19.011602	275.76419982	79.20143703	118.777	55919.8968287037	2011-12-24 21:31:26	55920.9286574074	2011-12-25 22:17:16	806065010	39.5769	40	39.6169	39.5769	0	39.6169	1	1	0	1	1	0	0	33.7703	33.7703	89.136	2	PROCESSED	57604.2337962963	2016-08-04 05:36:40	56339	2013-02-16 00:00:00	55972.6645833333	2012-02-15 15:57:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061523	To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORBERT WERNER		USA	6	AO6	LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806065010/	Quick Look
174	LOCK-365	161.9095	57.7105	161.128548	57.974475	136.113511	45.200495	149.74973686	52.48617693	106.5217	55897.0768981482	2011-12-02 01:50:44	55900.1780439815	2011-12-05 04:16:23	806077010	149.9102	150	149.9422	149.9102	0	149.9422	2	2	0	2	1	0	0	131.1259	131.1259	267.9076	0	PROCESSED	57604.1079050926	2016-08-04 02:35:23	56065	2012-05-18 00:00:00	55914.3640393518	2011-12-19 08:44:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061532	We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	6	AO6	OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806077010/	Quick Look
175	RCS051838-4324.9	79.6593	-43.4168	79.277976	-43.467716	71.171582	-66.18535	248.71475233	-34.61566895	286.4929	56016.4337268518	2012-03-30 10:24:34	56018.0001388889	2012-04-01 00:00:12	806083010	67.6666	75	67.6906	67.6666	0	67.6906	2	2	0	2	1	0	0	57.511	57.511	135.2938	1	PROCESSED	57605.0718402778	2016-08-05 01:43:27	56399	2013-04-17 00:00:00	56027.1518287037	2012-04-10 03:38:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061533	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	6	AO6	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806083010/	Quick Look
176	A3526	191.7105	-40.5689	191.023079	-40.2959	208.274178	-32.365083	301.98862911	22.29443097	109.9992	55942.9777314815	2012-01-16 23:27:56	55943.2362847222	2012-01-17 05:40:15	806086010	13.6391	12	13.6471	13.6471	0	13.6391	1	1	0	1	1	0	0	11.41	11.41	22.3279	0	PROCESSED	57604.3734606482	2016-08-04 08:57:47	56352	2013-03-01 00:00:00	55985.0806944444	2012-02-28 01:56:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806086010/	Quick Look
177	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
178	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
179	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
180	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
181	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
182	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
183	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
184	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
185	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
186	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
187	A3581_CEN	211.9083	-27.0199	211.193684	-26.782616	219.008869	-13.266139	323.17769244	32.83870198	117.8993	56308.5541782407	2013-01-16 13:18:01	56310.7078356482	2013-01-18 16:59:17	807026010	80.408	80	80.416	80.416	0	80.408	2	2	0	2	1	0	0	70.1715	70.1715	186.0419	1	PROCESSED	57608.5784259259	2016-08-08 13:52:56	56711	2014-02-23 00:00:00	56345.6637384259	2013-02-22 15:55:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070064	We propose to study the metallicity of Abell 3581 to the outer region beyond 0.5 r180. Abell 3581 is a very useful system for investigating the history of the chemical evolution of groups and clusters, because the temperature of the intra-cluster medium is about 1.7 keV, which is intermediate between groups and clusters of galaxies. Suzaku will enable us to measure for the first time the metal distributions to such outer regions of the clusters, because of the significantly lower background level and higher sensitivity below ~1 keV.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KOSUKE SATO		JAP	7	AO7	SEARCH FOR THE METALLICITY OF ABELL 3581 TO THE OUTER REGION BEYOND 0.5 R180	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807026010/	Quick Look
188	A2061_2	230.6122	30.8661	230.100044	31.043682	216.595507	47.269453	48.57175305	56.92431824	121.1842	56307.485625	2013-01-15 11:39:18	56308.5460185185	2013-01-16 13:06:16	807030010	41.788	40	41.788	41.788	0	41.788	2	2	0	2	1	0	0	37.7529	37.7529	91.6018	1	PROCESSED	57608.5263888889	2016-08-08 12:38:00	56707	2014-02-19 00:00:00	56338.5482291667	2013-02-15 13:09:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070070	We propose to conduct multi-pointing observations to cover the entire region of A2061 hosting radio relic. We discovered that the radio relic is located in the cluster outskirts of the opposite side of the filamentary large-scale structure. We found the same trend for 3 relic clusters compiling NVSS radio and SDSS optical data-sets, though the sample number is small. It suggests that an universal process to form radio relic potentially exists. We therefore aim to map out the temperature, density, pressure, and entropy of the intra-cluster medium (ICM) to understand the interplays among the large-scale structure, the ICM and radio relic. Our study provides us a comprehensive picture of the ICM in the radio relic cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NOBUHIRO OKABE		JAP	7	AO7	SUZAKU OBSERVATION OF THE OUTSKIRTS IN RADIO RELIC CLUSTER A2061	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807030010/	Quick Look
189	FG04	121.8798	33.9978	121.078663	34.143156	116.761327	13.47104	187.39667673	29.69857824	274.999	56053.6835648148	2012-05-06 16:24:20	56053.9411921296	2012-05-06 22:35:19	807053010	10.821	10	10.821	10.821	0	10.821	1	1	0	1	1	0	0	11.0766	11.0766	22.2559	0	PROCESSED	57605.3537268518	2016-08-05 08:29:22	56435	2013-05-23 00:00:00	56068.6337152778	2012-05-21 15:12:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071511	Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ELENA D'ONGHIA		USA	7	AO7	SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807053010/	Quick Look
190	RXJ1416.4+2315	214.0475	23.1701	213.473378	23.401516	202.507315	34.451007	25.95045598	70.44211392	293.1172	56123.5919675926	2012-07-15 14:12:26	56124.3335300926	2012-07-16 08:00:17	807065010	23.7192	120	23.7272	23.7192	0	23.7272	1	1	0	1	1	0	0	22.6028	22.6028	64.0639	1	PROCESSED	57606.624537037	2016-08-06 14:59:20	56598	2013-11-02 00:00:00	56144.9996180556	2012-08-05 23:59:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071514	Our study of the fossil group RXJ 1159+5531 does not find the gas clumping invoked to explain unexpectedly flat entropy profiles and large gas fractions near r_vir in some clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation, which may reflect that hydrostatic equilibrium is very accurate in this highly evolved fossil group. To examine whether these results extend to other fossils and to more massive systems, we propose to observe the fossil cluster RXJ 1416.4+2315 (M_vir ~3 x 10^14 M_sun) to constrain its entropy and gas fraction out to r_vir (r_112). Since it is located at a redshift of 0.137, this target provides an efficient means to explore the outer ICM, where a large azimuthal portion (~80%) of r_vir can be observed in a single Suzaku field.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DAVID BUOTE		USA	7	AO7	RXJ1416.4+2315: A MASSIVE FOSSIL CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807065010/	Quick Look
191	NGC 5044 NORTH 30'	199.0992	-15.8941	198.433238	-15.630477	203.627041	-7.241957	311.67530339	46.55349501	110.0017	55220.5889814815	2010-01-24 14:08:08	55222.2571064815	2010-01-26 06:10:14	804013010	62.8482	60	62.8562	62.8482	0	62.8562	2	2	0	2	1	0	0	44.5926	44.5926	144.0998	1	PROCESSED	57550.396099537	2016-06-11 09:30:23	55602	2011-02-10 00:00:00	55235.338587963	2010-02-08 08:07:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040013	Why groups of galaxies contain smaller amount of metals than clusters of galaxies? To study metal sysnthesis history of galaxies in groups, we propose to observe two offset pointings of the NGC 5044 group and HCG 62 to derive metal distribution of intragroup medium up to 0.5 r180. Due to its low background, Suzaku enables us to study regions at low surface brightness.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KYOKO MATSUSHITA		JAP	4	AO4	METAL MASS TO LIGHT RATIOS OF GROUPS OF GALAXIES UP TO 0.5R180	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804013010/	Quick Look
192	ANTLIA E4	158.9815	-35.3293	158.412243	-35.069878	177.109135	-40.308725	274.02289995	19.82417732	279.0004	56094.1885532407	2012-06-16 04:31:31	56095.3688888889	2012-06-17 08:51:12	807069010	46.5031	45	46.5031	46.5195	0	46.5111	2	2	0	2	1	0	0	38.6185	38.6185	101.9699	0	PROCESSED	57605.7108564815	2016-08-05 17:03:38	56477	2013-07-04 00:00:00	56111.0445023148	2012-07-03 01:04:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071521	We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	7	AO7	MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807069010/	Quick Look
193	ABELL 2597	351.5123	-12.2071	350.862263	-12.482246	347.371921	-7.852378	65.46064183	-65.03980804	250.0004	56263.5374884259	2012-12-02 12:53:59	56264.7744907407	2012-12-03 18:35:16	807073030	50.2983	50	50.3063	50.2983	0	50.2983	2	2	0	2	1	0	0	42.3364	42.3364	106.8558	0	PROCESSED	57608.190625	2016-08-08 04:34:30	56018	2012-04-01 00:00:00	56279.6896180556	2012-12-18 16:33:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073030/	Quick Look
194	RCS022456-0348.8	36.2382	-3.8143	35.608784	-4.039767	32.599151	-17.199331	170.77871975	-57.71972182	253.341	56324.4414814815	2013-02-01 10:35:44	56325.9579282407	2013-02-02 22:59:25	807078010	50.8118	49	50.8227	50.8147	0	50.8118	2	2	0	2	1	0	0	46.195	46.195	131.0078	0	PROCESSED	57610.5290509259	2016-08-10 12:41:50	56711	2014-02-23 00:00:00	56345.5401967593	2013-02-22 12:57:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071525	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	7	AO7	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807078010/	Quick Look
195	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
196	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
197	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
198	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
199	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
200	A401EAST	45.0348	13.3366	44.348124	13.13869	46.452106	-3.5684	164.66710088	-38.88860633	71.9996	56530.5043055556	2013-08-26 12:06:12	56531.6841782407	2013-08-27 16:25:13	808006010	51.6628	50	51.6868	51.6628	0	51.6868	2	2	0	2	1	0	0	47.8099	47.8099	101.9238	1	PROCESSED	57612.4270138889	2016-08-12 10:14:54	56956	2014-10-26 00:00:00	56587.515474537	2013-10-22 12:22:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080004	To investigate (i)the influence of the merging event on IntraCluster Medium (ICM), We propose 40 ks+50 ks ~2 =140 ks observations of the linked region between Abell 399 and Abell 401. A399 (z=0.0724) and A401 (z=0.0737) are expected be in the initial phase of a cluster merger. With Suzaku fs high sensitivity observations, we will (i)determine the ICM physical conditions by measuring the temperature and density distribution, (ii) characterize the dynamical state of the cluster linked region, (iii) confirm the presence of a shock front predicted by numerical simulations. Our study will reveal the nature of initial phase of merging event of clusters of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHITAKA ISHISAKI		JAP	8	AO8	MORPHOLOGY AND PHYSICAL PROPERTIES OF SHOCKED GAS BY MAJOR MERGER IN THE LINKED REGION OF ABELL 399 AND ABELL 401	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808006010/	Quick Look
201	COMA SUBHALO3	193.9804	27.7549	193.374568	28.025359	180.724315	30.814588	65.39722549	88.82429581	314.9967	56453.0272569444	2013-06-10 00:39:15	56453.5912384259	2013-06-10 14:11:23	808021010	24.0441	20	24.0521	24.0441	0	24.0521	2	2	0	2	1	0	0	25.5334	25.5334	48.6979	0	PROCESSED	57611.5202199074	2016-08-11 12:29:07	56872	2014-08-03 00:00:00	56506.7633101852	2013-08-02 18:19:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080023	We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NOBUHIRO OKABE		JAP	8	AO8	SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808021010/	Quick Look
202	COMA NW3	194.5571	28.6697	193.954123	28.93948	180.77176	31.860187	79.10101688	87.84902047	319.997	55732.646099537	2011-06-20 15:30:23	55732.9793865741	2011-06-20 23:30:19	806040010	10.469	10	10.469	10.469	0	10.469	2	2	0	2	1	0	0	10.1768	10.1768	28.7899	0	PROCESSED	57602.3615856482	2016-08-02 08:40:41	55652	2011-04-01 00:00:00	55768.2657523148	2011-07-26 06:22:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806040010/	Quick Look
203	A2255_NW	258.0206	64.3236	257.946874	64.381524	198.635574	84.547798	94.26240936	34.95584628	200.0017	56613.0157060185	2013-11-17 00:22:37	56613.9467476852	2013-11-17 22:43:19	808039010	43.7688	40	43.7688	43.7688	0	43.7688	2	2	0	2	1	0	0	41.8557	41.8557	80.4121	0	PROCESSED	57613.3414814815	2016-08-13 08:11:44	56991	2014-11-30 00:00:00	56625.6806481482	2013-11-29 16:20:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080047	We propose to obtain high-quality X-ray spectra of two subcluster regions in A2255 aiming at detection of supersonic motion of the intracluster gas. Previous optical and X-ray observations suggest that A2255 is indeed in the process of merging and subclusters have high velocities relative to the main cluster. Utilizing the high-sensitivity Suzaku spectroscopy, the line-of-sight velocity of the X-ray emitting gas can be measured from the Doppler shift of iron-K lines. With additional 40ks/80ks observations of the NW/SE subclusters, we expect to detect significant bulk velocities for the first time in this cluster. This will enhance our understanding of the 3-dimensional structure of the object including line-of-sight gas velocities and the cluster dynamical evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	HIROKO YOSHIDA		JAP	8	AO8	MAPPING GAS MOTIONS IN THE MERGING CLUSTER A2255	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808039010/	Quick Look
204	BULLET-OFFSET2	104.4232	-55.8309	104.179615	-55.762127	129.485135	-77.282926	265.86935635	-21.32349548	287.0017	56419.6209722222	2013-05-07 14:54:12	56422.4605439815	2013-05-10 11:03:11	808056010	101.3855	100	101.3935	101.3935	0	101.3855	2	2	0	2	1	0	0	93.6767	93.6767	245.3058	2	PROCESSED	57611.3171643518	2016-08-11 07:36:43	56799	2014-05-22 00:00:00	56433.6998958333	2013-05-21 16:47:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080080	We propose two offset pointings of the bullet cluster with one adjacent blank-sky pointing. By detecting a very hot component in the ICM and mapping temperature/entropy out to the outskirts, we study thermodynamical evolution of the ICM in the course of cluster merger. More specifically, we estimate the fraction of energy injected to the ICM from the energy released by the merger, and the amount of energy heating the ICM through the shock, irreversible process.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	8	AO8	THERMODYNAMICAL EVOLUTION OF THE ICM IN THE BULLET CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808056010/	Quick Look
205	ESO318-021	163.2697	-40.3328	162.69794	-40.066534	184.394245	-42.926152	279.73310675	17.14745123	111.1499	56639.0964467593	2013-12-13 02:18:53	56643.3605902778	2013-12-17 08:39:15	808063010	152.2198	150	152.2198	152.2198	0	152.2198	2	2	0	2	1	0	0	132.9733	132.9733	368.3777	4	PROCESSED	57613.6558101852	2016-08-13 15:44:22	57050	2015-01-28 00:00:00	56680.7667476852	2014-01-23 18:24:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081503	The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	DAVID BUOTE		USA	8	AO8	THE DARK MATTER AND BARYON PROFILES OF ISOLATED ELLIPTICAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808063010/	Quick Look
206	RXJ1416.4+2315	214.0623	23.3458	213.488767	23.577175	202.437112	34.617457	26.46691952	70.47697816	292.671	56496.6431712963	2013-07-23 15:26:10	56499.3349074074	2013-07-26 08:02:16	808064010	122.9317	120	122.9317	122.9317	0	122.9317	2	2	0	2	1	0	0	116.8226	116.8226	232.5474	2	PROCESSED	57612.032650463	2016-08-12 00:47:01	56953	2014-10-23 00:00:00	56587.4880671296	2013-10-22 11:42:49	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081511	Our preliminary analysis of AO7 XIS data of the fossil cluster RXJ 1416.4+2315 does not find evidence for the gas clumping invoked to explain the flat entropy profiles and large gas fractions found near r_vir in several nearby clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation as we found previously for the fossil group/cluster RXJ 1159+5531, which may reflect that hydrostatic equilibrium is very accurate in these highly evolved fossil systems. Therefore, we propose a Suzaku observation in a different azimuthal direction to double the azimuthal coverage at r_vir (from ~30% to ~60%) in order to test for the presence of azimuthal ICM variations expected for clusters that grow by accretion along large-scale filaments.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	DAVID BUOTE		USA	8	AO8	VERIFYING RELAXED ICM AT THE VIRIAL RADIUS IN A FOSSIL GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808064010/	Quick Look
207	MKW-N2	181.1507	2.5267	180.510236	2.805064	180.047061	2.775514	276.44275792	62.96433079	120.2659	56663.6701967593	2014-01-06 16:05:05	56666.0195023148	2014-01-09 00:28:05	808067010	99.7883	100	99.7883	99.7883	0	99.7883	2	2	0	2	1	0	0	99.9362	99.9362	202.9537	4	PROCESSED	57613.8221643518	2016-08-13 19:43:55	57096	2015-03-15 00:00:00	56730.5704166667	2014-03-14 13:41:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081512	We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUANYUAN SU		USA	8	AO8	PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808067010/	Quick Look
208	A133_FIELD_2	15.4723	-21.5865	14.860654	-21.855252	5.175152	-25.865615	146.72727626	-83.96930246	231.9996	56646.6689583333	2013-12-20 16:03:18	56647.8294212963	2013-12-21 19:54:22	808082010	50.6406	50	50.6646	50.6566	0	50.6406	2	2	0	2	1	0	0	46.4338	46.4338	100.2559	1	PROCESSED	57613.6561921296	2016-08-13 15:44:55	57061	2015-02-08 00:00:00	56695.6286689815	2014-02-07 15:05:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081525	We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ERIC MILLER		USA	8	AO8	A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808082010/	Quick Look
209	ABELL 1689 (OFFSET)	198.1816	-1.2688	197.539227	-1.003818	197.250037	5.95631	314.01012466	61.14421574	293.5484	56470.3775578704	2013-06-27 09:03:41	56473.3751273148	2013-06-30 09:00:11	808089010	105.7518	396	105.7598	105.7518	0	105.7518	2	2	0	2	1	0	0	95.0477	95.0477	258.9556	4	PROCESSED	57611.7314930556	2016-08-11 17:33:21	56383	2013-04-01 00:00:00	56523.7467708333	2013-08-19 17:55:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081528	Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	8	AO8	SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089010/	Quick Look
210	ABELL 1689 (OFFSET)	198.1818	-1.2687	197.539427	-1.003718	197.250185	5.956479	314.01056832	61.14428006	293.5484	56473.3751388889	2013-06-30 09:00:12	56475.3022916667	2013-07-02 07:15:18	808089020	67.8003	396	67.8083	67.8003	0	67.8083	2	2	0	2	1	0	0	60.9649	60.9649	166.4698	5	PROCESSED	57611.6944907407	2016-08-11 16:40:04	56383	2013-04-01 00:00:00	56491.6594675926	2013-07-18 15:49:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081528	Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	8	AO8	SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089020/	Quick Look
211	A2877-NORTH	17.5135	-45.1865	16.956259	-45.452478	352.566996	-47.330769	292.51418745	-71.56330592	266.5006	56649.9225810185	2013-12-23 22:08:31	56651.7884027778	2013-12-25 18:55:18	808102010	72.629	70	72.637	72.629	0	72.645	2	2	0	2	1	0	0	69.2641	69.2641	161.1857	0	PROCESSED	57613.7012615741	2016-08-13 16:49:49	57033	2015-01-11 00:00:00	56665.7969097222	2014-01-08 19:07:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082014	We propose to observe the galaxy group A2877 for a combine observation time of 150 ks, with two different pointings. The aim of the project is to obtain temperature and surface brightness profiles out to large radii to constrain entropies. We aim to see if the entropy profile flattens at large radii, which could indicate gas clumping and/or other processes. This would possibly be the first unrelaxed galaxy group whose entropy profile would have been studied in the outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	BHARADWAJ VIJAYSARATHY		EUR	8	AO8	INVESTIGATING THE OUTSKIRTS OF THE UNRELAXED GALAXY GROUP A2877	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808102010/	Quick Look
212	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
213	THE MOON	142.9426	9.1926	142.274308	9.413777	142.279358	-5.167487	223.99367078	39.68355518	285.4008	56784.5840162037	2014-05-07 14:00:59	56784.7155555556	2014-05-07 17:10:24	809001090	4.7558	45	4.7558	4.7558	0	4.7558	2	2	0	2	1	0	0	4.6674	4.6674	11.358	0	PROCESSED	57615.0740277778	2016-08-15 01:46:36	57162	2015-05-20 00:00:00	56796.5977546296	2014-05-19 14:20:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001090/	Quick Look
214	THE MOON	29.2087	11.3221	28.541439	11.078317	31.138176	-0.585907	147.49986562	-48.40533826	73.8007	56857.4028472222	2014-07-19 09:40:06	56857.5265856482	2014-07-19 12:38:17	809001170	5.6621	45	5.6701	5.6621	0	5.6701	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.4102314815	2016-08-15 09:50:44	57239	2015-08-05 00:00:00	56869.612974537	2014-07-31 14:42:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001170/	Quick Look
215	THE MOON	30.7597	12.0224	30.089346	11.782342	32.8056	-0.451848	149.17525918	-47.16814979	73.8003	56857.5278009259	2014-07-19 12:40:02	56857.5974189815	2014-07-19 14:20:17	809001180	3.4386	45	3.4466	3.4386	0	3.4546	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.4120601852	2016-08-15 09:53:22	57239	2015-08-05 00:00:00	56869.6134953704	2014-07-31 14:43:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001180/	Quick Look
216	THE MOON	138.5418	11.2369	137.863994	11.444435	137.511885	-4.561937	219.19555273	36.72863641	105.699	56975.1999768518	2014-11-14 04:47:58	56975.3237615741	2014-11-14 07:46:13	809001200	3.3796	45	3.3796	3.3796	0	3.3796	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7701041667	2016-08-16 18:28:57	57358	2015-12-02 00:00:00	56992.4114699074	2014-12-01 09:52:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001200/	Quick Look
217	THE MOON	141.4013	10.2837	140.728619	10.500242	140.487309	-4.611146	221.84323525	38.83162783	105.6986	56975.4499305556	2014-11-14 10:47:54	56975.5834143518	2014-11-14 14:00:07	809001220	4.2552	45	4.2552	4.2632	0	4.2632	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7742592593	2016-08-16 18:34:56	57358	2015-12-02 00:00:00	56992.4140625	2014-12-01 09:56:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001220/	Quick Look
218	THE MOON	145.8331	9.4283	145.16599	9.657722	144.909334	-4.019227	225.49397113	42.31232043	105.6985	56975.8485300926	2014-11-14 20:21:53	56975.9376388889	2014-11-14 22:30:12	809001250	4.244	45	4.244	4.308	0	4.324	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7786574074	2016-08-16 18:41:16	57358	2015-12-02 00:00:00	56992.4181828704	2014-12-01 10:02:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001250/	Quick Look
219	THE MOON	335.3702	-6.281	334.716283	-6.533427	334.875812	3.693556	56.37004308	-48.74864005	248.3898	56990.2098148148	2014-11-29 05:02:08	56990.3474768518	2014-11-29 08:20:22	809001310	6.2242	45	6.2242	6.2242	0	6.2242	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.4106481482	2016-08-17 09:51:20	57415	2016-01-28 00:00:00	57002.4438541667	2014-12-11 10:39:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001310/	Quick Look
220	THE MOON	340.8235	-5.0226	340.1744	-5.285051	340.39289	2.857324	63.09935011	-52.32405661	251.0714	56990.6104513889	2014-11-29 14:39:03	56990.733587963	2014-11-29 17:36:22	809001340	6.3566	45	6.3566	6.3566	0	6.3566	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.4124537037	2016-08-17 09:53:56	57415	2016-01-28 00:00:00	57007.4026041667	2014-12-16 09:39:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001340/	Quick Look
221	THE MOON	342.4216	-4.2139	341.77438	-4.478841	342.17578	3.00393	65.81829296	-53.01188957	247.9474	56990.7354513889	2014-11-29 17:39:03	56990.8683101852	2014-11-29 20:50:22	809001350	6.3196	45	6.3196	6.3196	0	6.3196	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.4131018518	2016-08-17 09:54:52	57415	2016-01-28 00:00:00	57006.4014699074	2014-12-15 09:38:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001350/	Quick Look
222	A1413	178.8303	23.6485	178.18646	23.926767	169.076487	21.133974	225.18767075	76.86550896	123.0348	53689.8362847222	2005-11-15 20:04:15	53692.5939699074	2005-11-18 14:15:19	800001010	107.8672	100	107.8672	108.0032	107.9472	107.9103	2	2	2	2	1	0	0	102.4315	102.4315	238.2397	7	PROCESSED	57528.0427546296	2016-05-20 01:01:34	54247	2007-05-27 00:00:00	54038.1136689815	2006-10-30 02:43:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001010	No cluster has had its X-ray temperature measured out to the virial radius. Hence no cluster has had it total mass measured using X-ray methods. Typically these measurements extend only to 60% of the virial radius. We propose to perform these measurements for the first time and with high accuracy for the relaxed cluster A1413. The low Suzaku background permits us to make this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	J. HENRY		JAP	0	SWG	CLUSTER TEMPERATURE AND MASS MEASUREMENT TO THE VIRIAL RADIUS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800001010/	Quick Look
223	FORNAX A WEST LOBE	50.4184	-37.1645	49.940428	-37.342839	32.47574	-52.998531	240.1258488	-56.89722719	219.7525	54092.8700462963	2006-12-23 20:52:52	54095.6113888889	2006-12-26 14:40:24	801014010	93.3093	100	93.3093	93.3093	0	93.3093	2	2	0	2	1	0	0	96.3716	96.3716	236.8358	5	PROCESSED	57536.4597569444	2016-05-28 11:02:03	54735	2008-09-26 00:00:00	54111.6821875	2007-01-11 16:22:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010029	We propose Suzaku observations of the Fornax A west radio lobe and the host galaxy. By measuring the inverse-Compton X-ray spectrum from the radio lobe precisely up to 20 keV and comparing with radio observation results, we are able to determine the electron energy spectrum and to derive magnetic field without any assumptions. This will be an important sample to measure the kinetic energy outflow from an active galactic nucleus.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO TASHIRO		JAP	1	AO1	RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801014010/	Quick Look
224	A262 E2	28.9415	35.8688	28.205018	35.624348	39.895398	22.433371	137.29682221	-25.20210685	249.9999	56695.375625	2014-02-07 09:00:54	56696.1043518518	2014-02-08 02:30:16	808113010	33.0569	32	33.0609	33.0569	0	33.0649	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57613.8024884259	2016-08-13 19:15:35	57074	2015-02-21 00:00:00	56709.7139814815	2014-02-21 17:08:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	083002	We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA	NORBERT WERNER	JUS	8	AO8	OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808113010/	Quick Look
225	A3112BG	50.3198	-44.6958	49.891219	-44.874421	26.077848	-59.651808	253.38706356	-55.37551095	204.9994	57009.69125	2014-12-18 16:35:24	57010.2550462963	2014-12-19 06:07:16	809028020	18.3545	15	18.3545	18.3545	0	18.3545	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.5354166667	2016-08-17 12:51:00	57394	2016-01-07 00:00:00	57027.3975	2015-01-05 09:32:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090061	We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KOSUKE SATO		JAP	9	AO9	ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809028020/	Quick Look
226	PKS 0558-504 VIC 1	90.9582	-50.6414	90.657059	-50.637494	92.232149	-74.075703	258.29690544	-27.96668923	6.4262	56825.0805208333	2014-06-17 01:55:57	56826.8543518518	2014-06-18 20:30:16	809034010	52.0132	60	52.0132	52.0132	0	52.0132	2	2	0	2	1	0	0	50.4874	50.4874	153.2479	0	PROCESSED	57615.2996180556	2016-08-15 07:11:27	57233	2015-07-30 00:00:00	56867.5608912037	2014-07-29 13:27:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090086	We have conducted joint analysis of absorption and emission lines toward several targets and successfully constrained temperatures, extents, and densities of the hot gas for each directions. The results are all consistent and indicate the disk-like hot gas with its height of a few kpc from the Galactic plane. However, other research group claimed that the hot gas extends to > 100 kpc and can be a reservoir of the missing baryon. We propose for an observation of the vicinities of PKS 0558-504 in order to limit an extent of the hot gas surrounding our Galaxy and to clinch an argument that the hot gas can be a huge reservoir of the missing baryon.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KAZUHIRO SAKAI		JAP	9	AO9	IS GALACTIC HOT GAS REALLY A HUGE RESERVOIR FOR THE MISSING BARYON?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809034010/	Quick Look
227	NGC 953	37.7955	29.584	37.059252	29.362946	44.923297	13.943505	147.58231113	-28.46974369	250.5565	57059.5397222222	2015-02-06 12:57:12	57063.4376157407	2015-02-10 10:30:10	809055010	150.8191	150	150.8191	150.8671	0	150.8671	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6137037037	2016-08-17 14:43:44	56748	2014-04-01 00:00:00	57107.4400578704	2015-03-26 10:33:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091503	The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^13 m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have complementary Chandra observations.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	DAVID BUOTE		USA	9	AO9	THE DARK MATTER AND BARYON PROFILES OF ISOLATED ELLIPTICAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809055010/	Quick Look
228	FG10	163.7228	55.3656	162.966111	55.632252	139.04941	43.748241	151.60913312	54.78459511	121.1085	56973.8939467593	2014-11-12 21:27:17	56975.0737615741	2014-11-14 01:46:13	809061010	61.1085	60	61.1085	61.2978	0	61.2978	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7792361111	2016-08-16 18:42:06	57444	2016-02-26 00:00:00	57076.4143865741	2015-02-23 09:56:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091512	Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ELENA D'ONGHIA		USA	9	AO9	SCALING RELATIONS OF FOSSIL GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809061010/	Quick Look
229	ABELL 2259	259.9722	27.8097	259.476075	27.85934	255.895749	50.75928	50.52312942	31.25775464	109.9997	57081.1636458333	2015-02-28 03:55:39	57082.4113194445	2015-03-01 09:52:18	809081010	42.2203	42.5	42.2203	43.0443	0	43.1003	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6840509259	2016-08-17 16:25:02	57465	2016-03-18 00:00:00	57091.4611226852	2015-03-10 11:04:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091526	Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	9	AO9	REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809081010/	Quick Look
230	ABELL 2259	260.1067	27.5543	259.609076	27.603301	256.126173	50.518333	50.27658806	31.07091189	109.9997	57083.6006018518	2015-03-02 14:24:52	57084.7258564815	2015-03-03 17:25:14	809081030	44.2468	42.5	44.2468	44.2548	0	44.2548	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.7027314815	2016-08-17 16:51:56	57475	2016-03-28 00:00:00	57107.4892476852	2015-03-26 11:44:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091526	Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	9	AO9	REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809081030/	Quick Look
231	IC1262	263.2444	43.7719	262.868526	43.80553	257.468416	66.917452	69.53148075	32.08557503	39.6325	56784.7266319444	2014-05-07 17:26:21	56784.9377777778	2014-05-07 22:30:24	809103010	8.569	10	8.569	8.569	0	8.569	1	1	0	1	1	0	0	8.943	8.943	18.2319	0	PROCESSED	57615.0791898148	2016-08-15 01:54:02	57166	2015-05-24 00:00:00	56800.6274537037	2014-05-23 15:03:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809103010/	Quick Look
232	NGC 7556	348.9407	-2.3789	348.297581	-2.651844	348.895625	2.187169	76.06549974	-56.282291	247.7522	56983.6865972222	2014-11-22 16:28:42	56984.009837963	2014-11-23 00:14:10	809109010	15.119	15	15.119	15.119	0	15.119	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.8029861111	2016-08-16 19:16:18	57365	2015-12-09 00:00:00	57009.4127777778	2014-12-18 09:54:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809109010/	Quick Look
233	NGC4325	185.7751	10.6242	185.139474	10.901318	181.016229	12.032879	279.57257446	72.19853871	120.2615	56997.2271990741	2014-12-06 05:27:10	56997.680775463	2014-12-06 16:20:19	809110010	17.4681	15	17.4761	17.4681	0	17.4761	1	1	0	1	1	0	0	16.8093	16.8093	39.184	0	PROCESSED	57617.4727083333	2016-08-17 11:20:42	57376	2015-12-20 00:00:00	57010.1165162037	2014-12-19 02:47:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809110010/	Quick Look
234	M82 N1	148.6748	70.0409	147.627175	70.277324	118.519213	52.349642	141.10131259	40.27429686	283.7057	57159.0836921296	2015-05-17 02:00:31	57160.4702546296	2015-05-18 11:17:10	809122010	59.5055	60	59.5055	59.5055	0	59.5135	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57618.6721759259	2016-08-18 16:07:56	57538	2016-05-30 00:00:00	57171.5244212963	2015-05-29 12:35:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091701	We propose to carry out joint Chandra and Suzaku observations of the starburst galaxy M82. We will search for extended clumps similar to the Northern Cap out to 45 kpc. We will also constrain the density and temperature profiles of the tenuous wind emission out to large radii. These data can place important constraints on theoretical models of starburst galaxies and their environments. We will test models such as the Chevalier & Clegg adiabatic wind model, hydrostatic halo model, shocked clouds in a wind, etc. The excellent Chandra spatial resolution combining with the low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	S	KA-WAH WONG		USA	9	AO9	SEARCH FOR THE OUTER BOUNDARY OF THE STARBURST GALAXY: M82	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809122010/	Quick Look
235	ABELL 2255 CENTER	258.2484	64.1467	258.17067	64.203551	200.767912	84.543322	94.02951141	34.88778486	111.176	55234.3014814815	2010-02-07 07:14:08	55235.405775463	2010-02-08 09:44:19	804041010	44.5337	50	44.5337	44.5417	0	44.5417	1	1	0	1	1	0	0	43.339	43.339	95.3759	1	PROCESSED	57550.5171180556	2016-06-11 12:24:39	55617	2011-02-25 00:00:00	55250.1645601852	2010-02-23 03:56:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040091	Suzaku discovered an supra thermal component in the plasma of Abell 3667 which exceeds 13 keV. In order to establish this component in merging clusters, we propose two pointing observations of Abell 2255, which hosts a huge radio halo and a radio relic. With these two pointings, we aim at roughly spotting the location of the supra thermal plasma.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MADOKA KAWAHARADA		JAP	4	AO4	PROBING SUPRA THERMAL PLASMA IN ABELL 2255 WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804041010/	Quick Look
236	OPHIUCHUS CLUSTER 1	258.2981	-23.3868	257.539766	-23.328523	259.261866	-0.380707	0.65649186	9.12279372	88.7031	54180.6159953704	2007-03-21 14:47:02	54181.1398611111	2007-03-22 03:21:24	801022010	24.067	15	24.075	24.067	0	24.075	2	2	0	2	1	0	0	21.8213	21.8213	45.254	1	PROCESSED	57537.7417476852	2016-05-29 17:48:07	54736	2008-09-27 00:00:00	54186.192650463	2007-03-27 04:37:25	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010065	The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUTAKA FUJITA		JAP	1	AO1	PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801022010/	Quick Look
237	COMA OUTSKIRTS6	193.974	28.5108	193.369273	28.781265	180.320045	31.486616	87.70306179	88.30207114	115.9975	55904.7228703704	2011-12-09 17:20:56	55905.1452662037	2011-12-10 03:29:11	806025010	21.503	20	21.503	21.503	0	21.503	1	1	0	1	1	0	0	20.265	20.265	36.4719	0	PROCESSED	57604.0827083333	2016-08-04 01:59:06	56284	2012-12-23 00:00:00	55915.2118402778	2011-12-20 05:05:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060099	In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKUYA SATO		JAP	6	AO6	STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806025010/	Quick Look
238	AWM7	43.631	41.5933	42.82175	41.390486	53.723626	23.815753	146.34082925	-15.61629549	90.4997	53954.2348842593	2006-08-07 05:38:14	53954.71625	2006-08-07 17:11:24	801035010	18.9858	20	18.9858	18.9858	18.9858	18.9858	2	2	2	2	1	0	0	17.5542	17.5542	41.588	0	PROCESSED	57535.2434953704	2016-05-27 05:50:38	54422	2007-11-18 00:00:00	54020.7471759259	2006-10-12 17:55:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010076	The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKAYA OHASHI		JAP	1	AO1	SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801035010/	Quick Look
239	NGC 4631	190.5387	32.5478	189.929771	32.821718	174.99352	33.703009	142.74124336	84.2191655	139.0678	54067.1412615741	2006-11-28 03:23:25	54068.9133217593	2006-11-29 21:55:11	801019010	81.0761	80	81.0841	81.0761	0	81.0841	2	2	0	2	1	0	0	74.4358	74.4358	153.07	0	PROCESSED	57536.2568865741	2016-05-28 06:09:55	54735	2008-09-26 00:00:00	54088.6914699074	2006-12-19 16:35:43	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010062	We propose to observe a edge-on nearby starburst galaxy, NGC 4631 for an exposure time of 80 ksec. This observation will give us a ``template'' of ejecta from type II SNe with less than 30% accuracy of abandance of alpha elemements.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORIKO YAMASAKI		JAP	1	AO1	OBSERVATION OF A STARBURST GALAXY NGC 4631 WITH XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801019010/	Quick Look
240	THE MOON	138.793	11.1278	138.115741	11.336148	137.780525	-4.592174	219.45159127	36.90361182	285.3988	56784.1992939815	2014-05-07 04:46:59	56784.3233101852	2014-05-07 07:45:34	809001060	6.4	45	6.4	6.4	0	6.4	1	1	0	1	1	0	0	6.2762	6.2762	10.7119	0	PROCESSED	57615.0611805556	2016-08-15 01:28:06	57218	2015-07-15 00:00:00	56852.5717708333	2014-07-14 13:43:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001060/	Quick Look
241	CIZA J2242.8+5301	340.7602	53.1616	340.242904	52.89922	13.612188	54.382245	104.28022824	-4.9963098	17.994	55770.5553703704	2011-07-28 13:19:44	55772.8210185185	2011-07-30 19:42:16	806001010	122.9419	120	122.9499	122.9499	0	122.9419	2	2	0	2	1	0	0	134.8043	134.8043	195.7079	1	PROCESSED	57602.7365393518	2016-08-02 17:40:37	56162	2012-08-23 00:00:00	55792.3410069445	2011-08-19 08:11:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060014	Radio relics in merging clusters have been considered to be synchrotron emission at a shock front. Nevertheless, no concrete evidence of the connection between relics and shocks has been unveiled yet. We propose a SUZAKU observation of a giant radio relic in a new merging cluster CIZA J2242.8+5301 recently discovered. Temperature and density maps across the giant radio relic will provide a clear illustration of the shock structure or a strong constraint of an origin of the radio relic.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HAJIME KAWAHARA	SHO NISHINO	JAP	6	AO6	SUZAKU OBSERVATION OF A NEW MERGING CLUSTER WITH A GIANT RADIO RELIC	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806001010/	Quick Look
242	A2319NORTH	290.2404	44.0121	289.851853	43.916672	305.965056	64.946826	75.73364984	13.56775034	191.4804	55925.1947222222	2011-12-30 04:40:24	55927.5001273148	2012-01-01 12:00:11	806014010	104.7893	100	104.8293	104.7893	0	104.8293	1	1	0	1	0	0	0	0	0	1.8661	0	PROCESSED	57604.2771064815	2016-08-04 06:39:02	56340	2013-02-17 00:00:00	55973.7475115741	2012-02-16 17:56:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060044	We propose the observations of the north subgroup region in the A2319 cluster with Suzaku to investigate dynamical status and particle acceleration process in the intracluster medium (ICM). A2319 is a nearby massive merging cluster whose collision axis is nearly along the line of sight, and has diffuse non-thermal radio emission. We will determine the radial velocity of the ICM in the north subgroup region, and compare it with that in the central region which has been already determined from the AO1 data (Sugawara et al. 2009). Using these results and optical observational data of member galaxies, we will determine dynamical status of the ICM and get implications on the particle acceleration process.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MOTOKAZU TAKIZAWA		JAP	6	AO6	DYNAMICAL STATUS OF THE HOT GAS AROUND THE NORTH SUBGROUP IN THE A2319 CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806014010/	Quick Look
243	COMA OUTSKIRTS2	195.8535	28.5112	195.253601	28.779358	182.053697	32.234375	61.20140467	87.01280614	116.0004	55901.4349189815	2011-12-06 10:26:17	55901.9223842593	2011-12-06 22:08:14	806021010	20.3577	20	20.3617	20.3577	0	20.3648	2	2	0	2	1	0	0	19.1946	19.1946	42.114	0	PROCESSED	57604.0414351852	2016-08-04 00:59:40	56282	2012-12-21 00:00:00	55914.2609375	2011-12-19 06:15:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060099	In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKUYA SATO		JAP	6	AO6	STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806021010/	Quick Look
244	ABELL 3341	81.3893	-31.5876	80.918035	-31.630439	77.271182	-54.650323	235.16288585	-31.086571	266.8997	57094.3290393518	2015-03-13 07:53:49	57094.5780092593	2015-03-13 13:52:20	809104010	11.439	10	11.439	11.439	0	11.439	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.7607407407	2016-08-17 18:15:28	57478	2016-03-31 00:00:00	57108.4097685185	2015-03-27 09:50:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809104010/	Quick Look
245	A3112	49.3536	-44.4489	48.920211	-44.631107	25.15452	-59.09191	253.34827073	-56.10640985	209.0009	57000.6762037037	2014-12-09 16:13:44	57003.8439351852	2014-12-12 20:15:16	809116010	107.9651	200	107.9651	107.9651	0	107.9651	2	2	0	2	1	0	0	8.1487	8.1487	33.9079	1	PROCESSED	57617.53125	2016-08-17 12:45:00	57387	2015-12-31 00:00:00	57016.2346180556	2014-12-25 05:37:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	094527	The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ESRA BULBUL	KOSUKE SATO	USJ	9	AO9	A DETAILED STUDY OF CHEMICAL ENRICHMENT OF A3112 OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809116010/	Quick Look
246	THE MOON	19.4299	8.4288	18.775956	8.165731	21.110635	0.205257	134.00151394	-53.87712274	73.8016	56856.6577777778	2014-07-18 15:47:12	56856.7905439815	2014-07-18 18:58:23	809001110	6.3696	45	6.3856	6.3696	0	6.3936	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.3999305556	2016-08-15 09:35:54	57233	2015-07-30 00:00:00	56867.740474537	2014-07-29 17:46:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001110/	Quick Look
247	THE MOON	20.9888	9.1871	20.332488	8.926606	22.823039	0.333671	136.29340358	-52.83899755	73.8	56856.7918055556	2014-07-18 19:00:12	56856.8877662037	2014-07-18 21:18:23	809001120	4.2623	45	4.2703	4.2623	0	4.2783	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.400775463	2016-08-15 09:37:07	57233	2015-07-30 00:00:00	56867.7339930556	2014-07-29 17:36:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001120/	Quick Look
248	RXCJ0018.9-4051	4.7354	-40.8551	4.113382	-41.132744	344.925025	-38.685562	326.87167276	-74.72717506	232.4175	55161.0142708333	2009-11-26 00:20:33	55161.4169444444	2009-11-26 10:00:24	804004010	19.3278	10	19.3278	19.3278	0	19.3278	1	1	0	1	1	0	0	13.3198	13.3198	34.7839	1	PROCESSED	57549.5606481482	2016-06-10 13:27:20	55553	2010-12-23 00:00:00	55182.6506712963	2009-12-17 15:36:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040005	We propose Suzaku observations of 8 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. With a total exposure time of 80 ksec, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	4	AO4	LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804004010/	Quick Look
249	PERSEUS OFFSET-H	50.3251	41.6598	49.495605	41.480554	58.942633	22.403293	150.73113668	-12.9828544	270.0006	55595.9611458333	2011-02-03 23:04:03	55596.3536805556	2011-02-04 08:29:18	805048010	18.241	25	18.249	18.249	0	18.241	1	1	0	1	1	0	0	14.88	14.88	33.9039	0	PROCESSED	57600.8294560185	2016-07-31 19:54:25	55979	2012-02-22 00:00:00	55610.233287037	2011-02-18 05:35:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050093	We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKAYUKI TAMURA		JAP	5	AO5	MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805048010/	Quick Look
250	ABELL 2667	357.9715	-25.9262	357.325218	-26.204419	347.258509	-22.861194	34.71945037	-76.63317585	64.8859	55721.5923611111	2011-06-09 14:13:00	55722.9050925926	2011-06-10 21:43:20	806029010	51.2214	50	51.2294	51.2294	0	51.2214	2	2	0	2	1	0	0	40.4843	40.4843	113.4098	1	PROCESSED	57602.2712962963	2016-08-02 06:30:40	55652	2011-04-01 00:00:00	55757.6995486111	2011-07-15 16:47:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806029010/	Quick Look
251	PERSEUS W1_2	49.5978	41.5445	48.771099	41.36257	58.342724	22.443076	150.3304489	-13.378921	258.3807	56328.3362615741	2013-02-05 08:04:13	56329.0106018518	2013-02-06 00:15:16	807022010	28.9492	25	28.9492	28.9732	0	28.9492	2	2	0	2	1	0	0	26.2751	26.2751	58.2559	0	PROCESSED	57610.5207523148	2016-08-10 12:29:53	56715	2014-02-27 00:00:00	56349.5185648148	2013-02-26 12:26:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070056	We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKAYUKI TAMURA		JAP	7	AO7	GAS MOTION IN THE PERSEUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807022010/	Quick Look
252	PERSEUS G_2	50.329	41.3745	49.501378	41.195271	58.861053	22.128129	150.89645322	-13.21839457	259.7649	56325.9651157407	2013-02-02 23:09:46	56326.3181828704	2013-02-03 07:38:11	807023010	14.2445	15	14.2445	14.2525	0	14.2525	2	2	0	2	1	0	0	20.5822	20.5822	30.4839	0	PROCESSED	57610.4949074074	2016-08-10 11:52:40	56711	2014-02-23 00:00:00	56345.4909953704	2013-02-22 11:47:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070056	We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKAYUKI TAMURA		JAP	7	AO7	GAS MOTION IN THE PERSEUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807023010/	Quick Look
253	COMA SW1	194.4352	27.7266	193.830461	27.996528	181.158138	30.970186	56.45564066	88.47880121	314.5924	55735.5408796296	2011-06-23 12:58:52	55735.8654166667	2011-06-23 20:46:12	806047010	8.9948	10	9.0028	8.9948	0	9.0108	2	2	0	2	1	0	0	8.5423	8.5423	28.0339	1	PROCESSED	57602.3938773148	2016-08-02 09:27:11	55652	2011-04-01 00:00:00	55794.9989583333	2011-08-21 23:58:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806047010/	Quick Look
254	COMA SW6	193.5264	26.9952	192.918358	27.266175	180.700954	29.954854	20.45636346	89.39137704	314.5991	55736.3040393518	2011-06-24 07:17:49	55736.5884259259	2011-06-24 14:07:20	806049010	15.6938	15	15.6938	15.7258	0	15.7098	1	1	0	1	1	0	0	13.0934	13.0934	24.5599	0	PROCESSED	57602.3988657407	2016-08-02 09:34:22	55652	2011-04-01 00:00:00	55795.0033333333	2011-08-22 00:04:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806049010/	Quick Look
255	COMA SW6.5	193.4098	26.8733	192.801305	27.144404	180.65639	29.799393	5.58469416	89.44734556	314.5984	55736.5887615741	2011-06-24 14:07:49	55737.1238773148	2011-06-25 02:58:23	806050010	16.5376	15	16.5616	16.5536	0	16.5376	2	2	0	2	1	0	0	16.6623	16.6623	46.208	2	PROCESSED	57602.4126157407	2016-08-02 09:54:10	55652	2011-04-01 00:00:00	55795.0480324074	2011-08-22 01:09:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806050010/	Quick Look
256	DDO 120	185.3167	45.8198	184.701182	46.097069	161.957395	43.126416	138.73502996	70.37152611	129.0479	56256.0169444444	2012-11-25 00:24:24	56258.4271990741	2012-11-27 10:15:10	807044010	101.7414	100	101.7414	101.7414	0	101.7414	2	2	0	2	1	0	0	91.0864	91.0864	208.1839	0	PROCESSED	57608.1579861111	2016-08-08 03:47:30	56644	2013-12-18 00:00:00	56275.7410648148	2012-12-14 17:47:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070107	We propose to observe an irregular dwarf galaxy DDO120 to detect a hot interstellar medium associated with the dwarf galaxy. The study of the temperature and density of the gas will give us important information about the pollution of the intergalactic medium from galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	RYO YAMAMOTO		JAP	7	AO7	SEARCH FOR HOT INTERSTELLAR MEDIUM OF AN IRREGULAR DWARF GALAXY DDO 120	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807044010/	Quick Look
257	UGC03957 NORTH	114.9138	55.8102	113.899292	55.925218	106.552165	33.791456	161.76581362	28.79157051	294.9973	56006.0767939815	2012-03-20 01:50:35	56007.0710532407	2012-03-21 01:42:19	806091010	41.3662	45	41.3662	41.3662	0	41.3662	2	2	0	2	1	0	0	40.6312	40.6312	85.9019	1	PROCESSED	57604.9833217593	2016-08-04 23:35:59	56389	2013-04-07 00:00:00	56022.2738888889	2012-04-05 06:34:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062024	Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	BRENDA MIRANDA OCEJO		EUR	6	AO6	MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806091010/	Quick Look
258	UGC03957 SOUTH	115.5259	55.024	114.524001	55.141747	107.151159	33.092194	162.70412876	29.04503782	294.9967	56007.0719907407	2012-03-21 01:43:40	56008.1328125	2012-03-22 03:11:15	806092010	48.8159	45	48.8159	48.8159	0	48.8159	2	2	0	2	1	0	0	46.4169	46.4169	91.6439	3	PROCESSED	57604.9862731482	2016-08-04 23:40:14	56389	2013-04-07 00:00:00	56022.2514930556	2012-04-05 06:02:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062024	Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	BRENDA MIRANDA OCEJO		EUR	6	AO6	MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806092010/	Quick Look
259	A1750C	202.6943	-1.8873	202.05036	-1.629855	201.691973	7.074913	322.57262201	59.47596371	293.5241	55766.9371064815	2011-07-24 22:29:26	55767.8814814815	2011-07-25 21:09:20	806095010	41.4893	40	41.5049	41.4893	0	41.5049	2	2	0	2	1	0	0	41.0991	41.0991	81.5778	0	PROCESSED	57602.6723148148	2016-08-02 16:08:08	56219	2012-10-19 00:00:00	55851.4572106482	2011-10-17 10:58:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	063019	We observe Abell 1750 which has three clusters of galaxies in a filamentary structure of the large-scale structure, with 4 pointing observations (80 x 3 + 40 ks). We reveal global spatial structures of temperature, density, and entropy in Abell 1750 for the first time. By a correlation with a galaxy map obtained from SDSS, and a comparison between thermal pressure and total pressure required by the total mass derived from weal lensing analysis, we explore the inflow of matter and evolutionary process in this system.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA	SCOTT RANDALL	JUS	6	AO6	SUZAKU OBSERVATION OF ABELL 1750 IN THE LARGE-SCALE STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806095010/	Quick Look
260	M31	10.6944	41.2627	10.010045	40.988882	27.852586	33.34214	121.18191229	-21.57961988	231.6592	54115.6775578704	2007-01-15 16:15:41	54117.4572222222	2007-01-17 10:58:24	801043010	99.8723	100	99.8723	99.8723	0	99.8723	2	2	0	2	1	0	0	103.9124	103.9124	153.7238	1	PROCESSED	57536.8902777778	2016-05-28 21:22:00	54744	2008-10-05 00:00:00	54132.9457291667	2007-02-01 22:41:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010089	We propose the 100 ks Suzaku observation of the central region of Andromeda Nebula (M31). Our gaol is to detect 3 components (cool, hot and hard) of galactic diffuse X-ray emission (GDXE) with the XIS and HXD. This detection shows the existance of the GDXE hot and hard component in the extragalactic normal spiral galaxy, for the first time.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	HIROMITSU TAKAHASHI		JAP	1	AO1	DETECTION OF GALACTIC DIFFUSE X-RAY EMISSION FROM THE CENTRAL REGION OF THE ANDROMEDA NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801043010/	Quick Look
261	ANTLIA E1	157.8782	-35.3295	157.312453	-35.072071	176.074864	-40.746998	273.21530285	19.3432713	277.4995	56091.5629398148	2012-06-13 13:30:38	56092.2633912037	2012-06-14 06:19:17	807066010	25.747	23	25.755	25.747	0	25.755	2	2	0	2	1	0	0	22.9291	22.9291	60.5139	1	PROCESSED	57605.6597106482	2016-08-05 15:49:59	56473	2013-06-30 00:00:00	56107.272650463	2012-06-29 06:32:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071521	We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	7	AO7	MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807066010/	Quick Look
262	A133_E	15.9075	-21.8935	15.297134	-22.16169	5.436545	-26.315725	151.49316881	-84.07673835	44.9955	55356.7284953704	2010-06-09 17:29:02	55358.0015393518	2010-06-11 00:02:13	805021010	51.5523	50	51.5641	51.5603	0	51.5523	2	2	0	2	1	0	0	46.2547	46.2547	109.984	1	PROCESSED	57551.9411458333	2016-06-12 22:35:15	55737	2011-06-25 00:00:00	55375.7548842593	2010-06-28 18:07:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050019	We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KOSUKE SATO		JAP	5	AO5	METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805021010/	Quick Look
263	COMA NW6.5	194.0774	29.5523	193.474522	29.822643	179.856398	32.45513	99.36309014	87.34957637	319.9974	55734.7422685185	2011-06-22 17:48:52	55735.2522569444	2011-06-23 06:03:15	806045010	15.5013	15	15.5013	15.5151	0	15.5093	2	2	0	2	1	0	0	17.3764	17.3764	44.0599	0	PROCESSED	57602.3928587963	2016-08-02 09:25:43	55652	2011-04-01 00:00:00	55768.3250231482	2011-07-26 07:48:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806045010/	Quick Look
264	ABELL 1795	207.2241	26.601	206.646901	26.849155	193.922602	34.994161	33.84733119	77.1817764	130.8638	53714.5034259259	2005-12-10 12:04:56	53714.7752199074	2005-12-10 18:36:19	800012010	13.0982	120	13.1062	13.0982	13.1062	13.1062	1	1	1	1	1	0	0	10.3759	10.3759	23.4639	1	PROCESSED	57532.3922453704	2016-05-24 09:24:50	54247	2007-05-27 00:00:00	54038.7903703704	2006-10-30 18:58:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012010/	Quick Look
265	Z8852	347.6318	7.5789	346.999079	7.307292	351.631711	11.858062	84.17423864	-47.55525942	260.3346	54065.5867013889	2006-11-26 14:04:51	54066.1543287037	2006-11-27 03:42:14	801074010	14.8526	15	14.8526	14.8526	0	14.8526	2	2	0	2	1	0	0	13.9834	13.9834	49.0379	0	PROCESSED	57536.1918402778	2016-05-28 04:36:15	54695	2008-08-17 00:00:00	54088.6000694444	2006-12-19 14:24:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801074010/	Quick Look
266	PERSEUS H_2	50.3295	41.6532	49.500037	41.47397	58.944091	22.396043	150.73770492	-12.98651547	259.0589	56327.8720949074	2013-02-04 20:55:49	56328.3355092593	2013-02-05 08:03:08	807021010	20.3456	20	20.3636	20.3456	0	20.3536	2	2	0	2	1	0	0	21.8776	21.8776	40.034	0	PROCESSED	57610.5111921296	2016-08-10 12:16:07	56715	2014-02-27 00:00:00	56349.4892708333	2013-02-26 11:44:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070056	We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKAYUKI TAMURA		JAP	7	AO7	GAS MOTION IN THE PERSEUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807021010/	Quick Look
267	A2495	342.5662	10.9218	341.941655	10.656649	348.262816	16.910805	81.19678392	-41.92445268	65.1354	54260.5857523148	2007-06-09 14:03:29	54261.1668287037	2007-06-10 04:00:14	801080020	25.7806	18	25.7806	25.7806	0	25.7806	2	2	0	2	1	0	0	20.9762	20.9762	50.1959	2	PROCESSED	57538.8757291667	2016-05-30 21:01:03	54695	2008-08-17 00:00:00	54270.430625	2007-06-19 10:20:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080020/	Quick Look
268	CENTAURUS CLUSTER	192.2012	-41.3132	191.510497	-41.040677	209.072585	-32.853902	302.40029759	21.55583076	106.2442	53731.2579050926	2005-12-27 06:11:23	53732.1808333333	2005-12-28 04:20:24	800014010	36.5192	30	36.5192	36.5464	36.5464	36.5224	2	2	2	2	1	0	0	32.1498	32.1498	79.7399	0	PROCESSED	57532.5349652778	2016-05-24 12:50:21	54247	2007-05-27 00:00:00	54039.373900463	2006-10-31 08:58:25	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001070	A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	0	SWG	OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800014010/	Quick Look
269	HCG62_W	192.9973	-9.0837	192.347013	-8.812069	195.480643	-3.238715	303.16227701	53.78780217	292.9782	55405.1509953704	2010-07-28 03:37:26	55406.9773611111	2010-07-29 23:27:24	805031010	66.947	60	66.955	66.955	0	66.947	2	2	0	2	1	0	0	52.9972	52.9972	157.7758	1	PROCESSED	57552.8094675926	2016-06-13 19:25:38	55808	2011-09-04 00:00:00	55441.3150925926	2010-09-02 07:33:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050034	We propose offset observations of groups of galaxies to study the metal distributions up to ~0.5 times of the virial radius. Metal mass to galaxy light ratios (MLRs) for groups are much smaller than those for clusters of galaxies. In order to solve the problem which is important to understand the chemical history of the universe, we need much information of the metal abundance and distributions to the outer region of the groups. Suzaku firstly enable us to measure the metals to such an outer region of groups.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KOSUKE SATO		JAP	5	AO5	SEARCH FOR THE METAL DISTRIBUTIONS OF GROUPS OF GALAXIES TO 0.5 R180	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805031010/	Quick Look
270	BEYOND VIRGO 4	187.7154	16.9006	187.085728	17.176651	180.130581	18.529302	276.92044319	78.71921322	118.472	55915.331099537	2011-12-20 07:56:47	55916.0466666667	2011-12-21 01:07:12	806063010	30.1361	30	30.1361	30.1361	0	30.1361	2	2	0	2	1	0	0	22.7334	22.7334	61.818	0	PROCESSED	57604.1732407407	2016-08-04 04:09:28	56299	2013-01-07 00:00:00	55932.1295949074	2012-01-06 03:06:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061523	To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORBERT WERNER		USA	6	AO6	LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806063010/	Quick Look
271	RCS215222-0503.9	328.0881	-5.0633	327.433899	-5.298799	328.489701	7.382957	52.1030598	-42.03624594	70.7002	55696.1248842593	2011-05-15 02:59:50	55696.8398263889	2011-05-15 20:09:21	806081010	30.6482	30	30.6482	30.6482	0	30.6482	1	1	0	1	1	0	0	25.3728	25.3728	61.744	0	PROCESSED	57602.0507986111	2016-08-02 01:13:09	56072	2012-05-25 00:00:00	55705.2063310185	2011-05-24 04:57:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061533	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AMALIA HICKS		USA	6	AO6	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806081010/	Quick Look
272	A3526	191.8847	-40.8272	191.196139	-40.554367	208.554246	-32.533282	302.13618529	22.03852437	109.9993	55942.6812037037	2012-01-16 16:20:56	55942.9772569444	2012-01-16 23:27:15	806085010	15.0057	11	15.0097	15.0057	0	15.0116	2	2	0	2	1	0	0	14.9297	14.9297	25.576	0	PROCESSED	57604.3736805556	2016-08-04 08:58:06	56331	2013-02-08 00:00:00	55960.1598726852	2012-02-03 03:50:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806085010/	Quick Look
273	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
274	A1060	159.1744	-27.531	158.58579	-27.271265	172.752913	-33.32931	269.60056717	26.48279097	103.6438	53696.6258796296	2005-11-22 15:01:16	53697.7211111111	2005-11-23 17:18:24	800003010	39.139	40	39.139	39.147	39.155	39.155	2	2	2	2	1	0	0	34.6024	34.6024	94.6259	1	PROCESSED	57528.0675462963	2016-05-20 01:37:16	54247	2007-05-27 00:00:00	54037.8583449074	2006-10-29 20:36:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001021	A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI		JAP	0	SWG	OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800003010/	Quick Look
275	NGC720	28.2529	-13.7362	27.644452	-13.982164	20.9363	-23.62893	173.01572713	-70.35499124	242.5294	53734.3673611111	2005-12-30 08:49:00	53739.5627546296	2006-01-04 13:30:22	800009010	177.1929	100	177.1929	177.1929	177.1929	177.1929	2	2	2	2	1	0	0	9.6621	9.6621	47.5408	0	PROCESSED	57532.602962963	2016-05-24 14:28:16	54247	2007-05-27 00:00:00	54039.6651736111	2006-10-31 15:57:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001031	We propose to observe an isolated elliptical galaxy NGC720 with Suzaku. Isolated elliptical galaxies are important to probe the ISM metal abundance, since their hot gas is not affected by the amibient bright intracluster medium which often exists around X-ray bright elliptical galaxies. Suzaku is expected to measure the Oxygen abundance in the ISM bettern than XMM-Newton and constrain the origin of metals in the ISM and also ICM. Dark matter content around elliptical galaxies can also be constrained better than XMM-Newton. Such a measurement is difficult for X-ray bright galaxies due to the superposition of the cluster potential.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	0	SWG	OXYGEN ABUNDANCE AND DARK MATTER CONTENT AROUDN AN ISOLATED ELLIPTICAL GALAXY NGC720	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800009010/	Quick Look
276	A2104N	235.0318	-3.1802	234.37876	-3.019346	233.471257	15.936264	2.94593816	39.29281704	117.689	54119.2779166667	2007-01-19 06:40:12	54119.7522337963	2007-01-19 18:03:13	801002010	18.8424	20	18.8424	18.8424	0	18.8424	2	2	0	2	1	0	0	13.6448	13.6448	40.9779	1	PROCESSED	57536.8705439815	2016-05-28 20:53:35	54735	2008-09-26 00:00:00	54133.3893518518	2007-02-02 09:20:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010012	We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO HATTORI		JAP	1	AO1	TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801002010/	Quick Look
277	NGC 507	20.9105	33.2598	20.206045	32.999169	32.202982	22.611804	130.6367604	-29.12969375	54.0771	53944.6189351852	2006-07-28 14:51:16	53946.5544444444	2006-07-30 13:18:24	801017010	79.5013	80	79.5253	79.5013	79.5253	79.5253	2	2	2	2	1	0	0	80.2867	80.2867	167.17	2	PROCESSED	57535.1047222222	2016-05-27 02:30:48	54394	2007-10-21 00:00:00	53955.7736689815	2006-08-08 18:34:05	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010061	We propose to observe luminous elliptical galaxies NGC 507 and NGC 499 for 80 and 100 ksec, respectively, to study abundance distribution of Fe and O. The good energy resolution and low background of the XIS instrument is crucial for this study, and we can perform the first reliable measurement of O distribution around elliptical galaxies. Comparison of O and Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. Comparison of NGC 507 and NGC 499 will show us how much metal production process differ with galaxy size.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KOSUKE SATO		JAP	1	AO1	CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES IN GROUP OF GALAXIES: NGC 507 AND NGC 499	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801017010/	Quick Look
278	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
279	OPHIUCHUS CLUSTER 2	257.7375	-23.3864	256.979428	-23.325463	258.749053	-0.422802	0.3572282	9.54416529	94.9391	54181.1423726852	2007-03-22 03:25:01	54181.825162037	2007-03-22 19:48:14	801023010	24.6782	15	24.7022	24.6942	0	24.6782	2	2	0	2	1	0	0	21.2781	21.2781	58.9879	1	PROCESSED	57537.9744097222	2016-05-29 23:23:09	54736	2008-09-27 00:00:00	54209.5433217593	2007-04-19 13:02:23	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010065	The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUTAKA FUJITA		JAP	1	AO1	PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801023010/	Quick Look
280	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
281	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
282	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
283	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
284	A2319CENTER	290.3341	43.878	289.944223	43.782148	306.012819	64.798086	75.63759851	13.45022652	251.6652	54035.9326041667	2006-10-27 22:22:57	54038.1466898148	2006-10-30 03:31:14	801040010	99.5332	100	99.5492	99.5412	99.5332	99.5492	2	2	2	2	1	0	0	93.9548	93.9548	191.268	2	PROCESSED	57535.9905555556	2016-05-27 23:46:24	54735	2008-09-26 00:00:00	54063.5741666667	2006-11-24 13:46:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010085	We propose the observations of the A2319 cluster with the Suzaku HXD and XIS to investigate particle acceleration processes in the intracluster medium(ICM). A2319 is a nearby massive merging cluster whose collision axis is nearly along the line of sight, and has diffuse non-thermal radio emission. We will detect non-thermal hard X-ray with HXD, and determine the velocity difference between the two subclusters with XIS. With these results, we will determine dynamical status of the ICM and get implications on the particle acceleration processes. We will compare the results with theoretical models, numerical simulations, and radio and optical observations to get an overall picture of particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MOTOKAZU TAKIZAWA		JAP	1	AO1	PARTICLE ACCELERATION IN THE A2319 CLUSTER	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801040010/	Quick Look
285	PERSEUS CL OFFSET	50.5735	41.8053	49.742345	41.626976	59.178685	22.492416	150.80595618	-12.75877318	65.9956	53982.1426736111	2006-09-04 03:25:27	53982.4377893518	2006-09-04 10:30:25	801049040	10.4206	30	10.4206	10.4206	10.4206	10.4206	2	2	2	2	1	0	0	7.5402	7.5402	25.4679	1	PROCESSED	57535.4390856482	2016-05-27 10:32:17	54526	2008-03-01 00:00:00	54021.0033680556	2006-10-13 00:04:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010097	We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	1	AO1	MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049040/	Quick Look
286	NGC3923	177.7599	-28.8047	177.126048	-28.526534	190.367331	-27.106442	287.27787622	32.22445477	293.1988	53899.8430671296	2006-06-13 20:14:01	53902.7293287037	2006-06-16 17:30:14	801054010	115.82	120	115.828	115.82	115.828	115.828	2	2	2	2	1	0	0	107.7313	107.7313	249.3528	3	PROCESSED	57534.7187731482	2016-05-26 17:15:02	54394	2007-10-21 00:00:00	53927.2880902778	2006-07-11 06:54:51	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010100	We propose to observe an isolated elliptical galaxy NGC3923, to meaasure a dark matter distribution. The large effective area and stable low background of XIS enable us to measure a faint extended X-ray emission such as the periphery of elliptical galaxies more accurately than ever. Since X-ray bright elliptical galaxies have been found to be surrounded by group-scale emission, X-ray faint elliptical galaxies are the best to investigate the dark matter associated with the galaxy itself. The dark matter around galaxies is a key to resolve the problem of why X-ray bright and faint elliptical galaxies exist. The oxygen abundance distribution is also useful to probe the above issue.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YASUSHI FUKAZAWA		JAP	1	AO1	ACCURATE MEASUREMENT OF DARK MATTER DISTRIBUTION AROUND AN ISOLATED ELLIPTICAL GALAXY NGC3923	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801054010/	Quick Look
287	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
288	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
289	A1631_N	193.3404	-15.1138	192.682958	-14.842526	198.153884	-8.661195	303.62251983	47.75536925	113.0007	56303.6628356482	2013-01-11 15:54:29	56304.4904861111	2013-01-12 11:46:18	807003010	28.0433	20	28.183	28.183	0	28.0433	3	3	0	3	1	0	0	25.3059	25.3059	71.48	1	PROCESSED	57608.4621296296	2016-08-08 11:05:28	56703	2014-02-15 00:00:00	56337.5115393518	2013-02-14 12:16:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070029	In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	7	AO7	PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807003010/	Quick Look
290	NGC 4472	187.4441	8.005	186.80838	8.281234	183.627851	10.299036	286.9163593	70.20028227	117.8054	54072.8427893518	2006-12-03 20:13:37	54075.7014699074	2006-12-06 16:50:07	801064010	121.0358	120	121.0358	121.0358	0	121.0358	2	2	0	2	1	0	0	103.4464	103.4464	246.9548	6	PROCESSED	57536.3089467593	2016-05-28 07:24:53	54702	2008-08-24 00:00:00	54089.1857523148	2006-12-20 04:27:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011403	We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MICHAEL LOEWENSTEIN		USA	1	AO1	INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801064010/	Quick Look
291	NGC 4649	190.9148	11.557	190.284732	11.830628	185.371113	14.926523	295.86493189	74.32191724	113.3108	54098.4203703704	2006-12-29 10:05:20	54104.1473263889	2007-01-04 03:32:09	801065010	224.0304	120	224.0304	224.0304	0	224.0304	2	2	0	2	1	0	0	26.3042	26.3042	69.2898	1	PROCESSED	57536.4300578704	2016-05-28 10:19:17	54743	2008-10-04 00:00:00	54132.9809027778	2007-02-01 23:32:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011403	We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MICHAEL LOEWENSTEIN		USA	1	AO1	INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801065010/	Quick Look
292	UGC03957	115.2433	55.429	114.235063	55.545488	106.863653	33.455815	162.22286538	28.93195726	271.243	53841.9927314815	2006-04-16 23:49:32	53842.2828587963	2006-04-17 06:47:19	801072010	10.7714	12	10.7794	10.7794	10.7874	10.7714	1	1	1	1	1	0	0	9.642	9.642	25.0079	0	PROCESSED	57533.4729166667	2016-05-25 11:21:00	54401	2007-10-28 00:00:00	53906.7753240741	2006-06-20 18:36:28	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801072010/	Quick Look
293	A272	28.7603	33.9026	28.031098	33.657734	38.955118	20.665911	137.73606223	-27.1341127	64.9465	53943.0449537037	2006-07-27 01:04:44	53943.6842476852	2006-07-27 16:25:19	801084010	22.2455	21	22.2535	22.2535	22.2455	22.2535	2	2	2	2	1	0	0	24.6035	24.6035	55.2319	0	PROCESSED	57535.0602430556	2016-05-27 01:26:45	54401	2007-10-28 00:00:00	53955.6516782407	2006-08-08 15:38:25	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801084010/	Quick Look
294	A566	106.0915	63.2647	104.91759	63.339113	99.420321	40.34898	152.76309519	25.45548296	285.637	54178.3128587963	2007-03-19 07:30:31	54178.8029976852	2007-03-19 19:16:19	801085010	22.2711	20	22.2711	22.2711	0	22.2711	2	2	0	2	1	0	0	22.1523	22.1523	42.3399	0	PROCESSED	57537.7151157407	2016-05-29 17:09:46	54695	2008-08-17 00:00:00	54185.9799305556	2007-03-26 23:31:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801085010/	Quick Look
295	RXJ 0658	104.704	-55.933	104.461428	-55.862903	130.333928	-77.302143	266.02429497	-21.20357002	164.9362	54095.6181597222	2006-12-26 14:50:09	54098.4099421296	2006-12-29 09:50:19	801089010	101.3845	100	101.3845	101.3845	0	101.3845	2	2	0	2	1	0	0	84.3679	84.3679	241.1547	2	PROCESSED	57637.5971180556	2016-09-06 14:19:51	54702	2008-08-24 00:00:00	54111.5842013889	2007-01-11 14:01:15	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011448	We propose SUZAKU X-ray observations of an intriguing cluster of galaxies, RXJ0658, to determine and characterize the nature of the hard X-ray spectral emission and other nonthermal activity. It also has many other interesting features, such as a cold front, evidence for merger, a shock, and regions of unusually high temperature, all of which are related to the hard X-ray emission and the nonthermal activity. The more accurate measure of the spectral characteristics of the hard component, when combined with the radio and other past X-ray data, can reveal the nature of the emission process and the acceleration mechanism of the relativistic electrons, provide a means of measuring the magnetic field strength, and aid in understanding the process of formation of clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	VAHE PETROSIAN		USA	1	AO1	HARD X-RAY EMISSION FROM CLUSTER RXJ0658	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801089010/	Quick Look
296	SEGUE 1	151.7658	16.0862	151.086487	16.330668	148.083031	4.208593	220.47149585	50.42674703	110.8027	56248.0740625	2012-11-17 01:46:39	56250.3182291667	2012-11-19 07:38:15	807046010	85.4391	85	85.4622	85.4431	0	85.4391	2	2	0	2	1	0	0	77.5645	77.5645	193.8419	4	PROCESSED	57608.0603240741	2016-08-08 01:26:52	56641	2013-12-15 00:00:00	56275.5584490741	2012-12-14 13:24:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071502	Our ongoing dedicated X-ray search for dark matter targeting dwarf spheroidal galaxies set new constraints on the mass and mixing angle of the sterile neutrino -- a plausible dark matter candidate that emits an X-ray via radiative decay. We have proposed a new well-motivated candidate -- moduli dark matter, that also produces a detectable X-ray line. We propose Suzaku observations of the Segue 1 dwarf spheroidal -- the most dark matter dominated galaxy known. Its extreme nature implies that it provides the tightest constraints on sterile neutrino and moduli parameters in the event of a detection, and best limits in the absence of one. The resulting spectrum is optimal for exploring new physics, such as string theory compactification or supersymmetry breaking, and as a legacy for Astro-H.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MICHAEL LOEWENSTEIN		USA	7	AO7	SEARCH FOR DARK MATTER WITH SUZAKU OBSERVATIONS OF THE MOST DARK MATTER DOMINATED GALAXY IN THE UNIVERSE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807046010/	Quick Look
297	COMA RADIO HALO	194.9267	27.9061	194.323466	28.175433	181.517491	31.325949	56.39742233	88.00849705	295.2687	53886.8435300926	2006-05-31 20:14:41	53890.7439699074	2006-06-04 17:51:19	801097010	178.6572	180	178.6892	178.6572	178.7132	178.6892	2	2	2	2	1	0	0	167.4506	167.4506	336.9758	7	PROCESSED	57534.5953472222	2016-05-26 14:17:18	54401	2007-10-28 00:00:00	53926.6760416667	2006-07-10 16:13:30	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014446	We will observe the central regions of the Coma cluster with the HXD/PIN to detect and characterize the nonthermal Inverse Compton (IC) emission from the radio halo. Coma has the best-studied and brightest radio halo, which makes it the best case to detect IC and the most useful one for testing theories for the origin of radio halos. Previous detections with BeppoSAX and RXTE are controversial. Suzaku is more sensitive, will avoid contamination by nearby AGNs including X Comae, and will detect IC even if it is fainter than the claimed BeppoSAX detection. The HXD/PIN data will allow the cluster magnetic field, and nonthermal energy and pressure to be derived. The XIS observations will be used to determine accurate abundances and gradients in Coma, and to test theories for ICM enrichment.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	CRAIG SARAZIN	KYOKO MATSUSHITA	USJ	1	AO1	NAILING DOWN THE HARD X-RAY INVERSE COMPTON EMISSION FROM THE RADIO HALO IN THE COMA CLUSTER	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801097010/	Quick Look
298	A963S	154.2641	38.9388	153.524075	39.18875	141.373211	26.246798	182.75442962	55.85527134	107.1093	54432.4435300926	2007-11-28 10:38:41	54432.9584953704	2007-11-28 23:00:14	802012010	27.7172	25	27.7252	27.7252	0	27.7172	2	2	0	2	1	0	0	25.6546	25.6546	44.492	1	PROCESSED	57540.6110185185	2016-06-01 14:39:52	54811	2008-12-11 00:00:00	54440.9716319444	2007-12-06 23:19:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020018	We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 10% precision in a few arcmin scale, which has not been done before to any cluster. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO HATTORI		JAP	2	AO2	TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802012010/	Quick Look
299	ABELL 2744	3.5397	-30.3446	2.908232	-30.62262	349.980606	-28.995561	9.24871336	-81.22170813	53.4742	54239.5874652778	2007-05-19 14:05:57	54243.7709953704	2007-05-23 18:30:14	802033010	153.2332	150	153.2412	153.2412	0	153.2332	2	2	0	2	1	0	0	133.8631	133.8631	361.4398	2	PROCESSED	57538.8170138889	2016-05-30 19:36:30	54745	2008-10-06 00:00:00	54248.6974074074	2007-05-28 16:44:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020077	We propose a 150 ks Suzaku observation of Abell 2744 aiming at non-thermal hard X-ray detection. It has a red-shift of 0.3, a radio-halo flux of 57 mJy at 1.4 GHz and ICM temperature of 9 keV. Our strategy here is to observe a luminous merging cluster hosting a bright radio halo, whilst avoiding the thermal ICM emission to overwhelm the 10-40 keV band, in which the HXD has the best sensitivity. The key is to look for relatively high red-shift cluster. Since the CMB density increases as (1+z)^4, the inverse Compton emission relative to the radio flux increases typically as (1+z)^2, while the thermal ICM emission is red-shifted. We believe this is one of the best method to utilize the Suzaku power for cluster hard X-ray survey.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA		JAP	2	AO2	HARD X-RAY VIEW OF A DISTANT RADIO-HALO CLUSTER ABELL2744	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802033010/	Quick Look
300	NGC4636_GALACTIC_1	192.513	5.4558	191.878088	5.727905	189.348778	9.962987	301.99802564	68.32503562	300.0459	54268.8414930556	2007-06-17 20:11:45	54269.9307175926	2007-06-18 22:20:14	802039010	41.4997	30	41.5157	41.5077	0	41.4997	2	2	0	2	1	0	0	34.3371	34.3371	94.0479	0	PROCESSED	57553.0490393518	2016-06-14 01:10:37	54695	2008-08-17 00:00:00	54319.4765740741	2007-08-07 11:26:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020119	We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YOH TAKEI		JAP	2	AO2	DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802039010/	Quick Look
301	FORNAX_GALACTIC_2	49.9904	-32.0719	49.483389	-32.25188	35.195492	-48.193254	230.76086762	-57.49880076	52.7651	54280.3368518518	2007-06-29 08:05:04	54280.9897453704	2007-06-29 23:45:14	802040010	21.0746	20	21.0826	21.0826	0	21.0746	2	2	0	2	1	0	0	20.131	20.131	56.3939	1	PROCESSED	57539.0651967593	2016-05-31 01:33:53	54696	2008-08-18 00:00:00	54322.4474537037	2007-08-10 10:44:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020119	We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YOH TAKEI		JAP	2	AO2	DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802040010/	Quick Look
302	DRACO	260.0265	57.929	259.823545	57.97767	237.171171	80.222303	86.38548758	34.73420948	52.1224	54196.7611458333	2007-04-06 18:16:03	54198.2216898148	2007-04-08 05:19:14	802051010	63.3232	67	63.3232	63.3232	0	63.3232	2	2	0	2	1	0	0	64.9572	64.9572	126.1818	2	PROCESSED	57538.1232291667	2016-05-30 02:57:27	54829	2008-12-29 00:00:00	54203.3603703704	2007-04-13 08:38:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021405	We propose 50 ksec Suzaku observations of the Ursa Minor and Draco dwarf spheroidal galaxies. These dense, dark-matter-dominated systems are carefully selected as the strongest potential sources of line emission from radiatively decaying keV dark matter of any astrophysical object. The low-level, stable Suzaku background makes it the most sensitive instrument to-date for this purpose. At the very least, constraints that enter a significant new regime are derived: non-detections are still of great importance. In the best case, the long sought-after identity of dark matter will be discovered, pointing the way to physics beyond the Standard Model.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MICHAEL LOEWENSTEIN		USA	2	AO2	SEARCH FOR WARM DARK MATTER WITH SUZAKU OBSERVATIONS OF DWARF SPHEROIDAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802051010/	Quick Look
303	SDSS J0854+3524	133.7386	35.4192	132.953536	35.610263	126.168595	17.306871	188.0033984	39.53150085	111.2842	56214.3546527778	2012-10-14 08:30:42	56214.8244560185	2012-10-14 19:47:13	807063010	20.6148	20	20.6148	20.6148	0	20.6148	1	1	0	1	1	0	0	18.084	18.084	40.56	0	PROCESSED	57607.7601157407	2016-08-07 18:14:34	56598	2013-11-02 00:00:00	56232.4365856482	2012-11-01 10:28:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071512	Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ERIC MILLER		USA	7	AO7	FINDING FOSSIL GROUPS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807063010/	Quick Look
304	BOOTES GROUP 30	219.4427	33.5107	218.918921	33.726455	202.46828	45.823682	55.01212205	66.25629851	308.903	54276.6949189815	2007-06-25 16:40:41	54277.5271875	2007-06-26 12:39:09	802056010	38.5045	38	38.5045	38.5045	0	38.5045	2	2	0	2	1	0	0	35.7473	35.7473	71.8979	1	PROCESSED	57539.0466782407	2016-05-31 01:07:13	54702	2008-08-24 00:00:00	54333.4389583333	2007-08-21 10:32:06	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021424	We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MARSHALL BAUTZ		USA	2	AO2	SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802056010/	Quick Look
305	RXJ1159+5531	179.9637	55.4123	179.320531	55.690619	149.995673	49.037125	137.70641489	60.21165624	302.8269	56074.0600694445	2012-05-27 01:26:30	56075.6800578704	2012-05-28 16:19:17	807064010	82.2339	100	82.2419	82.2419	0	82.2339	2	2	0	2	1	0	0	98.6011	98.6011	139.964	1	PROCESSED	57605.5596875	2016-08-05 13:25:57	56657	2013-12-31 00:00:00	56086.0194328704	2012-06-08 00:27:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071513	With Chandra and Suzaku we recently constrained the hot gas and dark matter out to the virial radius (rvir=R108) in the fossil group/cluster RXJ1159+5531. Unlike some recent observations of cluster outskirts, the gas fraction is consistent with the cosmic value, and the entropy profile at rvir is consistent with gravity-only structure formation simulations. As a fossil group, RXJ1159+5531 may be unusually relaxed at large scales. If so, the gas properties should not vary much azimuthally. We propose a complementary Suzaku observation to explore this by measuring the gas in a different azimuthal region, more than doubling the current (~27%) azimuthal coverage. Our results will help determine if gas clumping, invoked to explain the outskirts of some clusters, is ubiquitous.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	PHILIP HUMPHREY		USA	7	AO7	RELAXED GAS AT THE VIRIAL RADIUS IN A FOSSIL GROUP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807064010/	Quick Look
306	PKS 0745-191	116.7966	-19.5079	116.243978	-19.383587	123.623714	-39.870751	236.58636127	2.85363493	294.0004	54234.0374884259	2007-05-14 00:53:59	54234.8446643518	2007-05-14 20:16:19	802062050	33.4146	30	33.4146	33.4226	0	33.4226	2	2	0	2	1	0	0	31.3065	31.3065	69.7239	1	PROCESSED	57538.6567708333	2016-05-30 15:45:45	54695	2008-08-17 00:00:00	54245.5456712963	2007-05-25 13:05:46	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021440	PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ANDREW YOUNG		USA	2	AO2	PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062050/	Quick Look
307	N1550_OFFSET	65.2479	2.4086	64.596961	2.290593	63.774789	-18.807983	191.20173857	-31.56876902	90.0005	54693.1139351852	2008-08-15 02:44:04	54694.185	2008-08-16 04:26:24	803018010	41.1447	40	41.1447	41.1447	0	41.1447	3	3	0	3	1	0	0	29.9469	29.9469	92.508	0	PROCESSED	57543.3286226852	2016-06-04 07:53:13	55079	2009-09-05 00:00:00	54711.3163310185	2008-09-02 07:35:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030070	We propose 80 and 40 ksec observations of the central and 30' offset regions of fossil group, NGC 1550, respectively, to study metal abundance distributions of O to Fe to the ~0.2 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. A comparison of O to Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. In addition, a comparison of the metal distributions of the nominal group of galaxies and fossil group will show us how much metal production and diffusion processes differ with system.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KOSUKE SATO		JAP	3	AO3	OBSERVATIONS OF METAL DISTRIBUTIONS IN FOSSIL GROUP: NGC1550	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803018010/	Quick Look
308	SHAPLEY OFFSET	204.9135	-29.8943	204.20662	-29.641044	214.142611	-18.17761	315.23466303	31.82297967	289.7009	54665.2119907407	2008-07-18 05:05:16	54666.4244675926	2008-07-19 10:11:14	803021010	47.2435	40	47.2435	47.2435	0	47.2435	2	2	0	2	1	0	0	38.3578	38.3578	104.7418	0	PROCESSED	57543.0903356482	2016-06-04 02:10:05	55049	2009-08-06 00:00:00	54682.1908680556	2008-08-04 04:34:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030089	We aim at the first significant detection of redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in the Shapley Supercluster. The system, located at z = 0.048, shows the richest concentration of X-ray clusters in the nearby universe. Previous ROSAT observation showed enhanced soft X-ray emission along the cluster connection. We propose to observe for 80 ksec a region between A3558 (the brightest central cluster) and A3556, separated by 0.9 virial radius from both clusters and along the line of cluster connection. A 40 ksec observation is also proposed at a 2-degree offest region to measure the foreground Galactic spectrum. Based on the ROSAT flux, we expect to detect redshifted OVII and OVII lines at more than 7 sigma confidence.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI		JAP	3	AO3	SEARCH FOR WHIM IN THE SHAPLEY SUPERCLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803021010/	Quick Look
309	TRIANGULUM_AUSTRALIS	249.6225	-64.3477	248.441517	-64.24803	258.335963	-41.727543	324.61952374	-11.529112	306.6841	54750.3809143518	2008-10-11 09:08:31	54752.6453587963	2008-10-13 15:29:19	803028010	86.0101	80	86.0421	86.0101	0	86.0481	2	2	0	2	1	0	0	76.9675	76.9675	195.6378	1	PROCESSED	57544.1744560185	2016-06-05 04:11:13	55148	2009-11-13 00:00:00	54780.7199768518	2008-11-10 17:16:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030101	We propose an 80 ks pointed observation of one of the brightest near-by hot and merging galaxy cluster, Triangulum Australis. Recent Suzaku wide-band spectroscopy reveals a very hot (kT >20 keV) thermal component in several merging clusters (RXJ1347, Abell 3667 and so on). On the other hand, relaxed cluster (such as Abell 1060 and Centaurus) show no evidence of such component. These results suggests that the very-hot component is the key aspects of merging cluster. Triangulum Australis is a bright (f ~ 1e-10 cgs), mildly hot (kT ~ 9 keV) and relatively compact (size ~20x20 arcmin2) shaped cluster. ASCA detected a hot region in the center and to the east (Markevitch et al. 1996). Combination of these characteristics makes this cluster the best candidate for our research.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	SHO OKUYAMA		JAP	3	AO3	SEARCH FOR VERY-HIGH TEMPERATURE COMPONENT IN A NEAR-BY CLUSTER, TRIANGULUM AUSTRALIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803028010/	Quick Look
310	ABELL 665	127.3329	65.7462	126.195484	65.912794	110.615683	44.954956	149.92967896	34.55444535	289.9972	56027.8062847222	2012-04-10 19:21:03	56028.5592476852	2012-04-11 13:25:19	807072030	50.3486	50	50.3526	50.3486	0	50.3561	2	2	0	2	1	0	0	47.3856	47.3856	65.049	0	PROCESSED	57605.1517939815	2016-08-05 03:38:35	56018	2012-04-01 00:00:00	56044.1669791667	2012-04-27 04:00:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072030/	Quick Look
311	NGC 3079	150.444	55.6163	149.59923	55.857396	130.078493	40.265138	157.91350273	48.36319014	294.1052	54590.7432407407	2008-05-04 17:50:16	54591.1147800926	2008-05-05 02:45:17	803039010	14.4083	100	14.4083	14.4083	0	14.4083	2	2	0	2	1	0	0	12.9538	12.9538	32.0799	0	PROCESSED	57542.4484027778	2016-06-03 10:45:42	54999	2009-06-17 00:00:00	54602.2023958333	2008-05-16 04:51:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031303	We will determine whether AGN can drive galactic-scale winds by observing NGC 3079, the best nearby candidate for such a wind. The edge-on spiral NGC 3079 hosts a Compton-thick AGN and is surrounded by a 40 kpc-scale soft X-ray nebula, the largest manifestation of outflow activity also seen in the optical and radio. Proving the outflow is AGN-driven requires Suzaku's unique abilities. We will measure the AGN luminosity using the HXD in the 15-40 keV range and the 2-10 keV band reflection spectrum to assess whether the AGN can radiatively-or-mechanically power the observed superwind. We will determine the origin of the soft X-ray nebula using the relative elemental abundances in the plasma. We can also detect any significant starburst through the 6.7 keV line emission it would create.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DAVID STRICKLAND		USA	3	AO3	NGC 3079'S 40 KPC-SCALE OUTFLOW: AGN OR STARBURST-DRIVEN?	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803039010/	Quick Look
312	CYGNUS A CLUSTER	299.7609	40.7885	299.328588	40.65123	317.589132	59.411403	76.19456446	5.8531495	241.849	54785.9049537037	2008-11-15 21:43:08	54786.9154976852	2008-11-16 21:58:19	803050010	44.6587	45	44.6587	44.6587	0	44.6587	1	1	0	1	1	0	0	42.966	42.966	87.28	0	PROCESSED	57544.3868055556	2016-06-05 09:17:00	55167	2009-12-02 00:00:00	54796.9718981482	2008-11-26 23:19:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031426	The radio galaxy Cygnus A lies in a cooling core cluster which is currently undergoing a cluster merger with a particularly simple geometry. We propose XIS spectra of the radio source/cooling core interaction region, merger shock region, and second subcluster. The Fe K emission line will be used to measure gas velocities in these 3 regions to determine the dynamics of the merger, and to constrain hydro/N-body simulations of the merger. Collisionless merger shocks may produce detectable non-equilibrium effects. We will also determine an upper limit for the rate of expansion of the X-ray bubble around the radio source, studying the interaction of the radio galaxy and X-ray gas in the only FR-II radio galaxy in a nearby cluster. HXD data will constrain inverse Compton from the radio source.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	DANIEL WIK		USA	3	AO3	PROPERTIES OF THE MERGER AND RADIO SOURCE INTERACTION IN THE CYGNUS A CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803050010/	Quick Look
313	A2163	243.8156	-6.2315	243.147928	-6.107198	243.010913	14.789433	6.59879538	30.51803676	282.2871	54696.6726851852	2008-08-18 16:08:40	54700.4008449074	2008-08-22 09:37:13	803071010	135.7864	130	135.7944	135.7864	0	135.7944	2	2	0	2	1	0	0	122.1262	122.1262	322.0615	5	PROCESSED	57543.4331597222	2016-06-04 10:23:45	55080	2009-09-06 00:00:00	54713.5071875	2008-09-04 12:10:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032023	Measurements of intracluster gas temperatures out to large radii, where much of the cluster mass resides, are of the utmost importance for the use of clusters in precision cosmology and for studies of cluster physics. Previous attempts to measure robust temperatures at cluster virial radii failed. Here, we demonstrate that such measurements are feasible now for the first time with the Suzaku X-ray CCDs, using our observation of the cluster A2204, carefully treating background and PSF. To determine the temperature profile of the cluster population as a whole, more such observations are required. We show that A2163 is the optimal complementary target for such an investigation. We, therefore, propose to observe A2163 to measure the gas temperature to 15% accuracy out to the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	THOMAS REIPRICH		EUR	3	AO3	GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS OF A2163	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803071010/	Quick Look
314	ABELL 2597	351.1561	-12.0446	350.50582	-12.319475	347.114403	-7.564991	65.23010074	-64.66820365	250.0003	56262.3308680556	2012-12-01 07:56:27	56263.5369212963	2012-12-02 12:53:10	807073020	50.0345	50	50.0585	50.0425	0	50.0345	1	1	0	1	1	0	0	44.785	44.785	104.1919	0	PROCESSED	57608.1666319444	2016-08-08 03:59:57	56018	2012-04-01 00:00:00	56336.4705902778	2013-02-13 11:17:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073020/	Quick Look
315	A2029_3	227.6311	5.4874	227.010378	5.676114	223.4982	22.349991	6.05366388	50.47243927	112.9537	55224.9801041667	2010-01-28 23:31:21	55225.6140509259	2010-01-29 14:44:14	804024030	17.9095	22	17.9175	17.9255	0	17.9095	2	2	0	2	1	0	0	8.9268	8.9268	54.7659	0	PROCESSED	57550.4118865741	2016-06-11 09:53:07	55637	2011-03-17 00:00:00	55270.9888425926	2010-03-15 23:43:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040030	Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUZURU TAWARA		JAP	4	AO4	TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024030/	Quick Look
316	NGC 4125	182.0568	65.1777	181.434624	65.455888	140.391429	57.000336	130.16762444	51.33919783	175.9017	55103.512037037	2009-09-29 12:17:20	55105.4578009259	2009-10-01 10:59:14	804047010	104.0801	100	104.0801	104.0881	0	104.0961	2	2	0	2	1	0	0	93.7257	93.7257	168.0857	0	PROCESSED	57548.726712963	2016-06-09 17:26:28	55491	2010-10-22 00:00:00	55125.5744212963	2009-10-21 13:47:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041502	Recent observations of relaxed galaxy groups have revealed ubiquitous abundance gradients, indicating large-scale mixing of the gas, possibly driven by AGN feedback. Exploiting the low background and good sensitivity of Suzaku, we have found similar gradients in two lower mass, galaxy-scale systems, which has important implications for models of feedback and chemical enrichment. We propose to observe two more isolated elliptical galaxies, thus starting to building a sample for determining the frequency and properties of such abundance gradients in early-type galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	PHILIP HUMPHREY		USA	4	AO4	ABUNDANCE GRADIENTS IN EARLY-TYPE GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804047010/	Quick Look
317	FILAMENT OF GALAXIES	238.8797	27.1312	238.361126	27.276131	228.364873	46.172986	43.89595297	49.28386381	298.9982	55406.9857060185	2010-07-29 23:39:25	55408.8592939815	2010-07-31 20:37:23	805029010	73.9387	80	73.9501	73.9447	0	73.9387	2	2	0	2	1	0	0	66.4045	66.4045	161.8557	1	PROCESSED	57552.8140972222	2016-06-13 19:32:18	55791	2011-08-18 00:00:00	55418.4520717593	2010-08-10 10:50:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050032	Warm Hot Intergalactic Medium (WHIM) is the most promising candidate for the cosmic missing baryons. Nevertheless, no concrete evidence of the presence of the WHIM has been unveiled yet. We propose a SUZAKU observation of a filament discovered through a systematic analysis of the SDSS galaxy catalogue. The observation toward a 10 Mpc long section of this filament aligned with the line of sight will provide the redshifted OVII and OVIII emission lines from the WHIM or much stronger constraint on the overdensity of the WHIM.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	HAJIME KAWAHARA		JAP	5	AO5	SEARCHING FOR MISSING BARYONS ALONG A FILAMENT OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805029010/	Quick Look
318	NGC6482	267.957	23.086	267.434837	23.097176	267.256842	46.506557	48.10607859	22.91404378	109.6205	55238.2645949074	2010-02-11 06:21:01	55239.2919444444	2010-02-12 07:00:24	804050010	46.5467	45	46.5467	46.5467	0	46.5467	2	2	0	2	1	0	0	28.5166	28.5166	88.7438	0	PROCESSED	57550.5834143518	2016-06-11 14:00:07	55622	2011-03-02 00:00:00	55251.3186458333	2010-02-24 07:38:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041513	Fossil groups present a puzzle to current theories of structure formation. Despite the low number of bright galaxies, their high velocity dispersions and gas temperatures indicate potential wells deeper than that of normal groups. Their measured c200 are high indicating very early formation epochs, which is in contradiction with the lack of cooling cores observed. We can constrain their ages by looking at the distribution of the SN Ia and II ejecta near their core. If they are formed more recently than normal groups by galaxy merging near the core, the central gas should have a reduction of SN Ia dominance, differently from what is observed in normal groups. We propose to test this with the most optimal and nearest fossil group, NGC6482, matching very well the capabilities of Suzaku.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	RENATO DUPKE		USA	4	AO4	DISCRIMINATING COMPETING MODELS FOR THE ORIGIN OF FOSSIL GROUPS OF GALAXIES WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804050010/	Quick Look
319	NGC741MOSAICE_P4	29.8808	5.7741	29.226568	5.531917	29.834623	-6.020542	152.02832852	-53.20754513	71.8261	55054.5770138889	2009-08-11 13:50:54	55054.8084953704	2009-08-11 19:24:14	804052040	11.0257	10	11.0257	11.3217	0	11.3057	3	2	0	2	1	0	0	11.3902	11.3902	19.9959	0	PROCESSED	57548.1244328704	2016-06-09 02:59:11	55448	2010-09-09 00:00:00	55081.2593055556	2009-09-07 06:13:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052040/	Quick Look
320	ABELL 426 E2	50.6767	41.5228	49.847142	41.344864	59.17553	22.199581	151.03351832	-12.94989772	90.0008	55041.7150115741	2009-07-29 17:09:37	55041.9654976852	2009-07-29 23:10:19	804057010	12.9048	10	12.9048	12.9048	0	12.9048	2	2	0	2	1	0	0	12.962	12.962	21.6399	1	PROCESSED	57547.969849537	2016-06-08 23:16:35	55419	2010-08-11 00:00:00	55050.2440277778	2009-08-07 05:51:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804057010/	Quick Look
321	ABELL 426 N6	48.8242	42.9264	47.990569	42.741631	58.170143	23.930613	149.06870737	-12.52705179	59.999	55063.8243055556	2009-08-20 19:47:00	55064.6334837963	2009-08-21 15:12:13	804068010	36.5265	30	36.5345	36.5265	0	36.5425	2	2	0	2	1	0	0	30.8843	30.8843	69.9119	0	PROCESSED	57548.3037731482	2016-06-09 07:17:26	55441	2010-09-02 00:00:00	55075.1362037037	2009-09-01 03:16:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804068010/	Quick Look
322	A76 WEST	9.903	6.838	9.256884	6.56348	11.779086	2.367721	117.68922859	-55.91332108	260	55183.8756481482	2009-12-18 21:00:56	55184.3334953704	2009-12-19 08:00:14	804088010	15.1164	15	15.1244	15.1164	0	15.1324	2	2	0	2	1	0	0	14.2066	14.2066	39.5479	0	PROCESSED	57549.8934722222	2016-06-10 21:26:36	55575	2011-01-14 00:00:00	55209.4668055556	2010-01-13 11:12:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042018	In our flux limited survey of galaxy clusters in the ROSAT All-Sky Atlas we find that about 5 - 10 percent of the galaxy clusters have a diffuse, low X-ray surface brightness. These objects could possibly be explained as dynamically very young clusters, which have not yet formed a central core. Three such clusters in our XMM-Newton study of an unbiased sub-sample of 33 galaxy clusters, REXCESS, show suprisingly high entropies in their centers which does not readily support the early formation stage. To shed more light on the nature of these clusters we propose to observe two extremely low surface brightness clusters at low redshift, for which we also have detailed optical data. SUZAKU with its low background is ideally suited for this study.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	HANS BOEHRINGER		EUR	4	AO4	SHEDDING LIGHT ON THE NATURE OF EXTREMELY LOW SURFACE BRIGHTNESS CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804088010/	Quick Look
323	A478 OFFSET D	63.1009	10.3754	62.415271	10.247963	63.081843	-10.587617	182.33525373	-28.5396849	259.0002	55612.7107986111	2011-02-20 17:03:33	55613.7362731482	2011-02-21 17:40:14	805004010	47.1066	45	47.1066	47.1066	0	47.1066	3	2	0	2	1	0	0	42.161	42.161	88.5959	1	PROCESSED	57601.0027314815	2016-08-01 00:03:56	56018	2012-04-01 00:00:00	55649.2441203704	2011-03-29 05:51:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050008	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 a representative regular cluster, Abell 478	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA	ANDREW FABIAN	JAP	5	AO5	DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805004010/	Quick Look
324	A222/223 BRIDGE	24.4438	-12.9141	23.829522	-13.168194	17.57702	-21.440022	162.54430913	-72.12239011	224.9995	55555.161099537	2010-12-25 03:51:59	55557.4654861111	2010-12-27 11:10:18	805035010	101.2149	100	101.2843	101.2149	0	101.2843	2	2	0	2	1	0	0	88.9171	88.9171	199.0699	4	PROCESSED	57554.5537268518	2016-06-15 13:17:22	55961	2012-02-04 00:00:00	55595.1387847222	2011-02-03 03:19:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050035	We propose to observe the unusual X-ray bridge connecting the two clusters of galaxies Abell 222 and Abell 223 (z=0.21). XMM observation showed the temperature to be 0.9 keV, interpreted as due to WHIM. Suzaku will observe the temperature distribution over the bridge region, which will tell us the origin of the bridge to be either WHIM or merger onset. Merger process should indicate a characteristic temperature increase. Redshifted oxygen lines, if detected, will be the clear evidence of WHIM. Joint study with weak lensing analysis will show us spatial offset of the dark matter against baryons, helping us to constrain dark matter properties.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KAORI HENMI		JAP	5	AO5	ORIGIN OF THE X-RAY BRIDGE CONNECTING THE CLUSTERS OF GALAXIES ABELL 222 AND ABELL 223	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805035010/	Quick Look
325	ABELL1835 OFFSET3	210.0673	2.8311	209.433725	3.072798	206.943622	14.143739	340.00426802	60.64916276	306.4895	55385.4673611111	2010-07-08 11:13:00	55386.9855555556	2010-07-09 23:39:12	805039010	53.6971	50	53.7201	53.7131	0	53.6971	2	2	0	2	1	0	0	44.8377	44.8377	131.1598	3	PROCESSED	57552.5941087963	2016-06-13 14:15:31	55779	2011-08-06 00:00:00	55411.2395717593	2010-08-03 05:44:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050040	We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	NOBUHIRO OKABE		JAP	5	AO5	UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805039010/	Quick Look
326	A1413_FIELD_3	179.0207	23.4251	178.377297	23.70339	169.347727	21.006295	226.37028623	76.95859752	302.9994	55347.1862037037	2010-05-31 04:28:08	55348.2079050926	2010-06-01 04:59:23	805061010	40.9225	40	40.9225	40.9385	0	40.9305	2	2	0	2	1	0	0	32.9944	32.9944	88.2578	0	PROCESSED	57553.3965856482	2016-06-14 09:31:05	55287	2010-04-01 00:00:00	55393.4280208333	2010-07-16 10:16:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805061010/	Quick Look
327	A383_FIELD_2	41.9447	-3.4083	41.315431	-3.616408	38.400744	-18.662791	177.53047769	-53.46482162	60.9996	55389.1380208333	2010-07-12 03:18:45	55390.062662037	2010-07-13 01:30:14	805063010	43.3415	40	43.3575	43.3415	0	43.3575	2	2	0	2	1	0	0	39.2589	39.2589	79.8749	0	PROCESSED	57552.6168055556	2016-06-13 14:48:12	55287	2010-04-01 00:00:00	55411.2445601852	2010-08-03 05:52:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805063010/	Quick Look
328	ABELL1835 OFFSET4	210.2225	3.0556	209.589504	3.296921	207.010904	14.408613	340.51868842	60.75430015	304.9986	55390.9913194444	2010-07-13 23:47:30	55392.4001736111	2010-07-15 09:36:15	805040010	48.8185	50	48.8265	48.8265	0	48.8185	2	2	0	2	1	0	0	43.9631	43.9631	121.6839	4	PROCESSED	57552.6731828704	2016-06-13 16:09:23	55793	2011-08-20 00:00:00	55427.1333796296	2010-08-19 03:12:04	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050040	We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	NOBUHIRO OKABE		JAP	5	AO5	UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805040010/	Quick Look
329	A1914_OFFSET2	216.7383	37.763	216.226328	37.986791	196.709268	48.583272	66.87630822	67.3091462	329.9943	55363.4747569444	2010-06-16 11:23:39	55364.3800115741	2010-06-17 09:07:13	805092010	28.5462	40	28.5542	28.5542	0	28.5462	2	2	0	2	1	0	0	25.8343	25.8343	78.204	0	PROCESSED	57552.3515856482	2016-06-13 08:26:17	55766	2011-07-24 00:00:00	55399.3275231482	2010-07-22 07:51:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	053087	We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA	ERIC MILLER	JUS	5	AO5	THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805092010/	Quick Look
330	CENA N LOBE 3	201.1567	-39.315	200.435438	-39.054679	215.153584	-28.04573	309.90401242	23.10702351	110.949	56316.327349537	2013-01-24 07:51:23	56318.4140046296	2013-01-26 09:56:10	807134010	81.984	75	81.992	81.992	0	81.984	2	2	0	2	1	0	0	73.8838	73.8838	180.2478	2	PROCESSED	57608.6528356482	2016-08-08 15:40:05	56708	2014-02-20 00:00:00	56342.7001157407	2013-02-19 16:48:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070127	Radio source Centaurus A is the closest active galaxy in the Universe (3.7 Mpc). It is surrounded by poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose Chandra follow-up of four regions in the Southern and Northern lobes where Suzaku time was allocated. We also propose joint Chandra-Suzaku observation toward interacting filamentary region where ASCA found a hint of X-ray emission. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in inhomogeneous and multi-phase plasma. The obtained results are guaranteed to improve our knowledge regarding not only the Centaurus A, but all jetted active galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	S	YASUYUKI TANAKA		JAP	7	AO7	STUDYING GIANT FILAMENTARY LOBES OF CENTAURUS A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807134010/	Quick Look
331	NGC 2300 OFFSET	116.7261	85.6829	112.689891	85.799301	94.232742	62.638745	127.68344404	28.08274711	339.9009	55235.4123148148	2010-02-08 09:53:44	55235.7606365741	2010-02-08 18:15:19	804031010	19.196	20	19.196	19.196	0	19.196	1	1	0	1	1	0	0	17.1477	17.1477	30.0879	0	PROCESSED	57550.5104282407	2016-06-11 12:15:01	55633	2011-03-13 00:00:00	55266.1898148148	2010-03-11 04:33:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040055	We propose to observe the NGC 2300 group for 100 ks and a offset pointing for 200 ks to evaluate the background emission from the Galaxy. The purpose of the observations are to measure O, Mg, Si and Fe abundances of intragaractic medium to study metal synthesis in this small group of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KYOKO MATSUSHITA		JAP	4	AO4	O, MG, S AND FE ABUNDANCES OF INTRAGROUP MEDIUM IN THE NGC 2300 GROUP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804031010/	Quick Look
332	MKW 4-OFFSET1	181.1304	2.2289	180.489911	2.507266	180.147119	2.494288	276.66004128	62.68282085	114.5816	55528.2862847222	2010-11-28 06:52:15	55530.2501967593	2010-11-30 06:00:17	805081010	79.4261	80	79.4261	79.4261	0	79.4261	2	2	0	2	1	0	0	68.2112	68.2112	169.6679	2	PROCESSED	57554.312025463	2016-06-15 07:29:19	55909	2011-12-14 00:00:00	55543.4043402778	2010-12-13 09:42:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051525	We propose a set of two 19 arcmin offset observations for the galaxy groups MKW 4 to measure spatially resolved density, temperature and iron abundance out to r_{500}. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to its brightness, regularity and low temperature, the object is an ideal candidate for an offset observation of its peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	FABIO GASTALDELLO		USA	5	AO5	THE OUTSKIRTS OF MKW 4	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805081010/	Quick Look
333	PKS 0745-191	116.3632	-19.0871	115.808852	-18.964679	122.979801	-39.556071	236.01662317	2.71025988	294.0001	55316.6424189815	2010-04-30 15:25:05	55317.3675231482	2010-05-01 08:49:14	805085010	34.9999	35	34.9999	34.9999	0	34.9999	2	2	0	2	1	0	0	32.7804	32.7804	62.6419	2	PROCESSED	57551.3324074074	2016-06-12 07:58:40	55696	2011-05-15 00:00:00	55330.1114236111	2010-05-14 02:40:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051526	Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MATTHEW GEORGE		USA	5	AO5	BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805085010/	Quick Look
334	A1914_OFFSET4	216.4424	37.6372	215.928949	37.861845	196.491265	48.360248	66.78881215	67.57279807	134.0011	55566.4311574074	2011-01-05 10:20:52	55566.8258912037	2011-01-05 19:49:17	805094020	17.3531	12	17.3531	17.3611	0	17.3691	2	2	0	2	1	0	0	16.0606	16.0606	34.1	0	PROCESSED	57600.564375	2016-07-31 13:32:42	55995	2012-03-09 00:00:00	55627.1583333333	2011-03-07 03:48:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	053087	We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA	ERIC MILLER	JUS	5	AO5	THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805094020/	Quick Look
335	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
336	OPHIUCHUS CLUSTER BG	257.0147	-25.0612	256.247464	-24.996818	258.237934	-2.148508	358.58755189	9.10838139	89.7146	54183.5662268518	2007-03-24 13:35:22	54183.9169444444	2007-03-24 22:00:24	801030010	15.2983	15	15.3063	15.3063	0	15.2983	2	2	0	2	1	0	0	14.6351	14.6351	30.296	0	PROCESSED	57537.9841898148	2016-05-29 23:37:14	54736	2008-09-27 00:00:00	54209.5187384259	2007-04-19 12:26:59	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010065	The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUTAKA FUJITA		JAP	1	AO1	PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801030010/	Quick Look
337	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
338	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
339	ABELL 1795 Far South	207.2227	26.2001	206.644395	26.44826	194.131601	34.631873	32.0541753	77.13779505	129.4115	53716.5361921296	2005-12-12 12:52:07	53717.4168865741	2005-12-13 10:00:19	800012050	40.1206	30	40.1366	40.1526	40.1206	40.1366	2	2	2	2	1	0	0	39.4373	39.4373	76.0819	1	PROCESSED	57532.4477314815	2016-05-24 10:44:44	54247	2007-05-27 00:00:00	54039.1460069445	2006-10-31 03:30:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012050/	Quick Look
340	FORNAX OFFSET2	54.357	-35.2813	53.876494	-35.444531	38.536942	-52.548461	236.43807346	-53.85479755	63.6004	54663.2151388889	2008-07-16 05:09:48	54664.1793287037	2008-07-17 04:18:14	803007010	40.6477	30	40.678	40.6717	0	40.6477	2	2	0	2	1	0	0	34.8358	34.8358	83.2979	0	PROCESSED	57595.6271875	2016-07-26 15:03:09	55188	2009-12-23 00:00:00	54822.5201736111	2008-12-22 12:29:03	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030036	We proposeto observe 5 offset pointings of the Fornax cluster for 160 ks with Suzaku. The purpose of the observation is to determine O, Mg and Fe distribution of the intracluster medium up to 0.15-0.2 r180 and to study the origin of the metals.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	3	AO3	METAL DISTRIBUTION OF THE FORNAX CLUSTER UP TO 0.2R180.	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803007010/	Quick Look
341	ABELL 3112	49.4982	-44.2507	49.063827	-44.432376	25.5219	-58.972557	252.95298598	-56.06981795	43.5004	56466.5743634259	2013-06-23 13:47:05	56468.5418055556	2013-06-25 13:00:12	808068010	119.1247	200	119.1247	119.1247	0	119.1247	2	2	0	2	1	0	0	114.5618	114.5618	169.9418	0	PROCESSED	57611.6340856482	2016-08-11 15:13:05	56848	2014-07-10 00:00:00	56481.8003356482	2013-07-08 19:12:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081522	The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ESRA BULBUL		USA	8	AO8	CHEMICAL EVOLUTION HISTORY OF A COOL CORE CLUSTER A3112 OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808068010/	Quick Look
342	RXCJ0243.6-4834	40.9015	-48.5654	40.467277	-48.776586	11.225079	-59.344649	265.11995755	-59.50535864	228.2843	55191.5472685185	2009-12-26 13:08:04	55192.0001967593	2009-12-27 00:00:17	804001010	13.2059	10	13.2139	13.2059	0	13.2219	2	2	0	2	1	0	0	10.5448	10.5448	39.1299	0	PROCESSED	57549.9594097222	2016-06-10 23:01:33	55575	2011-01-14 00:00:00	55209.1119328704	2010-01-13 02:41:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040005	We propose Suzaku observations of 8 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. With a total exposure time of 80 ksec, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	4	AO4	LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804001010/	Quick Look
343	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
344	ABELL2811	10.4703	-28.5552	9.856516	-28.82929	357.097887	-30.138768	358.34166022	-87.45073592	232.1065	53702.1678240741	2005-11-28 04:01:40	53702.8814699074	2005-11-28 21:09:19	800005010	30.6546	25	30.6626	30.6826	30.6546	30.6659	2	2	2	2	1	0	0	28.3254	28.3254	61.656	0	PROCESSED	57528.0937268518	2016-05-20 02:14:58	54247	2007-05-27 00:00:00	54038.5109722222	2006-10-30 12:15:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001025	We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYUKI TAMURA		JAP	0	SWG	THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800005010/	Quick Look
345	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
346	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
347	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
348	MACSJ0717.5+3547	109.4283	37.7329	108.583729	37.823554	105.833167	15.353649	180.28338253	21.07400371	90.0014	55841.8814699074	2011-10-07 21:09:19	55844.0440046296	2011-10-10 01:03:22	806006010	100.5473	100	100.5473	100.5553	0	100.5553	2	2	0	2	1	0	0	93.847	93.847	186.8279	1	PROCESSED	57603.4085763889	2016-08-03 09:48:21	56240	2012-11-09 00:00:00	55872.2982523148	2011-11-07 07:09:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060016	MACSJ0717.5+3547 is a forming hot cluster located at z=0.55. Chandra observation resolved a >20 keV hot component near its center, in addition to the average ICM temperature of 11.6 keV. With the most luminous radio halo observed to date, the cluster is in a moment of major merging event. It is also associated with a stream of galaxies oriented to the south east. We propose a Suzaku observation with an exposure of 100 ks, aiming at; confirming the bright > 20 keV component, the very hot component (e.g. Nakazawa+ 2010) evidencing the strong merger, and obtain temperature map of the dim diffuse X-ray observed to the south east and the south west to resolve the nature of these emission. With these observation, merging orientation and phase in this very hot cluster can be resolved.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KAZUHIRO NAKAZAWA		JAP	6	AO6	OBSERVING THE FORMATION EPOCH OF A HOT CLUSTER : SUZAKU OBSERVATION OF MACSJ0717.5+3547	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806006010/	Quick Look
349	A426	49.9554	41.5039	49.127963	41.323287	58.608686	22.329679	150.58326426	-13.26576669	260.2176	53767.568900463	2006-02-01 13:39:13	53768.5294560185	2006-02-02 12:42:25	800010010	50.3986	50	50.4066	50.4066	50.3986	50.4066	2	2	2	2	1	0	0	54.4364	54.4364	82.9758	0	PROCESSED	57532.8781365741	2016-05-24 21:04:31	54247	2007-05-27 00:00:00	54041.0862152778	2006-11-02 02:04:09	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001036	A426 is the X-ray brightest cluster in the Sky. The core is X-ray peaked, has a short radiative cooling time, a temperature drop and a central radio source which is blowing bubbles in the intracluster medium. A radio minihalo extends over the central 6 arcmin. A coincident power-law component is seen in deep Chandra data. This is likely to be inverse Compton emission from the electron population responsible for the radio emission. The region is expected to be a luminous, extended, hard X-ray source easily detectable by the Suzaku HXD. Confirmation of this hard X-ray component will enable the magnetic field to be securely determined in the intracluster gas.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ANDREW FABIAN		JAP	0	SWG	THE HARD X-RAY FLUX FROM THE CORE OF THE PERSEUS CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800010010/	Quick Look
350	COMA OUTSKIRTS5	193.6628	28.7109	193.057562	28.981718	179.928046	31.541197	98.9627641	88.26548083	115.9998	55903.9110532407	2011-12-08 21:51:55	55904.722349537	2011-12-09 17:20:11	806024010	31.635	30	31.659	31.651	0	31.635	2	2	0	2	1	0	0	29.4491	29.4491	70.0899	0	PROCESSED	57604.0811226852	2016-08-04 01:56:49	56284	2012-12-23 00:00:00	55915.2478587963	2011-12-20 05:56:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060099	In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKUYA SATO		JAP	6	AO6	STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806024010/	Quick Look
351	ABELL 773	139.6415	51.5835	138.770726	51.794221	124.818527	33.970374	166.25628799	43.50358503	276.9979	55683.2110185185	2011-05-02 05:03:52	55684.0730208333	2011-05-03 01:45:09	806027020	47.2223	50	47.2303	47.2223	0	47.2383	2	2	0	2	1	0	0	46.5115	46.5115	74.4719	0	PROCESSED	57601.9085185185	2016-08-01 21:48:16	55652	2011-04-01 00:00:00	55697.3168981482	2011-05-16 07:36:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806027020/	Quick Look
352	CENCL OFFSET2	192.2009	-41.1804	191.510431	-40.907877	208.999282	-32.736275	302.39848339	21.68862024	106.52	53733.2507407407	2005-12-29 06:01:04	53734.3543865741	2005-12-30 08:30:19	800016010	43.2773	40	43.2853	43.2853	43.2773	43.2933	2	2	2	2	1	0	0	35.2531	35.2531	95.332	1	PROCESSED	57532.5900578704	2016-05-24 14:09:41	54247	2007-05-27 00:00:00	54039.6041203704	2006-10-31 14:29:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001070	A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	0	SWG	OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800016010/	Quick Look
353	NGC 4636	190.7243	2.7556	190.086173	3.029415	188.766391	6.778722	297.77503713	65.54179663	112.2967	53710.1073726852	2005-12-06 02:34:37	53711.9446643518	2005-12-07 22:40:19	800018010	79.201	80	79.201	79.201	79.201	79.201	2	2	2	2	1	0	0	75.7771	75.7771	158.7278	2	PROCESSED	57532.4099421296	2016-05-24 09:50:19	54247	2007-05-27 00:00:00	54038.9551388889	2006-10-30 22:55:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001083	We propose to observe NGC 4636 for 50~ksec in a single pointing, to determine the chemical evolution of elliptical galaxies via the determination of the spatially resolved abundance of Oxygen and other elements. Being one of the most X-ray luminous ellipticals, and having been observed by both Chandra and XMM, this is also an important target to compare the capabilities of the three observatories and interpret the results of the Suzaku XIS in light of the source spectrum provided by the XMM RGS.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ENECTALI FIGUEROA-FELICIANO		JAP	0	SWG	OBSERVATION OF THE X-RAY LUMINOUS EXTENDED EARLY-TYPE GALAXY NGC 4636	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800018010/	Quick Look
354	AWM7 WEST OFFSET	43.2295	41.594	42.421509	41.389857	53.412323	23.911285	146.06522235	-15.7568529	90.4999	53953.2407060185	2006-08-06 05:46:37	53954.2343171296	2006-08-07 05:37:25	801037010	39.8177	40	39.8497	39.8177	39.8497	39.8497	2	2	2	2	1	0	0	38.1089	38.1089	85.8359	1	PROCESSED	57535.2509375	2016-05-27 06:01:21	54394	2007-10-21 00:00:00	54020.7562384259	2006-10-12 18:08:59	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010076	The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKAYA OHASHI		JAP	1	AO1	SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801037010/	Quick Look
355	ABELL 2667	357.7341	-26.0226	357.087227	-26.30077	347.004408	-22.85609	34.17814736	-76.43580815	64.8804	55722.9055208333	2011-06-10 21:43:57	55724.4196990741	2011-06-12 10:04:22	806029020	51.6577	50	51.6657	51.6577	0	51.6721	2	2	0	2	1	0	0	45.656	45.656	130.802	1	PROCESSED	57602.2808333333	2016-08-02 06:44:24	55652	2011-04-01 00:00:00	55757.7009027778	2011-07-15 16:49:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806029020/	Quick Look
356	COMA E6.5	196.9526	27.8857	196.354379	28.152377	183.408228	32.112773	45.6576416	86.29162208	279.9993	55731.5902199074	2011-06-19 14:09:55	55732.0578935185	2011-06-20 01:23:22	806037010	14.9596	15	14.9676	14.9596	0	14.9676	1	1	0	1	1	0	0	13.6142	13.6142	40.3999	0	PROCESSED	57602.3577314815	2016-08-02 08:35:08	55652	2011-04-01 00:00:00	55770.17125	2011-07-28 04:06:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806037010/	Quick Look
357	COMA SW7	193.2936	26.7739	192.684688	27.045132	180.600519	29.664204	350.54999025	89.47529971	314.5993	55737.124212963	2011-06-25 02:58:52	55737.4447106482	2011-06-25 10:40:23	806051010	15.4152	15	15.4152	15.4232	0	15.4232	1	1	0	1	1	0	0	15.0368	15.0368	27.6719	0	PROCESSED	57602.4087847222	2016-08-02 09:48:39	55652	2011-04-01 00:00:00	55795.0185763889	2011-08-22 00:26:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806051010/	Quick Look
358	A2256	256.0138	78.7112	256.73222	78.776756	102.386288	77.234603	111.08264828	31.72462704	207.9671	54049.8560069445	2006-11-10 20:32:39	54052.0834722222	2006-11-13 02:00:12	801061010	95.5111	100	95.5111	95.5111	0	95.5111	2	2	0	2	1	0	0	103.5789	103.5789	192.4418	4	PROCESSED	57536.1203009259	2016-05-28 02:53:14	54456	2007-12-22 00:00:00	54089.4338425926	2006-12-20 10:24:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010139	A2256 is a nearby (z=0.058) rich cluster with strong X-ray emission. The cluster has variety of indications of a on-going merger; two peaks separated by 3.5 arcmin are clearly visible near the center of X-ray emission, gas temperature map show sub structure and a cold front etc. The velocity distribution of member galaxies also exhibits two or three sub groups in this cluster. We measure the bulk motion of the hot gas using Suzaku XIS, in particular, about 2000km/s velocity difference between the main-cluster and the sub-cluster is the target. We also aim to search for hard X-ray emission claimed by previous missions with Suzaku HXD.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KIYOSHI HAYASHIDA		JAP	1	AO1	BULK MOTION AND NON THERMAL PROCESS IN THE MERGING CLUSTER A2256	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801061010/	Quick Look
359	30 DORADUS	84.6512	-69.1008	84.737262	-69.126573	305.902613	-86.759222	279.46621821	-31.68092384	162.7542	55895.6278472222	2011-11-30 15:04:06	55897.0640162037	2011-12-02 01:32:11	806052010	101.6448	100	101.6528	101.6528	0	101.6448	2	2	0	2	1	0	0	89.0823	89.0823	124.076	0	PROCESSED	57604.044837963	2016-08-04 01:04:34	56281	2012-12-20 00:00:00	55907.9795486111	2011-12-12 23:30:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061322	We propose a deep Suzaku observation of 30 Doradus to provide a direct X-ray measurement of the chemical enrichment in the enclosed hot gas. The soft X-ray sensitivity and spectral resolution of this observation will allow us to measure key elemental abundances and thus to test models for metal yields of massive stars. We will determine the spatial variation in the thermal and chemical properties of the hot gas and the effect on the global estimation of the chemical enrichment from an integrated spectrum, as would be obtained for a distant starburst region. We will also estimate the mass-loading from the general interstellar medium --- a key parameter for determining the evolution of the hot gas. The results will serve as an observational benchmark for understanding massive star feedback.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	Q. DANIEL WANG		USA	6	AO6	X-RAY SPECTROSCOPIC MAPPING OF 30 DORADUS: CHEMICAL ENRICHMENT BY MASSIVE STARS IN A CLOSED BOX	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806052010/	Quick Look
360	RCS131723-0201.3	199.3422	-2.034	198.698505	-1.770799	198.620431	5.687336	316.04491283	60.17589221	291.8811	55756.3454513889	2011-07-14 08:17:27	55756.9585532407	2011-07-14 23:00:19	806078010	24.921	25	24.921	24.921	0	24.921	2	2	0	2	1	0	0	23.1205	23.1205	52.9619	1	PROCESSED	57602.5803009259	2016-08-02 13:55:38	56163	2012-08-24 00:00:00	55783.6867939815	2011-08-10 16:28:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061533	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AMALIA HICKS		USA	6	AO6	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806078010/	Quick Look
361	UGC03957 WEST	114.5487	55.2415	113.541037	55.354916	106.445391	33.192967	162.38027408	28.51701147	289.9984	56004.175150463	2012-03-18 04:12:13	56005.2466550926	2012-03-19 05:55:11	806093010	48.2169	45	48.2249	48.2169	0	48.2249	1	1	0	1	1	0	0	46.846	46.846	92.5679	0	PROCESSED	57604.9538773148	2016-08-04 22:53:35	56388	2013-04-06 00:00:00	56020.0984837963	2012-04-03 02:21:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062024	Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	BRENDA MIRANDA OCEJO		EUR	6	AO6	MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806093010/	Quick Look
362	SERSIC 159-03	348.4959	-42.7314	347.802109	-43.003937	330.666566	-34.355163	348.33340728	-64.81387916	47.3295	53851.5323611111	2006-04-26 12:46:36	53853.2668055556	2006-04-28 06:24:12	801093010	67.7843	70	67.8003	67.8003	67.7843	67.7923	2	2	2	2	1	0	0	41.5833	41.5833	149.8278	2	PROCESSED	57533.6210532407	2016-05-25 14:54:19	54400	2007-10-27 00:00:00	53907.8625231482	2006-06-21 20:42:02	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012045	We propose to observe the cluster of galaxies Sersic 159-03 using a total exposure time of 70 ks to investigate the soft excess emission previously detected in the observations with ROSAT and XMM-Newton. The superior redistribution function of Suzaku will allow us to determine whether the O VII line emission detected with XMM-Newton is of local (Galactic) origin or is emitted by the warm-hot intergalactic medium (WHIM) in the vicinity of the cluster. The strong soft emission around this cluster together with the much improved response function of the XIS detectors at low energies make Sersic 159-03 the most promising target to unambiguously detect the WHIM for the first time in emission with Suzaku.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JELLE KAASTRA		EUR	1	AO1	O VII LINE EMISSION IN SERSIC 159-03 - WHIM OR GALACTIC ORIGIN?	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801093010/	Quick Look
363	FORNAX CLUSTER N30'	54.7324	-34.9521	54.250694	-35.113851	39.207877	-52.359999	235.87381769	-53.55297023	245	54479.2031134259	2008-01-14 04:52:29	54480.3542708333	2008-01-15 08:30:09	802021010	55.8107	53	55.8107	55.8107	0	55.8107	2	2	0	2	1	0	0	58.3441	58.3441	99.4438	2	PROCESSED	57541.3134259259	2016-06-02 07:31:20	54864	2009-02-02 00:00:00	54490.3658680556	2008-01-25 08:46:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020038	To study chemical evolution of groups and clusters of galaxies, observations of outer regions are the most important. The surface brightness of these regions is very low. Thereofre, to derive metal abundances of the intracluster medium, Suzaku has an advantage due to its low stable background. We propose to observe two groups of galaxies and 1 clusters of galaxies whose central regions were observed during SWG time. The total exposure is 180 ks, with 5 pointings.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KYOKO MATSUSHITA		JAP	2	AO2	DETERMINATION OF METAL ABUNDANCES OF OUTSKIRTS OF CLUSTERS AND GROUPS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802021010/	Quick Look
364	NGC 4636 NORTH	190.6832	3.0555	190.045327	3.32935	188.609453	7.038209	297.61641621	65.83736523	111.9967	54441.2091087963	2007-12-07 05:01:07	54443.0530555556	2007-12-09 01:16:24	802022010	71.4294	67	0	71.4294	0	71.4294	0	2	0	2	1	0	0	61.781	61.781	159.3101	3	PROCESSED	57540.8428703704	2016-06-01 20:13:44	55000	2009-06-18 00:00:00	54633.6943402778	2008-06-16 16:39:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020038	To study chemical evolution of groups and clusters of galaxies, observations of outer regions are the most important. The surface brightness of these regions is very low. Thereofre, to derive metal abundances of the intracluster medium, Suzaku has an advantage due to its low stable background. We propose to observe two groups of galaxies and 1 clusters of galaxies whose central regions were observed during SWG time. The total exposure is 180 ks, with 5 pointings.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KYOKO MATSUSHITA		JAP	2	AO2	DETERMINATION OF METAL ABUNDANCES OF OUTSKIRTS OF CLUSTERS AND GROUPS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802022010/	Quick Look
365	THE MOON	142.9239	10.1507	142.252683	10.371816	141.955643	-4.265217	222.87402657	40.10832518	105.6986	56975.5846296296	2014-11-14 14:01:52	56975.7154166667	2014-11-14 17:10:12	809001230	5.1848	45	5.1848	5.2128	0	5.2208	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7753009259	2016-08-16 18:36:26	57358	2015-12-02 00:00:00	56992.4173148148	2014-12-01 10:00:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001230/	Quick Look
366	A2052_GALACTIC_1	225.6293	8.2927	225.017778	8.488428	220.521255	24.436359	7.81905694	53.73503279	292.5625	54295.7150810185	2007-07-14 17:09:43	54296.5765509259	2007-07-15 13:50:14	802038010	33.7334	30	33.7334	33.7334	0	33.7334	1	1	0	1	1	0	0	30.5272	30.5272	74.4239	1	PROCESSED	57539.2674305556	2016-05-31 06:25:06	54709	2008-08-31 00:00:00	54339.4114583333	2007-08-27 09:52:30	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020119	We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YOH TAKEI		JAP	2	AO2	DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802038010/	Quick Look
367	ABELL 3395	96.7698	-54.5043	96.516816	-54.472103	108.474853	-77.510268	263.27498484	-25.21804833	150.0003	54815.4865046296	2008-12-15 11:40:34	54817.3168865741	2008-12-17 07:36:19	803020010	104.3469	100	104.3469	104.3469	0	104.3469	2	2	0	2	1	0	0	81.661	81.661	158.1299	3	PROCESSED	57545.0306828704	2016-06-06 00:44:11	55210	2010-01-14 00:00:00	54840.5412268518	2009-01-09 12:59:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030078	We propose to observe a merging cluster Abell 3395 with Suzaku for 100 ks. Abell 3395 has two X-ray emission peaks in the ICM, and they can have a large velocity difference of 3000 km/s at maximum. From the line shift of iron K line, we detect the bulk motion of the ICM, and compare it with the velocity distribution of galaxies. The difference of velocity distributions between the ICM and galaxies reflects the difference of their cross sections during the cluster merging.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MADOKA KAWAHARADA		JAP	3	AO3	COMPARISON BETWEEN VELOCITY DISTRIBUTIONS OF ICM AND GALAXIES IN A MERGING CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803020010/	Quick Look
368	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
369	PKS 0745-191	116.9737	-19.0727	116.418821	-18.947622	123.702706	-39.408553	236.29361594	3.21678926	294.0001	54232.5006712963	2007-05-12 12:00:58	54233.2258564815	2007-05-13 05:25:14	802062030	30.7942	30	30.8022	30.7942	0	30.8022	2	2	0	2	1	0	0	26.6388	26.6388	62.6301	0	PROCESSED	57538.6331134259	2016-05-30 15:11:41	54695	2008-08-17 00:00:00	54245.5042592593	2007-05-25 12:06:08	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021440	PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ANDREW YOUNG		USA	2	AO2	PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062030/	Quick Look
370	RXCJ2157.4-0747 NW	329.1863	-7.8673	328.525365	-8.105597	328.55802	4.374692	49.60582387	-44.43308021	249.9998	56972.0423726852	2014-11-11 01:01:01	56972.5418171296	2014-11-11 13:00:13	809020010	23.1307	20	23.1307	23.1307	0	23.1307	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7608101852	2016-08-16 18:15:34	57352	2015-11-26 00:00:00	56986.4053819444	2014-11-25 09:43:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090049	About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	9	AO9	PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809020010/	Quick Look
371	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
372	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
373	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
374	COMA11	194.6305	28.3939	194.027281	28.663593	180.9862	31.643484	72.26601068	87.98563538	292.5148	54270.6441782407	2007-06-19 15:27:37	54272.0078009259	2007-06-21 00:11:14	802082010	53.0217	50	53.0217	53.0217	0	53.0217	2	2	0	2	1	0	0	46.6673	46.6673	117.806	2	PROCESSED	57539.0191203704	2016-05-31 00:27:32	54695	2008-08-17 00:00:00	54322.5438888889	2007-08-10 13:03:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	024438	Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JOEL BREGMAN	Yoh Takei	USJ	2	AO2	THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802082010/	Quick Look
375	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
376	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
377	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
378	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
379	A1631_W	193.0037	-15.2462	192.346534	-14.974562	197.903914	-8.910337	303.13836962	47.6253175	112.9992	56305.7238541667	2013-01-13 17:22:21	56306.3738194444	2013-01-14 08:58:18	807006010	21.0052	20	21.0212	21.0052	0	21.027	2	2	0	2	1	0	0	18.5999	18.5999	56.1539	0	PROCESSED	57608.4939351852	2016-08-08 11:51:16	56703	2014-02-15 00:00:00	56337.5213541667	2013-02-14 12:30:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070029	In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	7	AO7	PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807006010/	Quick Look
380	PERSEUS F_2	49.9481	41.7834	49.118842	41.602757	58.6868	22.59977	150.42037818	-13.03556783	257.3692	56324.1634259259	2013-02-01 03:55:20	56324.4342939815	2013-02-01 10:25:23	807019010	17.2086	15	17.2156	17.2156	0	17.2086	1	1	0	1	1	0	0	18.5555	18.5555	23.3999	0	PROCESSED	57610.4952314815	2016-08-10 11:53:08	56731	2014-03-15 00:00:00	56365.4862731482	2013-03-14 11:40:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070056	We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKAYUKI TAMURA		JAP	7	AO7	GAS MOTION IN THE PERSEUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807019010/	Quick Look
381	PERSEUS S1_2	49.8718	41.2522	49.04624	41.071281	58.468323	22.105155	150.6720925	-13.51034913	256.4607	56333.5592939815	2013-02-10 13:25:23	56334.2077546296	2013-02-11 04:59:10	807020010	24.4245	25	24.4485	24.4245	0	24.4485	1	1	0	1	1	0	0	23.7447	23.7447	55.9999	0	PROCESSED	57610.5627083333	2016-08-10 13:30:18	56731	2014-03-15 00:00:00	56365.492662037	2013-03-14 11:49:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070056	We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKAYUKI TAMURA		JAP	7	AO7	GAS MOTION IN THE PERSEUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807020010/	Quick Look
382	ABELL 3395 N	96.6064	-54.3394	96.351199	-54.307997	107.885857	-77.369468	263.07484149	-25.27687082	220.9999	56329.4933449074	2013-02-06 11:50:25	56330.7758564815	2013-02-07 18:37:14	807031010	46.9751	45	46.98	46.9751	0	46.9861	2	2	0	2	1	0	0	42.0083	42.0083	110.7998	2	PROCESSED	57610.5772337963	2016-08-10 13:51:13	56715	2014-02-27 00:00:00	56349.5329398148	2013-02-26 12:47:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070072	We propose observations of north and south regions of merging cluster Abell 3395 (A3395), which have high temperature intracluster gas, with each exposure time of 45 ks in order to obtain a detailed temperature distribution in these regions. A3395 is a very complex system, which is composed of three subclusters (A3395 NE, SW and NW) and a bridge structure which joining the A3395 NE and NW subclusters. We can obtain the information of the merging direction and the structure formation in A3395 from the detailed high-accuracy temperature distribution. In addition, it might be possible to get from this observations some information of the hot gas filling the supercluster which includes A3395.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NOBUHIRO TANAKA		JAP	7	AO7	INVESTIGATION OF TEMPERATURE DISTRIBUTION OF OUTER REGIONS IN MERGING CLUSTER ABELL 3395	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807031010/	Quick Look
383	ABELL 3395 S	96.923	-54.6479	96.67195	-54.614958	109.024535	-77.630718	263.45062321	-25.16108018	230.2008	56339.3357060185	2013-02-16 08:03:25	56340.1778703704	2013-02-17 04:16:08	807032010	47.1849	45	47.1849	47.1849	0	47.1849	2	2	0	2	1	0	0	49.7509	49.7509	72.7539	2	PROCESSED	57610.6116898148	2016-08-10 14:40:50	56717	2014-03-01 00:00:00	56349.6397569444	2013-02-26 15:21:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070072	We propose observations of north and south regions of merging cluster Abell 3395 (A3395), which have high temperature intracluster gas, with each exposure time of 45 ks in order to obtain a detailed temperature distribution in these regions. A3395 is a very complex system, which is composed of three subclusters (A3395 NE, SW and NW) and a bridge structure which joining the A3395 NE and NW subclusters. We can obtain the information of the merging direction and the structure formation in A3395 from the detailed high-accuracy temperature distribution. In addition, it might be possible to get from this observations some information of the hot gas filling the supercluster which includes A3395.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NOBUHIRO TANAKA		JAP	7	AO7	INVESTIGATION OF TEMPERATURE DISTRIBUTION OF OUTER REGIONS IN MERGING CLUSTER ABELL 3395	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807032010/	Quick Look
384	CENA LOBE BGD2	197.06	-39.3239	196.354066	-39.057193	211.892811	-29.411895	306.47248435	23.43231323	291.4078	56123.1069212963	2012-07-15 02:33:58	56123.5835300926	2012-07-15 14:00:17	807043010	21.2772	20	21.2772	21.2772	0	21.2772	1	1	0	1	1	0	0	19.4729	19.4729	41.1679	0	PROCESSED	57606.6117476852	2016-08-06 14:40:55	56018	2012-04-01 00:00:00	56142.2269675926	2012-08-03 05:26:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070106	Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LUKASZ STAWARZ		JAP	7	AO7	STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807043010/	Quick Look
385	SDSS J1302+4729	195.5068	47.4831	194.946247	47.751657	168.926268	48.423966	117.80880843	69.53967787	316.2365	56076.2710648148	2012-05-29 06:30:20	56076.7058217593	2012-05-29 16:56:23	807060010	20.427	20	20.427	20.427	0	20.427	1	1	0	1	1	0	0	24.66	24.66	37.5599	1	PROCESSED	57605.5578240741	2016-08-05 13:23:16	56500	2013-07-27 00:00:00	56134.0735300926	2012-07-26 01:45:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071512	Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ERIC MILLER		USA	7	AO7	FINDING FOSSIL GROUPS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807060010/	Quick Look
386	ANTLIA E5	159.3469	-35.3315	158.776481	-35.071439	177.451568	-40.165459	274.29394045	19.97884062	279.4997	56095.3697337963	2012-06-17 08:52:25	56096.5972916667	2012-06-18 14:20:06	807070010	46.7814	45	46.7894	46.7814	0	46.7974	2	2	0	2	1	0	0	41.0617	41.0617	106.0579	2	PROCESSED	57605.7158333333	2016-08-05 17:10:48	56590	2013-10-25 00:00:00	56219.6892361111	2012-10-19 16:32:30	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071521	We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	7	AO7	MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807070010/	Quick Look
387	RCS0442-2815	70.5602	-28.2499	70.060746	-28.343732	62.940418	-49.88298	228.44078987	-39.40072076	273.8381	54903.705462963	2009-03-13 16:55:52	54905.2669444444	2009-03-15 06:24:24	803060010	52.3573	40	52.3573	52.3573	0	52.3573	2	2	0	2	1	0	0	47.4137	47.4137	134.8779	1	PROCESSED	57545.8322222222	2016-06-06 19:58:24	55329	2010-05-13 00:00:00	54917.4174652778	2009-03-27 10:01:09	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031441	Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	3	AO3	COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803060010/	Quick Look
388	A496 P-CENTER	68.4146	-13.2791	67.835234	-13.38285	64.149602	-34.804694	209.60984883	-36.48888222	55.8718	54680.8514814815	2008-08-02 20:26:08	54682.0543865741	2008-08-04 01:18:19	803073010	44.2607	30	44.2607	44.2607	0	44.2607	1	1	0	1	1	0	0	36.9355	36.9355	103.904	2	PROCESSED	57543.1885416667	2016-06-04 04:31:30	55059	2009-08-16 00:00:00	54693.2133796296	2008-08-15 05:07:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	034424	A496 is a "normal" nearby cluster that has been the testbed for metal enrichment models in clusters and, more recently, of different mechanisms to generate cold fronts. Suzaku's excellent spectral resolution, low background and high effective area, combined with the moderate temperatures of this cluster allows us to probe, with two short exposures, into the large scale metal enrichment processes through determination of elemental abundance ratios out to half the virial radius for the first time.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	RENATO DUPKE	KYOKO MATSUSHITA	USJ	3	AO3	LARGE SCALE METAL ENRICHMENT MECHANISMS IN ABELL 496	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803073010/	Quick Look
389	A2219	250.0709	46.72	249.708198	46.815683	232.227971	67.561681	72.64070926	41.481603	57.4824	54924.5730787037	2009-04-03 13:45:14	54927.1154282407	2009-04-06 02:46:13	804011010	106.6481	100	106.6481	106.6481	0	106.659	2	2	0	2	1	0	0	114.7986	114.7986	219.6398	2	PROCESSED	57546.0936921296	2016-06-07 02:14:55	55324	2010-05-08 00:00:00	54949.5242939815	2009-04-28 12:34:59	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040011	We propose Suzaku observations of two massive clusters with different radio morphologies, A2219 and A2390, to search for extremely hot (~25 keV) thermal gas. Because of the presence of hot regions indicated in X-ray temperature maps as well as extended radio halo emission, they are the best candidates hosting strongly heated gas due to the past mergers. With the Suzaku broad-band spectroscopy, we can examine properties of very hot gas with high accuracy, and also put constraints on non-thermal emission. This study can only be achieved by the Suzaku's excellent sensitivity to spectral observations over the wide band, and will bring us new insights into physics of gas heating in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NAOMI OTA		JAP	4	AO4	SEARCH FOR EXTREMELY HOT GAS IN TWO MASSIVE GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804011010/	Quick Look
390	ABELL 665	128.154	65.9045	127.018266	66.074275	110.985423	45.219486	149.6634974	34.85484411	289.999	56026.3998958333	2012-04-09 09:35:51	56027.1251967593	2012-04-10 03:00:17	807072010	50.431	50	50.431	50.431	0	50.431	2	2	0	2	1	0	0	41.0111	41.0111	62.6599	1	PROCESSED	57605.1298958333	2016-08-05 03:07:03	56018	2012-04-01 00:00:00	56044.1528240741	2012-04-27 03:40:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072010/	Quick Look
391	ABELL 665	127.5519	65.9953	126.410061	66.162736	110.613991	45.219649	149.61230509	34.59661242	290.0005	56027.1259953704	2012-04-10 03:01:26	56027.8057638889	2012-04-10 19:20:18	807072020	51.446	50	51.446	51.446	0	51.446	2	2	0	2	1	0	0	43.2769	43.2769	58.728	1	PROCESSED	57605.1345717593	2016-08-05 03:13:47	56018	2012-04-01 00:00:00	56044.1899537037	2012-04-27 04:33:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072020/	Quick Look
392	RCS110619-0423.6	166.5769	-4.3915	165.941193	-4.121064	169.375504	-9.341083	260.07293798	49.52807614	109.9541	56253.8521296296	2012-11-22 20:27:04	56256.0092476852	2012-11-25 00:13:19	807075010	77.0765	75	77.0925	77.0765	0	77.1005	2	2	0	2	1	0	0	69.3805	69.3805	186.3458	4	PROCESSED	57608.1296875	2016-08-08 03:06:45	56641	2013-12-15 00:00:00	56275.577025463	2012-12-14 13:50:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071525	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	7	AO7	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807075010/	Quick Look
393	A2029_1	227.7409	5.7498	227.121161	5.938119	223.529064	22.632778	6.48668362	50.54283023	112.9511	55224.0253819444	2010-01-28 00:36:33	55224.3328703704	2010-01-28 07:59:20	804024010	7.6925	10	7.6925	7.7079	0	7.7005	2	2	0	2	1	0	0	4.6083	4.6083	26.5639	1	PROCESSED	57550.3752314815	2016-06-11 09:00:20	55612	2011-02-20 00:00:00	55245.2966203704	2010-02-18 07:07:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040030	Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUZURU TAWARA		JAP	4	AO4	TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024010/	Quick Look
394	HYDRA A SW	139.253	-12.251	138.651756	-12.041032	145.924531	-26.640711	242.88145003	24.78864489	106.4205	56241.8334490741	2012-11-10 20:00:10	56242.8342708333	2012-11-11 20:01:21	807090010	39.8399	40	39.8479	39.8559	0	39.8399	1	1	0	1	1	0	0	33.7085	33.7085	86.4639	0	PROCESSED	57607.9882407407	2016-08-07 23:43:04	56631	2013-12-05 00:00:00	56265.6332986111	2012-12-04 15:11:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072020	Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DOMINIQUE ECKERT		EUR	7	AO7	MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807090010/	Quick Look
395	NGC741 E	29.459	5.6113	28.805334	5.368113	29.381945	-6.027315	151.51137993	-53.53548595	71.776	55054.8091087963	2009-08-11 19:25:07	55055.0619675926	2009-08-12 01:29:14	804053010	11.3778	10	11.3778	11.3858	0	11.3938	2	2	0	2	1	0	0	8.0052	8.0052	21.838	0	PROCESSED	57548.1250231482	2016-06-09 03:00:02	55430	2010-08-22 00:00:00	55064.1656134259	2009-08-21 03:58:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804053010/	Quick Look
396	NGC2841	140.401	51.0226	139.538295	51.235726	125.597618	33.622725	166.8971148	44.0746119	94.9994	55518.5609259259	2010-11-18 13:27:44	55519.8036342593	2010-11-19 19:17:14	805028010	85.5269	80	85.5429	85.5269	0	85.5429	2	2	0	2	1	0	0	59.375	59.375	107.3518	1	PROCESSED	57554.1596180556	2016-06-15 03:49:51	55898	2011-12-03 00:00:00	55530.1645949074	2010-11-30 03:57:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050028	We propose a 80 ksec observation of an edge-on nearby spiral galaxy, NGC 2841 and the halo region. The expected temperature of the halo is ∼0.5 keV, and the characteristics enable Suzku to study the gas properties out to intergalactic space in a reliable way. We aim to obtain the temperature in the halo region within ∼5%, and hopefully an evidence for the gas dynamics not only between the disk and the halo region, but also between the halo and the intergalactic medium.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	IKUYUKI MITSUISHI		JAP	5	AO5	STUDY OF X-RAY HALO OF AN EDGE-ON GALAXY NGC 2841	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805028010/	Quick Look
397	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
398	NGC741MOSAICS_P1	29.0595	4.7357	28.408059	4.491575	28.699079	-6.708921	151.53660126	-54.49712787	71.6617	55052.4780671296	2009-08-09 11:28:25	55052.6946643518	2009-08-09 16:40:19	804054010	9.3222	10	9.3302	9.3222	0	9.3302	1	1	0	1	1	0	0	8.003	8.003	18.6719	1	PROCESSED	57548.0801967593	2016-06-09 01:55:29	55451	2010-09-12 00:00:00	55084.9869212963	2009-09-10 23:41:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054010/	Quick Look
399	NGC 6338	258.8129	57.4208	258.599761	57.475287	235.015954	79.490546	85.8195722	35.41601483	46.4308	56771.4831712963	2014-04-24 11:35:46	56771.8058333333	2014-04-24 19:20:24	809099010	15.4756	10	15.4756	15.4756	0	15.4756	3	2	0	2	1	0	0	14.5259	14.5259	26.0449	0	PROCESSED	57614.9892708333	2016-08-14 23:44:33	57155	2015-05-13 00:00:00	56789.6384722222	2014-05-12 15:19:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809099010/	Quick Look
400	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
401	ABELL 426 E3	51.0503	41.5202	50.219736	41.343661	59.4655	22.121233	151.27232524	-12.79481746	89.0003	55041.9666666667	2009-07-29 23:12:00	55042.2904398148	2009-07-30 06:58:14	804058010	11.2798	10	11.2798	11.5518	0	11.5518	3	2	0	2	1	0	0	10.7201	10.7201	27.9661	0	PROCESSED	57547.981412037	2016-06-08 23:33:14	55427	2010-08-19 00:00:00	55060.7814236111	2009-08-17 18:45:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804058010/	Quick Look
402	AWM4	241.2331	23.9108	240.70062	24.045882	232.521444	43.67819	39.92527821	46.49145981	302.6954	56859.2473263889	2014-07-21 05:56:09	56859.4627314815	2014-07-21 11:06:20	809102010	9.31	11	9.31	9.438	0	9.438	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.4155092593	2016-08-15 09:58:20	57239	2015-08-05 00:00:00	56873.5548958333	2014-08-04 13:19:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809102010/	Quick Look
403	A133_W	15.4513	-21.8877	14.840059	-22.156478	5.012562	-26.12974	147.70952455	-84.25382555	44.9935	55354.0979513889	2010-06-07 02:21:03	55355.296099537	2010-06-08 07:06:23	805019010	50.0449	50	50.0449	50.0449	0	50.0449	2	2	0	2	1	0	0	41.2813	41.2813	103.4758	0	PROCESSED	57551.9211689815	2016-06-12 22:06:29	55765	2011-07-23 00:00:00	55393.3189467593	2010-07-16 07:39:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050019	We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KOSUKE SATO		JAP	5	AO5	METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805019010/	Quick Look
404	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
405	ABELL 3733	315.4567	-28.0341	314.710836	-28.231283	309.79285	-10.656463	17.77333082	-39.60697798	260.2652	56981.8706481482	2014-11-20 20:53:44	56982.1530439815	2014-11-21 03:40:23	809108010	14.5884	15	14.5964	14.6044	0	14.5884	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7988541667	2016-08-16 19:10:21	57362	2015-12-06 00:00:00	56996.4060300926	2014-12-05 09:44:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809108010/	Quick Look
406	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
407	RCS1620+3046	245.0418	30.7908	244.551505	30.909318	234.634805	51.209306	50.54291734	44.60353773	131.519	55203.6116666667	2010-01-07 14:40:48	55204.6008564815	2010-01-08 14:25:14	804081010	43.4882	38	43.4882	43.4882	0	43.4882	2	2	0	2	1	0	0	16.6324	16.6324	85.4538	0	PROCESSED	57550.1212615741	2016-06-11 02:54:37	55584	2011-01-23 00:00:00	55218.2018402778	2010-01-22 04:50:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041525	Understanding relationships between baryons in galaxy clusters and the underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a cluster sample chosen independently of X-ray properties. We propose to study 14 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Chandra observations of 8 high-dispersion, low-z targets. Suzaku s superior throughput is required to probe the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 6 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AMALIA HICKS		USA	4	AO4	DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804081010/	Quick Look
408	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
409	A3404	101.1266	-54.2028	100.864696	-54.149703	118.987538	-76.520827	263.61200949	-22.68018452	319.1401	54971.6181944444	2009-05-20 14:50:12	54974.625162037	2009-05-23 15:00:14	804089010	122.0929	121	122.1009	122.1009	0	122.0929	2	2	0	2	1	0	0	106.1261	106.1261	259.7879	4	PROCESSED	57546.7060532407	2016-06-07 16:56:43	55358	2010-06-11 00:00:00	54992.6862615741	2009-06-10 16:28:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042025	Robust and precise mass measurements for a large number of galaxy clusters represent the single most important step to prepare for dark energy cluster surveys to be performed, e.g., with eROSITA. Robustness and precision can best be achieved by a comparative and combined analysis of independent techniques. Here, we propose to use measurements from Suzaku, APEX-SZ, and wide-field optical telescopes to determine cluster masses up to the virial radius. X-ray, SZ, and gravitational lensing reduction and analyses will all be performed by experts at a single location. We demonstrate that we have selected the optimal targets for this study. Further, we show promising results from our Suzaku analysis of cluster outskirts, from our lensing pipeline, as well as from our combined SZ/X-ray method.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	THOMAS REIPRICH		EUR	4	AO4	COMBINED SUZAKU/APEX-SZ/LENSING MASS MEASUREMENTS OF THE GALAXY CLUSTERS A3404 AND A2537	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804089010/	Quick Look
410	NGC 253	11.8603	-25.2295	11.246067	-25.502313	0.06066	-27.714636	97.43086004	-87.9001973	242.9983	55544.0947685185	2010-12-14 02:16:28	55546.9460763889	2010-12-16 22:42:21	805018010	101.0026	100	101.0026	101.0026	0	101.0026	2	2	0	2	1	0	0	82.6689	82.6689	246.3359	1	PROCESSED	57554.5316203704	2016-06-15 12:45:32	55975	2012-02-18 00:00:00	55607.3286111111	2011-02-15 07:53:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050015	Suzaku observations of a hot halo of nearby, edge-on starburst galaxy, NGC 253 are proposed. The low background and high energy resolution of Suzaku XIS is the best tool to study the low surface brightness emission like halo emission around galaxies. In addition, we will eliminate the contamination from the the point source by XMM-Newton and the Galactic hot emission by a previous offset observation. The temperature and pressure structure and the chemical composition in the bright halo will reveal the physical condition and dynamics of the galaxy outflow to the intergalactic space.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORIKO YAMASAKI		JAP	5	AO5	SUZAKU OBSERVATION OF A BRIGHTEST STARBURST GALAXY NGC 253	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805018010/	Quick Look
411	A3667_SE	303.4605	-57.0338	302.458448	-57.1853	291.78529	-36.098363	340.61636005	-33.57067764	74.2668	55298.167349537	2010-04-12 04:00:59	55299.2716435185	2010-04-13 06:31:10	805036010	66.2872	50	66.2952	66.2872	0	66.2872	2	2	0	2	1	0	0	51.249	51.249	95.3978	1	PROCESSED	57551.2001967593	2016-06-12 04:48:17	55675	2011-04-24 00:00:00	55309.2055324074	2010-04-23 04:55:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050039	We propose an additional offset pointing of Abell 3667, one of the nearest, typical merging cluster. Using the 3 observations pointed along the merger axis on AO-1, we detected a possible super hot component around the cluster center (Nakazawa et al. 2009). To identify the existence and location of this component, we propose to observe the South-East Relic region, about 17 f south to the original southern-most pointing. This observation aims at verifying and locating the super hot component in this cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA		JAP	5	AO5	TRACING THE POSSIBLE SUPER-HOT COMPONENT IN THE MERGING CLUSTER ABELL 3667	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805036010/	Quick Look
412	ABELL1835 OFFSET1	210.441	2.9038	209.807683	3.144591	207.277058	14.34402	340.72312739	60.50812136	306.2398	55382.6847453704	2010-07-05 16:26:02	55384.1217361111	2010-07-07 02:55:18	805037010	49.4391	50	49.4471	49.4391	0	49.4471	2	2	0	2	1	0	0	43.0599	43.0599	124.1398	1	PROCESSED	57552.5235532407	2016-06-13 12:33:55	55807	2011-09-03 00:00:00	55441.2415856482	2010-09-02 05:47:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050040	We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	NOBUHIRO OKABE		JAP	5	AO5	UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805037010/	Quick Look
413	ABELL 85 S1	10.6021	-9.9841	9.970303	-10.258056	5.733976	-13.366048	115.42621428	-72.72412936	230	56292.2572800926	2012-12-31 06:10:29	56295.6314583333	2013-01-03 15:09:18	807135010	139.9982	50	139.9982	139.9982	0	139.9982	2	2	0	2	1	0	0	11.82	11.82	25.4779	0	PROCESSED	57608.4068402778	2016-08-08 09:45:51	56703	2014-02-15 00:00:00	56337.496875	2013-02-14 11:55:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071791	We propose exposures with CHandra and Suzaku in Abell 85 to trace the impact of a galaxy group merging with a galaxy cluster at multiple scales. Existing observations of Abell 85 reveal an infalling galaxy group ~300 kpc to the south of the main cluster moving supersonically through the ICM. Stripped gas is observed trailing behind this group to distances of 2 Mpc. We will investigate interactions between this group and the main cluster by observing the shocks associated with the group's motion and the properties of stripped gas. We will be able to measure the properties of the stripped gas from the group's current location out to the virial radius by combining the data from both telescopes. These observations will provide key insights into how the largest structures form.	EXTRAGALACTIC DIFFUSE SOURCES	8	S	STEVEN ALLEN		USA	7	AO7	TRACING A MERGER FROM START TO FINISH IN ABELL 85	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807135010/	Quick Look
414	NGC3402 BACKGROUND	161.6656	-13.5535	161.046219	-13.289693	168.522728	-19.671776	262.34680831	39.29035073	110.091	55549.4379282407	2010-12-19 10:30:37	55549.7563425926	2010-12-19 18:09:08	805071010	12.5184	10	12.5344	12.5184	0	12.5344	1	1	0	1	1	0	0	11.8582	11.8582	27.4799	0	PROCESSED	57554.4605439815	2016-06-15 11:03:11	55960	2012-02-03 00:00:00	55593.0714699074	2011-02-01 01:42:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051512	Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	XINYU DAI		USA	5	AO5	BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805071010/	Quick Look
415	ESO3060170	85.0359	-40.9515	84.636079	-40.976582	81.358883	-64.245092	246.54247084	-30.30516606	320.0075	55327.721400463	2010-05-11 17:18:49	55328.2676388889	2010-05-12 06:25:24	805075010	31.3959	30	31.4039	31.3959	0	31.4119	2	2	0	2	1	0	0	28.684	28.684	47.1899	2	PROCESSED	57551.4609953704	2016-06-12 11:03:50	55707	2011-05-26 00:00:00	55341.5181365741	2010-05-25 12:26:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051513	We propose 30 and 80 ksec observations of the X-ray brightest fossil group, ESO 3060170. The target pointings will reach to 75% of the virial radius from the center of the galaxy, in order to determine the temperature and metal abundances of group gas at large radii. This will allow us to determine the radial profiles of the gaseous iron mass to stellar light ratio, the relative distributions of ejecta from SN Ia and SN II, the entropy, the total mass to light ratio, and the dark matter concentration for this fossil group. The energy resolution and low background of the XIS instrument are crucial for this study, which will help constrain the evolutional history of this fossil group and tell us how fossil groups relate to normal groups and clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YUANYUAN SU		USA	5	AO5	HOW DO FOSSIL GROUPS OF GALAXIES DIFFER FROM NORMAL GROUPS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805075010/	Quick Look
416	CYGNUS A SUB	299.7227	40.8585	299.290982	40.72139	317.590165	59.487138	76.23979532	5.91406977	241.0006	56615.3145717593	2013-11-19 07:32:59	56616.3224189815	2013-11-20 07:44:17	808016010	42.5204	40	42.5284	42.5284	0	42.5204	2	2	0	2	1	0	0	38.9173	38.9173	87.0719	1	PROCESSED	57613.3640625	2016-08-13 08:44:15	56995	2014-12-04 00:00:00	56629.6679050926	2013-12-03 16:01:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080018	We have observed a merging cluster Cygnus A in the Suzaku GO-3 with 45ks. This observation confirmed a hot region between the main and sub components. Furthermore, we found a gas velocity shift between the main and sub by about 2500 km/s. We believe that these are colliding with each other. The current result are limited by statistics and systematic uncertainty. To improve the accurary of the measurement and complete our study, we propose two additional observations located the main and sub components at the center of the FOV. These will provide the best chance to look into a merging cluster "in motion".	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKAYUKI TAMURA		JAP	8	AO8	CYGNUS A CLUSTER: THE BEST MERGING SYSTEM FOR THE SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808016010/	Quick Look
417	PKS 0745-191	116.4685	-19.4632	115.915912	-19.340315	123.218132	-39.89918	236.39245911	2.60836561	294.0003	55317.3681365741	2010-05-01 08:50:07	55318.1516087963	2010-05-02 03:38:19	805086010	31.7299	35	31.7299	31.7299	0	31.7299	2	2	0	2	1	0	0	27.646	27.646	67.682	0	PROCESSED	57551.3418981482	2016-06-12 08:12:20	55696	2011-05-15 00:00:00	55330.121087963	2010-05-14 02:54:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051526	Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MATTHEW GEORGE		USA	5	AO5	BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805086010/	Quick Look
418	RCS2318-0024	349.6301	-0.4169	348.988896	-0.690483	350.299766	3.723056	79.21894267	-55.19865221	248.0438	55526.0185648148	2010-11-26 00:26:44	55527.293912037	2010-11-27 07:03:14	805089010	50.305	73	50.329	50.305	0	50.337	2	2	0	2	1	0	0	45.6346	45.6346	110.1738	0	PROCESSED	57554.2552893518	2016-06-15 06:07:37	55903	2011-12-08 00:00:00	55537.0791898148	2010-12-07 01:54:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051527	Understanding relationships between baryons in galaxy clusters and underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a sample chosen independently of X-ray properties. We propose to study 13 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Suzaku/Chandra observations of 11 high-dispersion, low-z targets. Suzaku's superior throughput is required to complete the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 2 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	5	AO5	DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805089010/	Quick Look
419	NGC1550_BGD	66.1553	2.4144	65.504252	2.300401	64.719628	-18.959095	191.78857248	-30.8138174	260.0006	56697.3550694444	2014-02-09 08:31:18	56698.0418634259	2014-02-10 01:00:17	808061010	31.1456	30	31.1536	31.1536	0	31.1456	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57613.8043171296	2016-08-13 19:18:13	57102	2015-03-21 00:00:00	56736.7213425926	2014-03-20 17:18:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080110	We propose to study the entropy profile and the metal enrichment process of the fossil group, NGC 1550 with total 170 ksec observations. NGC 1550 is a bright nearby group (z=0.0124), and classified as a fossil group which has no bright galaxies except for a central elliptical galaxy. Fossil groups, therefore, are a very useful system for investigating how the ICM metals have been enriched from galaxies. On the other hand, it is known that the entropy of groups has a several times larger than that of clusters within ~0.2 r180, and has similar value to clusters at 0.5 r180. However, in r > 0.5 r180 region, the entropy profile of groups has not been observed yet, while those of clusters have shown a flatter slope than the expected value from simulations in the Suzaku results.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TORU SASAKI		JAP	8	AO8	STUDY OF THE ENTROPY PROFILE AND THE METAL ENRICHMENT PROCESS IN THE FOSSIL GROUP, NGC~1550	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808061010/	Quick Look
420	A133_FIELD_3	15.3292	-22.0955	14.718033	-22.364433	4.799478	-26.269218	147.50079252	-84.48957915	231.9998	56631.4102314815	2013-12-05 09:50:44	56632.6168981482	2013-12-06 14:48:20	808083010	51.8568	50	51.8568	51.8568	0	51.8568	2	2	0	2	1	0	0	47.9569	47.9569	104.2418	0	PROCESSED	57613.5483217593	2016-08-13 13:09:35	57009	2014-12-18 00:00:00	56643.7003587963	2013-12-17 16:48:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081525	We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	8	AO8	A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808083010/	Quick Look
421	A133_FIELD_4	16.0019	-22.0663	15.391978	-22.334366	5.44253	-26.509377	153.04375578	-84.18809016	231.9997	56632.6176967593	2013-12-06 14:49:29	56633.8716666667	2013-12-07 20:55:12	808084010	52.5282	50	52.5282	52.5282	0	52.5282	2	2	0	2	1	0	0	49.912	49.912	108.3281	0	PROCESSED	57613.5467013889	2016-08-13 13:07:15	57061	2015-02-08 00:00:00	56695.6415046296	2014-02-07 15:23:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081525	We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	8	AO8	A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808084010/	Quick Look
422	ABELL 1068	160.2123	39.7867	159.491465	40.048011	145.700686	28.920989	179.4205229	60.1860041	130.0008	55863.1263310185	2011-10-29 03:01:55	55864.5459837963	2011-10-30 13:06:13	806028030	53.3186	50	53.3186	53.335	0	53.3266	2	2	0	2	1	0	0	49.0713	49.0713	122.6438	0	PROCESSED	57603.6522800926	2016-08-03 15:39:17	55652	2011-04-01 00:00:00	55874.122662037	2011-11-09 02:56:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806028030/	Quick Look
423	A426VIR N	48.9538	42.7811	48.120761	42.596803	58.224249	23.764199	149.23070312	-12.5987294	270.5957	56710.5023726852	2014-02-22 12:03:25	56711.155775463	2014-02-23 03:44:19	808087010	23.3776	25	23.3856	23.3856	0	23.3776	2	2	0	2	1	0	0	20.5612	20.5612	56.4419	0	PROCESSED	57613.8896296296	2016-08-13 21:21:04	57089	2015-03-08 00:00:00	56723.6141898148	2014-03-07 14:44:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081526	Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ONDREJ URBAN		USA	8	AO8	SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808087010/	Quick Look
424	A426VIR W	48.7321	42.6495	47.900602	42.4644	58.012629	23.684677	149.16205221	-12.79713949	270.0001	56711.1564351852	2014-02-23 03:45:16	56711.6279976852	2014-02-23 15:04:19	808088010	24.7428	25	24.7587	24.7428	0	24.7667	1	1	0	1	1	0	0	22.0168	22.0168	40.7359	0	PROCESSED	57613.8909259259	2016-08-13 21:22:56	57141	2015-04-29 00:00:00	56764.7613657407	2014-04-17 18:16:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081526	Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ONDREJ URBAN		USA	8	AO8	SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808088010/	Quick Look
425	ABELL 1689 (OFFSET)	198.1886	-1.1923	197.54634	-0.927328	197.227317	6.029723	314.05162405	61.21838483	111.865	56657.0769444444	2013-12-31 01:50:48	56660.6460069445	2014-01-03 15:30:15	808089030	53.2272	130	53.2272	53.2272	0	53.2272	1	1	0	1	0	0	0	0	0	3.3279	0	PROCESSED	57613.7319791667	2016-08-13 17:34:03	56383	2013-04-01 00:00:00	56713.6636342593	2014-02-25 15:55:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081528	Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	8	AO8	SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089030/	Quick Look
426	ABELL 1689 (OFFSET)	198.1809	-1.2604	197.538539	-0.995417	197.246177	5.963813	314.01167358	61.15261163	111.9001	56670.9898148148	2014-01-13 23:45:20	56672.9376388889	2014-01-15 22:30:12	808089040	37.4667	90	37.4667	37.4667	0	37.4667	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57613.7681134259	2016-08-13 18:26:05	56383	2013-04-01 00:00:00	56687.7783564815	2014-01-30 18:40:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081528	Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	8	AO8	SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089040/	Quick Look
427	COMA W SHOCK2	194.0639	28.3374	193.459144	28.607762	180.49458	31.367738	81.80911298	88.38803012	275.4001	56475.6616782407	2013-07-02 15:52:49	56476.1674884259	2013-07-03 04:01:11	808091010	15.6934	15	15.7094	15.6934	0	15.7094	2	2	0	2	1	0	0	16.6254	16.6254	43.694	0	PROCESSED	57611.6755902778	2016-08-11 16:12:51	56858	2014-07-20 00:00:00	56492.6168865741	2013-07-19 14:48:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081529	Our analysis of Suzaku data of the Coma Cluster revealed an intriguing correlation between the outer edge of its radio halo and the thermodynamic properties of the gas. This correlation seems to be the most pronounced in the western direction where the temperature drops from about 10keV in the annulus spanning 35'-41' to only 1.7keV in the annulus spanning 50'-60'. The Planck Collaboration found a marked local steepening of the radial gradient of the SZ signal at this location and interpret this feature as a shock with a Mach number of about 2. Unfortunately, we currently lack X-ray coverage towards the W in this critical range of 41'-50'. We therefore propose two additional pointings with a total exposure time of 30ks, that will allow us to resolve the temperature gradient in this region.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AURORA SIMIONESCU		USA	8	AO8	THE MISSING PUZZLE PIECE IN THE COMA SHOCK FRONT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808091010/	Quick Look
428	A2877-SOUTH	17.378	-46.6527	16.824483	-46.918871	351.212416	-48.486015	293.76700694	-70.15260223	237.9995	56647.8346643518	2013-12-21 20:01:55	56649.916875	2013-12-23 22:00:18	808103010	83.5172	80	83.5172	83.5252	0	83.5332	2	2	0	2	1	0	0	81.2993	81.2993	179.8979	4	PROCESSED	57613.6802199074	2016-08-13 16:19:31	57033	2015-01-11 00:00:00	56665.8173263889	2014-01-08 19:36:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082014	We propose to observe the galaxy group A2877 for a combine observation time of 150 ks, with two different pointings. The aim of the project is to obtain temperature and surface brightness profiles out to large radii to constrain entropies. We aim to see if the entropy profile flattens at large radii, which could indicate gas clumping and/or other processes. This would possibly be the first unrelaxed galaxy group whose entropy profile would have been studied in the outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	BHARADWAJ VIJAYSARATHY		EUR	8	AO8	INVESTIGATING THE OUTSKIRTS OF THE UNRELAXED GALAXY GROUP A2877	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808103010/	Quick Look
429	COMA NW6	194.1545	29.4183	193.551623	29.688554	179.999631	32.366617	96.76135884	87.44172405	319.9992	55734.4158796296	2011-06-22 09:58:52	55734.7419328704	2011-06-22 17:48:23	806044010	13.52	15	13.52	13.52	0	13.52	1	1	0	1	1	0	0	11.5945	11.5945	28.1679	1	PROCESSED	57602.3747453704	2016-08-02 08:59:38	55652	2011-04-01 00:00:00	55768.2886574074	2011-07-26 06:55:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806044010/	Quick Look
430	A3528-S OFFSET 1	193.8801	-29.4768	193.202783	-29.206094	204.617979	-21.613954	303.99602967	33.38651365	289.4829	56500.4359953704	2013-07-27 10:27:50	56501.528587963	2013-07-28 12:41:10	808104010	40.3411	50	40.3491	40.3491	0	40.3411	2	2	0	2	1	0	0	40.8623	40.8623	94.384	2	PROCESSED	57612.0687037037	2016-08-12 01:38:56	56955	2014-10-25 00:00:00	56587.7834490741	2013-10-22 18:48:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082018	We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	LORENZO LOVISARI		EUR	8	AO8	TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808104010/	Quick Look
431	BEYOND VIRGO 3	187.7131	16.6287	187.083239	16.904753	180.24751	18.281087	277.46526397	78.4695575	119.4716	55906.3990277778	2011-12-11 09:34:36	55907.0070717593	2011-12-12 00:10:11	806062010	24.1336	30	24.1336	24.1336	0	24.1336	1	1	0	1	1	0	0	22.399	22.399	52.5119	1	PROCESSED	57604.102974537	2016-08-04 02:28:17	56289	2012-12-28 00:00:00	55920.9612731482	2011-12-25 23:04:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061523	To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORBERT WERNER		USA	6	AO6	LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806062010/	Quick Look
432	BEYOND VIRGO 5	187.715	17.1647	187.085509	17.440751	180.014258	18.769278	276.35604201	78.95966269	118.1329	55918.8504976852	2011-12-23 20:24:43	55919.8960300926	2011-12-24 21:30:17	806064010	41.7692	40	41.7772	41.7692	0	41.7772	2	2	0	2	1	0	0	34.3124	34.3124	90.2919	1	PROCESSED	57604.2418402778	2016-08-04 05:48:15	56340	2013-02-17 00:00:00	55972.6886458333	2012-02-15 16:31:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061523	To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORBERT WERNER		USA	6	AO6	LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806064010/	Quick Look
433	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
434	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
435	THE MOON	137.2637	11.2624	136.584895	11.465744	136.302979	-4.908841	218.49853071	35.60818154	285.3989	56784.0743402778	2014-05-07 01:47:03	56784.198125	2014-05-07 04:45:18	809001050	5.7625	45	5.7705	5.7625	0	5.7785	1	1	0	1	1	0	0	4.371	4.371	10.6879	1	PROCESSED	57615.062337963	2016-08-15 01:29:46	57218	2015-07-15 00:00:00	56852.5744328704	2014-07-14 13:47:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001050/	Quick Look
436	BEYOND VIRGO 7	187.7158	17.6999	187.086679	17.97595	179.778986	19.25601	275.1422843	79.44418151	118.4175	55920.9292708333	2011-12-25 22:18:09	55922.3029166667	2011-12-27 07:16:12	806066010	51.5018	50	51.5258	51.5178	0	51.5018	2	2	0	2	1	0	0	45.0209	45.0209	118.6698	0	PROCESSED	57604.2629861111	2016-08-04 06:18:42	56340	2013-02-17 00:00:00	55972.6991203704	2012-02-15 16:46:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061523	To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORBERT WERNER		USA	6	AO6	LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806066010/	Quick Look
437	THE MOON	24.3624	9.7895	23.702448	9.535235	26.139692	-0.327211	141.30582848	-51.43331262	73.7995	56857.0209259259	2014-07-19 00:30:08	56857.1515856482	2014-07-19 03:38:17	809001140	4.2907	45	4.2907	4.2907	0	4.2907	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.4055439815	2016-08-15 09:43:59	57267	2015-09-02 00:00:00	56902.7022685185	2014-09-02 16:51:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001140/	Quick Look
438	THE MOON	139.925	10.5889	139.25032	10.800859	139.007269	-4.769046	220.6720528	37.66748388	105.6998	56975.3249305556	2014-11-14 07:47:54	56975.4487615741	2014-11-14 10:46:13	809001210	3.5246	45	3.5246	3.5246	0	3.5246	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.771412037	2016-08-16 18:30:50	57358	2015-12-02 00:00:00	56992.4131018518	2014-12-01 09:54:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001210/	Quick Look
439	THE MOON	144.4436	10.011	143.773859	10.236526	143.42105	-3.916716	223.94276709	41.37428155	105.6999	56975.7165856482	2014-11-14 17:11:53	56975.8473611111	2014-11-14 20:20:12	809001240	6.2192	45	6.2192	6.2272	0	6.2512	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7771412037	2016-08-16 18:39:05	57358	2015-12-02 00:00:00	56992.4178703704	2014-12-01 10:01:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001240/	Quick Look
440	RCS211853-6334.5	319.7157	-63.5732	318.707212	-63.784045	298.683481	-45.002818	330.73727963	-40.23433007	78.3879	55689.9756018518	2011-05-08 23:24:52	55691.0148148148	2011-05-10 00:21:20	806079010	69.5446	70	69.5526	69.5446	0	69.5526	2	2	0	2	1	0	0	57.3836	57.3836	89.7739	0	PROCESSED	57601.9954398148	2016-08-01 23:53:26	56068	2012-05-21 00:00:00	55701.1727314815	2011-05-20 04:08:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061533	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AMALIA HICKS		USA	6	AO6	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806079010/	Quick Look
441	THE MOON	330.3821	-8.1914	329.721062	-8.43265	329.560437	3.662364	50.06648816	-45.61675095	252.3	56989.8522685185	2014-11-28 20:27:16	56989.9654976852	2014-11-28 23:10:19	809001280	4.7272	45	4.7272	4.7272	0	4.7272	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.401712963	2016-08-17 09:38:28	57415	2016-01-28 00:00:00	57002.4419444445	2014-12-11 10:36:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001280/	Quick Look
442	THE MOON	332.0733	-7.3936	331.41518	-7.63885	331.413251	3.82441	52.31004503	-46.62982693	251.0013	56989.9669444444	2014-11-28 23:12:24	56990.1008449074	2014-11-29 02:25:13	809001290	4.227	45	4.227	4.2506	0	4.235	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.4062962963	2016-08-17 09:45:04	57415	2016-01-28 00:00:00	57002.4422453704	2014-12-11 10:36:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001290/	Quick Look
443	CEN_A_LOBE_N2	201.2142	-42.0778	200.484454	-41.817568	216.546241	-30.52743	309.53774085	20.36490033	292.2294	56861.2578587963	2014-07-23 06:11:19	56862.6946990741	2014-07-24 16:40:22	809003010	52.1427	50	52.1507	52.1427	0	52.1587	2	2	0	2	1	0	0	19.3107	19.3107	40.0719	0	PROCESSED	57615.4510648148	2016-08-15 10:49:32	57242	2015-08-08 00:00:00	56875.1594560185	2014-08-06 03:49:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090021	In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROMI SETA		JAP	9	AO9	MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809003010/	Quick Look
444	A3526	191.2847	-39.8559	190.600127	-39.582502	207.545871	-31.88181	301.61867579	22.99978629	109.9984	55943.9465393518	2012-01-17 22:43:01	55944.2683333333	2012-01-18 06:26:24	806089010	15.9106	15	15.9186	15.9106	0	15.9186	1	1	0	1	1	0	0	12.985	12.985	27.7919	0	PROCESSED	57604.3987268518	2016-08-04 09:34:10	56332	2013-02-09 00:00:00	55964.1580439815	2012-02-07 03:47:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806089010/	Quick Look
445	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
446	N23_DEML71	76.4544	-67.9572	76.483575	-68.02238	338.831134	-84.597327	278.75688601	-34.83345845	297.0986	56021.0207986111	2012-04-04 00:29:57	56023.6043402778	2012-04-06 14:30:15	807008010	101.9614	100	101.9614	101.9614	0	101.9614	2	2	0	2	1	0	0	99.0031	99.0031	223.204	1	PROCESSED	57605.1620023148	2016-08-05 03:53:17	56401	2013-04-19 00:00:00	56034.2910069444	2012-04-17 06:59:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070036	Recently, we discovered recombining plasma (RP) from several mixed-morphology (MM) SNRs in our galaxy, which provides us a new insight into the evolution of SNRs. On the other hand, the RP has not been detected yet from extragalactic SNRs, while many MM-SNRs exist also in extra galaxies. We investigated all the X-ray spectra obtained from previous observations with Suzaku, XMM-Newton and Chandra and found a clear signal of the RP from three LMC SNRs (N49, N23 and DEM L71). Long-time observations with Suzaku XIS will provide us a first evidence of RP from extra galaxies. We propose 2-pointing observations of three SNRs for 290ks.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROYUKI UCHIDA		JAP	7	AO7	FIRST INVESTIGATION OF RECOMBINING PLASMA FROM EXTRAGALACTIC SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807008010/	Quick Look
447	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
448	CEN_A_LOBE_N4	200.0149	-42.0781	199.290063	-41.815855	215.61315	-30.91319	308.59567712	20.47867303	294.4884	56864.2718634259	2014-07-26 06:31:29	56865.6863194444	2014-07-27 16:28:18	809005010	49.4215	50	49.4215	50.3093	0	50.3093	2	2	0	2	1	0	0	14.7711	14.7711	31.0519	0	PROCESSED	57615.4593055556	2016-08-15 11:01:24	57242	2015-08-08 00:00:00	56875.2119675926	2014-08-06 05:05:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090021	In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROMI SETA		JAP	9	AO9	MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809005010/	Quick Look
449	A3112W	49.1257	-44.1666	48.689569	-44.349648	25.156648	-58.765875	252.9579492	-56.34974536	40.0005	56834.0356481482	2014-06-26 00:51:20	56835.5486458333	2014-06-27 13:10:03	809025010	48.949	45	48.949	48.949	0	48.949	2	2	0	2	1	0	0	11.966	11.966	40.6069	2	PROCESSED	57615.3397685185	2016-08-15 08:09:16	57249	2015-08-15 00:00:00	56881.2363078704	2014-08-12 05:40:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090061	We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KOSUKE SATO		JAP	9	AO9	ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809025010/	Quick Look
450	FJ0846+5326	131.5564	53.4343	130.632054	53.617254	118.481008	34.023671	164.73615985	38.37651034	277.0006	56764.8665393518	2014-04-17 20:47:49	56766.1148032407	2014-04-19 02:45:19	809037010	44.7166	45	44.7166	44.7166	0	44.7166	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57614.9585416667	2016-08-14 23:00:18	57145	2015-05-03 00:00:00	56782.5079976852	2014-05-05 12:11:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090090	Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	IKUYUKI MITSUISHI		JAP	9	AO9	EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809037010/	Quick Look
451	OFF-FIELD1	154.5616	22.312	153.870987	22.562652	148.318203	10.965902	212.25034337	55.01303699	298.5999	56782.6031712963	2014-05-05 14:28:34	56783.5417939815	2014-05-06 13:00:11	809052010	41.103	40	41.103	41.103	0	41.103	2	2	0	2	1	0	0	39.0283	39.0283	81.0719	1	PROCESSED	57615.0526388889	2016-08-15 01:15:48	57162	2015-05-20 00:00:00	56793.5659490741	2014-05-16 13:34:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091501	Late-type galaxies in the Local Universe are missing over 70% of their baryonic mass, a large fraction of which is likely embedded in the extended, low density warm-hot gaseous halo. However, searches of hot diffuse halos around massive spiral galaxies found them to be relatively small and not very massive. The UV observations have shown that the baryonic halo mass depends on the specific star formation rate (sSFR) and not on the total mass of the galaxy. We propose to observe the halo emission of NGC3221 with very high sSFR. Detection and characterization of the hot halo around this galaxy will expand our understanding of the dependence of halo properties on galaxy properties, and advance our understanding of galaxy formation, feedback and metal enrichment proposed by theoretical models.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ANJALI GUPTA		USA	9	AO9	SEARCH FOR THE HOT GASEOUS HALO AROUND THE NEARBY SPIRAL GALAXY NGC3221	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809052010/	Quick Look
452	ABELL 98-SOUTH	11.6766	20.275	11.015845	20.00206	18.757977	14.029978	121.42486866	-42.58290308	251.4904	57011.5401736111	2014-12-20 12:57:51	57012.9168171296	2014-12-21 22:00:13	809080010	48.2579	100	48.2579	49.0544	0	49.1104	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.5485532407	2016-08-17 13:09:55	56748	2014-04-01 00:00:00	57107.4443171296	2015-03-26 10:39:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091525	We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	SCOTT RANDALL		USA	9	AO9	EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809080010/	Quick Look
453	ABELL 3411 OFFSET	130.7649	-17.3143	130.18997	-17.133567	138.838529	-34.101685	241.9812862	15.18552207	105.3327	56967.309849537	2014-11-06 07:26:11	56968.1939467593	2014-11-07 04:39:17	809083010	38.952	39	38.952	39.272	0	39.288	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7398263889	2016-08-16 17:45:21	57358	2015-12-02 00:00:00	56982.4550231482	2014-11-21 10:55:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091528	Galaxy cluster mergers trigger Mpc-scale shocks in the ICM, which can accelerate particles to relativistic energies to form arc-shaped radio relics. Last year, we discovered a spectacular radio relic in the Planck cluster A3411. The relic has a complex, fragmentary morphology, at odds with the arc-shaped shocks predicted by hydrodynamical simulations. In light of this unexpected discovery, we propose for a 169-ks Suzaku observation to characterize the ICM properties at the radio relic in A3411. The combination of high-quality X-ray and radio data will provide a unique opportunity to (1) measure the shock properties and relate them to the radio structures; (2) explore the reason for the fragmentation of the relic; (3) model the merger event; and (4) test different shock acceleration models.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	REINOUT VAN WEEREN		USA	9	AO9	ABELL 3411: PARTICLE RE-ACCELERATION AND A COMPLEX SHOCK GEOMETRY?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809083010/	Quick Look
454	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
455	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
456	SWCL1330+4206	202.7007	42.1031	202.156429	42.360378	179.6615	46.801465	97.22165079	73.00355707	325.866	57166.2929166667	2015-05-24 07:01:48	57167.0793171296	2015-05-25 01:54:13	809088020	34.7796	34	34.7796	34.7876	0	34.7796	1	1	0	1	1	0	0	21.0686	21.0686	53.048	1	PROCESSED	57618.72625	2016-08-18 17:25:48	57548	2016-06-09 00:00:00	57178.157025463	2015-06-05 03:46:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091531	The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	XINYU DAI		USA	9	AO9	X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809088020/	Quick Look
457	CENA LOBE 1	201.4716	-38.9356	200.750271	-38.675827	215.22462	-27.598918	310.226071	23.44775478	285.9999	56117.7018287037	2012-07-09 16:50:38	56119.8959953704	2012-07-11 21:30:14	807040010	84.161	80	84.161	84.161	0	84.161	2	2	0	2	1	0	0	72.2838	72.2838	188.7955	3	PROCESSED	57606.6375347222	2016-08-06 15:18:03	56018	2012-04-01 00:00:00	56159.3425925926	2012-08-20 08:13:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070106	Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LUKASZ STAWARZ		JAP	7	AO7	STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807040010/	Quick Look
458	CENA LOBE 2	201.7887	-39.7611	201.063779	-39.501882	215.867616	-28.245975	310.35734609	22.59512331	290.5003	56122.1648958333	2012-07-14 03:57:27	56122.4584490741	2012-07-14 11:00:10	807041020	12.9463	80	12.9463	12.9463	0	12.9463	1	1	0	1	1	0	0	12.6518	12.6518	25.3519	0	PROCESSED	57606.6009027778	2016-08-06 14:25:18	56018	2012-04-01 00:00:00	56142.1626736111	2012-08-03 03:54:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070106	Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LUKASZ STAWARZ		JAP	7	AO7	STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807041020/	Quick Look
459	FG09	160.7604	0.8965	160.118108	1.158829	161.901438	-6.701816	247.95154277	49.5505044	288.8833	56077.2212731482	2012-05-30 05:18:38	56077.5397337963	2012-05-30 12:57:13	807050010	12.49	10	12.4944	12.49	0	12.5	1	1	0	1	1	0	0	10.8506	10.8506	27.5119	0	PROCESSED	57605.5584722222	2016-08-05 13:24:12	56462	2013-06-19 00:00:00	56096.107662037	2012-06-18 02:35:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071511	Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ELENA D'ONGHIA		USA	7	AO7	SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807050010/	Quick Look
460	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
461	FG03	118.182	45.9572	117.286088	46.086737	111.16384	24.564923	173.26592635	29.42392711	92.9981	56228.7772453704	2012-10-28 18:39:14	56229.1078819444	2012-10-29 02:35:21	807052010	14.3185	10	14.3265	14.3185	0	14.3345	1	1	0	1	1	0	0	15.365	15.365	28.544	0	PROCESSED	57607.868125	2016-08-07 20:50:06	56696	2014-02-08 00:00:00	56330.5013541667	2013-02-07 12:01:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071511	Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ELENA D'ONGHIA		USA	7	AO7	SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807052010/	Quick Look
462	ANTLIA NW4	156.477	-34.4731	155.913183	-34.218342	174.203454	-40.552676	271.69853818	19.42589093	299.2985	57168.4177546296	2015-05-26 10:01:34	57169.4605902778	2015-05-27 11:03:15	810066010	6.3596	40	6.3596	6.8635	0	6.8635	3	2	0	2	1	0	0	6.7341	6.7341	78.0621	0	PROCESSED	57618.7963657407	2016-08-18 19:06:46	57626	2016-08-26 00:00:00	57178.2408101852	2015-06-05 05:46:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101522	We have measured hot gas properties of the nearest non-cool core cluster, Antlia, in the eastern direction out to R200. Our initial results suggest that its density profile is more consistent with some massive clusters, but significantly steeper than its cool core counterpart with a similar temperature (mass), Virgo. We propose to extend our program to observe two other directions to test azimuthal variation, which is likely to be significant. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KA-WAH WONG		USA	10	AO10	MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/810066010/	Quick Look
463	A2256N	256.1941	78.9961	256.949832	79.060716	101.697267	76.992175	111.38046428	31.59001765	219.8042	56234.8690625	2012-11-03 20:51:27	56236.1877083333	2012-11-05 04:30:18	807024010	62.2855	60	62.2855	62.2855	0	62.2855	1	1	0	1	1	0	0	76.5361	76.5361	113.9039	0	PROCESSED	57607.9455555556	2016-08-07 22:41:36	56630	2013-12-04 00:00:00	56260.5238657407	2012-11-29 12:34:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070058	We observe outskirts of the famous merging cluster of galaxies A2256 with 4 pointings (60ks for each), and obtain spatial distributions of temperature, electron density, pressure and entropy. In a recent study, the thermal profiles after a merger are thought to be similar to those at cluster formation age. By comparing the spatial distributions of A2256 with those of nearby relaxed clusters, we observationally study the evolution of thermal spatial properties of the ICM in the course of cluster evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MADOKA KAWAHARADA		JAP	7	AO7	THERMAL EVOLUTION OF THE ICM STUDIED WITH A2256	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807024010/	Quick Look
464	FG26	237.2323	8.8441	236.628181	8.995997	232.656986	28.135005	17.92603672	44.32356312	282.0742	56137.0874305556	2012-07-29 02:05:54	56137.3307986111	2012-07-29 07:56:21	807054010	11.8912	10	11.8912	11.8912	0	11.8912	1	1	0	1	1	0	0	8.5983	8.5983	20.9999	0	PROCESSED	57606.6870023148	2016-08-06 16:29:17	56626	2013-11-30 00:00:00	56260.480474537	2012-11-29 11:31:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071511	Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ELENA D'ONGHIA		USA	7	AO7	SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807054010/	Quick Look
465	ANTLIA E2	158.2496	-35.3292	157.682674	-35.071089	176.423673	-40.599314	273.48585529	19.50669913	277.9997	56092.2642361111	2012-06-14 06:20:30	56093.0181944444	2012-06-15 00:26:12	807067010	24.1741	23	24.1821	24.1741	0	24.1901	2	2	0	2	1	0	0	22.8534	22.8534	65.1359	3	PROCESSED	57605.6727546296	2016-08-05 16:08:46	56476	2013-07-03 00:00:00	56110.5259027778	2012-07-02 12:37:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071521	We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	7	AO7	MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807067010/	Quick Look
466	ABELL 2597	351.2512	-12.298	350.600815	-12.572949	347.099073	-7.834502	64.91051751	-64.90126459	250.0013	56264.7750115741	2012-12-03 18:36:01	56266.2606134259	2012-12-05 06:15:17	807073040	54.7187	50	54.7187	54.7427	0	54.7267	2	2	0	2	1	0	0	47.919	47.919	128.3278	1	PROCESSED	57608.2146759259	2016-08-08 05:09:08	56018	2012-04-01 00:00:00	56279.7033912037	2012-12-18 16:52:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073040/	Quick Look
467	COMA NW7	194.0035	29.6909	193.400635	29.961328	179.713479	32.548963	101.76403044	87.24693436	319.9995	55735.2525925926	2011-06-23 06:03:44	55735.5383680556	2011-06-23 12:55:15	806046010	16.1218	15	16.1514	16.1458	0	16.1218	1	1	0	1	1	0	0	14.8517	14.8517	24.6879	0	PROCESSED	57602.3868518518	2016-08-02 09:17:04	55652	2011-04-01 00:00:00	55768.6489930556	2011-07-26 15:34:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806046010/	Quick Look
468	AWM7 27' SOUTH	43.6454	41.2726	42.837995	41.069836	53.624746	23.507895	146.50839268	-15.89370788	257.401	55975.6646296296	2012-02-18 15:57:04	55976.5071180556	2012-02-19 12:10:15	806009010	34.9735	30	34.9815	34.9735	0	34.9735	2	2	0	2	1	0	0	33.6452	33.6452	72.7819	1	PROCESSED	57604.6468055556	2016-08-04 15:31:24	56361	2013-03-10 00:00:00	55994.9781828704	2012-03-08 23:28:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060029	X-ray observations of cluster outskirts give us valuable information about star formation and metal enrichment histories in clusters. Here, we propose to observe three fields with total exposures of 100 ks, 45' east, 27' and 45' south from the center. With these observations, we will compare distributions of Fe and galaxies up to 0.6r180, and study metal-enrichment history in filaments of large-scale structure.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	6	AO6	DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM OF AWM7 CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806009010/	Quick Look
469	J2218.6-0346	334.6629	-3.7693	334.013965	-4.02026	335.129241	6.290164	58.79146355	-46.71055995	71.7798	56063.8991550926	2012-05-16 21:34:47	56064.7196875	2012-05-17 17:16:21	807085010	28.629	25	28.629	28.629	0	28.629	2	2	0	2	1	0	0	26.8327	26.8327	70.8839	1	PROCESSED	57605.4341550926	2016-08-05 10:25:11	56442	2013-05-30 00:00:00	56076.0273726852	2012-05-29 00:39:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072018	We propose to observe the three clusters of galaxies J2218.2-0350, J2218.6-0346 and J2218.8-0258 with exposure times of 15, 25 and 35 ks respectively. These clusters are part of a structure of four linearly aligned clusters, separated from each other by 4 to 10 Mpc. We will accurately determine their masses and orientation. This will allow us to fully map the tidal force field of the structure, which is the prime force behind the formation of filaments in the cosmic web. We will study the effects of cluster mass, separation and mutual orientation on the filamentary structure of the cosmic web and on the evolution of galaxies therein.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	E.G. PATRICK BOS		EUR	7	AO7	CLUSTERS AND THE COSMIC WEB	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807085010/	Quick Look
470	MS 1512.4+3647	228.6059	36.6198	228.120322	36.804723	210.693369	51.882401	59.43888584	58.40149096	128.9265	54463.6508449074	2007-12-29 15:37:13	54469.6946527778	2008-01-04 16:40:18	802034010	268.8898	200	268.9458	268.8898	0	268.9458	2	2	0	2	1	0	0	47.4803	47.4803	102.8019	2	PROCESSED	57541.0217476852	2016-06-02 00:31:19	54909	2009-03-19 00:00:00	54542.2596296296	2008-03-17 06:13:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020086	Evolution of the amount of metals depends on history of super novae activities and metal tranport from inter-stellar space into the ICM. We observe a distant cluster, MS 1512+3647 (z=0.372), and determine the abundance ratio of alpha particles which are created by type II supernovae to iron by type Ia. This reveals the evolution of branch ratio of metals in a galaxy between stars and the ICM which has been unresolved observationally.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	2	AO2	EVOLUTION STUDY ON AMOUNT OF METALS IN THE ICM USING A DISTANT CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802034010/	Quick Look
471	A2061	230.3095	30.6453	229.795666	30.824015	216.361499	46.967712	48.13899774	57.1713197	293.2901	53943.6955092593	2006-07-27 16:41:32	53943.9946643518	2006-07-27 23:52:19	801081010	13.8887	14	13.9047	13.9047	13.8887	13.8967	1	1	1	1	1	0	0	11.8443	11.8443	25.8399	0	PROCESSED	57535.0552083333	2016-05-27 01:19:30	54401	2007-10-28 00:00:00	53955.6442939815	2006-08-08 15:27:47	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801081010/	Quick Look
472	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
473	A2249	257.46	34.4851	257.00595	34.546595	250.753931	57.089244	57.64541352	34.94797305	129.9858	54114.5939467593	2007-01-14 14:15:17	54115.1252777778	2007-01-15 03:00:24	801082010	22.8156	15	22.8156	22.8236	0	22.8236	1	1	0	1	1	0	0	19.7637	19.7637	45.9039	1	PROCESSED	57536.8308333333	2016-05-28 19:56:24	54695	2008-08-17 00:00:00	54133.0295833333	2007-02-02 00:42:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801082010/	Quick Look
474	THE MOON	344.0153	-3.4	343.369759	-3.667219	343.958901	3.149835	68.62224539	-53.63365394	247.8502	56990.8695717593	2014-11-29 20:52:11	56991.0002546296	2014-11-30 00:00:22	809001360	4.8998	45	4.8998	4.8998	0	4.8998	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.4137615741	2016-08-17 09:55:49	57415	2016-01-28 00:00:00	57007.4035648148	2014-12-16 09:41:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001360/	Quick Look
475	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
476	CIZA J2242 OFFSET	339.3149	52.6806	338.804058	52.420641	11.931322	54.574747	103.28112871	-4.99517915	17.9944	55772.8222337963	2011-07-30 19:44:01	55774.1446180556	2011-08-01 03:28:15	806002010	55.9134	60	55.9356	55.9134	0	55.9134	2	2	0	2	1	0	0	73.1891	73.1891	114.2	2	PROCESSED	57602.7241666667	2016-08-02 17:22:48	56162	2012-08-23 00:00:00	55792.2422222222	2011-08-19 05:48:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060014	Radio relics in merging clusters have been considered to be synchrotron emission at a shock front. Nevertheless, no concrete evidence of the connection between relics and shocks has been unveiled yet. We propose a SUZAKU observation of a giant radio relic in a new merging cluster CIZA J2242.8+5301 recently discovered. Temperature and density maps across the giant radio relic will provide a clear illustration of the shock structure or a strong constraint of an origin of the radio relic.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HAJIME KAWAHARA	SHO NISHINO	JAP	6	AO6	SUZAKU OBSERVATION OF A NEW MERGING CLUSTER WITH A GIANT RADIO RELIC	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806002010/	Quick Look
477	FILAMENT JUNCTION 2	149.2538	26.1497	148.542222	26.388047	142.296251	12.813389	204.13118538	51.20952403	290.4949	55699.3618402778	2011-05-18 08:41:03	55701.114849537	2011-05-20 02:45:23	806004010	70.1591	70	70.1591	70.1671	0	70.1671	2	2	0	2	1	0	0	63.3295	63.3295	151.4357	1	PROCESSED	57602.1051851852	2016-08-02 02:31:28	56092	2012-06-14 00:00:00	55722.7303356482	2011-06-10 17:31:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060015	Haloes, such as galaxy clusters or groups have been considered to form at intersections of cosmological filaments. Nevertheless, there are a lot of junctions of galaxy filaments without X-ray strong signal from massive clusters. We propose a SUZAKU observation of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey using a new method. The SUZAKU observation of high sensitivity in low energy will reveal nature of faint haloes growing in the large filament junctions.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HAJIME KAWAHARA		JAP	6	AO6	EXPLORING JUNCTIONS OF GALAXY FILAMENTS BY SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806004010/	Quick Look
478	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
479	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
480	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
481	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
482	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
483	NGC 720 OFFSET	28.2673	-13.4983	27.658292	-13.744232	21.049561	-23.414412	172.55217141	-70.17529179	242.404	55560.2543634259	2010-12-30 06:06:17	55565.2502083333	2011-01-04 06:00:18	805069010	223.9663	150	223.9722	223.9663	0	223.9722	2	2	0	2	1	0	0	13.3571	13.3571	28.3639	0	PROCESSED	57600.5655671296	2016-07-31 13:34:25	55994	2012-03-08 00:00:00	55627.1378009259	2011-03-07 03:18:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051503	Models of galaxy formation suggest that as many as half the baryons may reside in an extended, hot halo. Detecting such a halo around a disk galaxy is, however, extremely challenging for current instrumentation. We propose instead to measure the baryon content of an isolated, X-ray bright elliptical galaxy (Mvir~6E12Msun), which provides the best opportunity to take a census of the baryons in a normal, galaxy-scale system. Currently little is known about the total baryon content of such objects, which are the likely end points of spiral galaxy merging. Combined with archival data, our offset pointing will enable the gas to be traced to ~0.75R500, comparable to what has been achieved for galaxy groups and clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	PHILIP HUMPHREY		USA	5	AO5	THE BARYON FRACTION OF AN ISOLATED ELLIPTICAL GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805069010/	Quick Look
484	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
485	AWM7 SE1	44.3556	41.1876	43.546511	40.987213	54.148816	23.260587	147.03812428	-15.71286613	256.9997	56706.6681828704	2014-02-18 16:02:11	56707.1284953704	2014-02-19 03:05:02	808025010	16.8194	15	16.8194	16.8434	0	16.8274	2	2	0	2	1	0	0	15.321	15.321	39.7619	0	PROCESSED	57613.8533912037	2016-08-13 20:28:53	57085	2015-03-04 00:00:00	56719.747662037	2014-03-03 17:56:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080034	We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	8	AO8	METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808025010/	Quick Look
486	MKW4	181.137	1.9141	180.496491	2.192466	180.278577	2.208157	276.9409609	62.39583381	136.3986	56655.392662037	2013-12-29 09:25:26	56656.271099537	2013-12-30 06:30:23	808066010	34.57	30	34.57	34.57	0	34.57	2	2	0	2	1	0	0	30.1435	30.1435	75.8879	0	PROCESSED	57613.7104861111	2016-08-13 17:03:06	57033	2015-01-11 00:00:00	56667.6362268518	2014-01-10 15:16:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081512	We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUANYUAN SU		USA	8	AO8	PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808066010/	Quick Look
487	A3528-S OFFSET 3	194.0873	-29.8404	193.408879	-29.569931	204.956936	-21.869821	304.20210274	33.01923597	288.9994	56502.3985300926	2013-07-29 09:33:53	56503.6522453704	2013-07-30 15:39:14	808106010	61.2339	60	61.2579	61.2499	0	61.2339	2	2	0	2	1	0	0	61.6474	61.6474	108.3097	2	PROCESSED	57612.1235763889	2016-08-12 02:57:57	56955	2014-10-25 00:00:00	56587.4691782407	2013-10-22 11:15:37	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082018	We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	8	AO8	TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808106010/	Quick Look
488	AWM7 BGD	41.6937	42.4876	40.885444	42.278459	52.542503	25.125109	144.58796377	-15.48250354	257.001	56707.9150810185	2014-02-19 21:57:43	56708.3828587963	2014-02-20 09:11:19	808027010	20.4971	20	20.5011	20.5051	0	20.4971	2	2	0	2	1	0	0	22.116	22.116	40.41	0	PROCESSED	57613.8622106482	2016-08-13 20:41:35	57086	2015-03-05 00:00:00	56720.6154976852	2014-03-04 14:46:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080034	We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	8	AO8	METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808027010/	Quick Look
489	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
490	NGC 5044	198.8504	-16.3899	198.183934	-16.125889	203.593771	-7.791309	311.2339251	46.09520433	290.0016	53918.7631712963	2006-07-02 18:18:58	53919.3600115741	2006-07-03 08:38:25	801046010	19.7466	20	19.7466	19.7466	19.7466	19.7466	2	2	2	2	1	0	0	17.9716	17.9716	51.562	1	PROCESSED	57534.8255208333	2016-05-26 19:48:45	54394	2007-10-21 00:00:00	53930.6133217593	2006-07-14 14:43:11	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010092	We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	1	AO1	THE METAL DISTRIBUTION OF THE NGC 5044 GROUP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801046010/	Quick Look
491	THE MOON	17.8678	7.6685	17.216041	7.403045	19.391263	0.083978	131.57870726	-54.86656285	73.8004	56856.4839814815	2014-07-18 11:36:56	56856.6565162037	2014-07-18 15:45:23	809001100	8.2482	45	8.2642	8.2482	0	8.2642	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.3962962963	2016-08-15 09:30:40	57233	2015-07-30 00:00:00	56867.7358912037	2014-07-29 17:39:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001100/	Quick Look
492	THE MOON	27.6562	10.6142	26.991894	10.366866	29.46244	-0.715898	145.72862444	-49.61972993	73.8014	56857.2778935185	2014-07-19 06:40:10	56857.4015856482	2014-07-19 09:38:17	809001160	6.3331	45	6.3411	6.3411	0	6.3331	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.4093287037	2016-08-15 09:49:26	57267	2015-09-02 00:00:00	56902.690775463	2014-09-02 16:34:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001160/	Quick Look
493	CEN_A_LOBE_N1	201.8136	-42.0782	201.081414	-41.819016	217.012441	-30.336854	310.00727378	20.30096505	292.0832	56859.7082060185	2014-07-21 16:59:49	56861.2571990741	2014-07-23 06:10:22	809002010	50.3801	50	50.3881	50.3881	0	50.3801	2	2	0	2	1	0	0	11.4775	11.4775	24.4719	0	PROCESSED	57615.4533333333	2016-08-15 10:52:48	57242	2015-08-08 00:00:00	56875.1360185185	2014-08-06 03:15:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090021	In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROMI SETA		JAP	9	AO9	MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809002010/	Quick Look
494	A3112BG	50.3312	-44.7001	49.902687	-44.878678	26.087437	-59.659599	253.38993788	-55.36648392	25.002	56828.7830208333	2014-06-20 18:47:33	56829.3648611111	2014-06-21 08:45:24	809028010	13.041	30	13.041	13.041	0	24.268	1	1	0	1	1	0	0	20.199	20.199	50.2559	0	PROCESSED	57615.2871064815	2016-08-15 06:53:26	57394	2016-01-07 00:00:00	56873.1992824074	2014-08-04 04:46:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090061	We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KOSUKE SATO		JAP	9	AO9	ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809028010/	Quick Look
495	FJ0854+4908_OFFSET	133.7467	48.8373	132.873661	49.028229	121.743576	30.102388	170.52256786	40.09070343	275.4911	56776.9674074074	2014-04-29 23:13:04	56777.6286805556	2014-04-30 15:05:18	809039010	31.9155	30	31.9155	31.9155	0	31.9155	2	2	0	2	1	0	0	28.928	28.928	57.1259	0	PROCESSED	57615.0205555556	2016-08-15 00:29:36	57218	2015-07-15 00:00:00	56852.6002546296	2014-07-14 14:24:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090090	Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	IKUYUKI MITSUISHI		JAP	9	AO9	EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809039010/	Quick Look
496	FJ1336+3553	203.9051	36.0067	203.345869	36.26171	185.165039	42.045012	79.05269341	77.07938329	299.9994	56835.5627546296	2014-06-27 13:30:22	56836.6564814815	2014-06-28 15:45:20	809040010	49.8464	50	49.8464	49.8464	0	49.8464	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.3306828704	2016-08-15 07:56:11	57212	2015-07-09 00:00:00	56846.5971180556	2014-07-08 14:19:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090090	Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	IKUYUKI MITSUISHI		JAP	9	AO9	EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809040010/	Quick Look
497	NGC3221	155.5344	21.5594	154.847338	21.812076	149.453825	10.59718	213.96748211	55.66659318	113.4999	56977.5304513889	2014-11-16 12:43:51	56980.5453125	2014-11-19 13:05:15	809051010	121.2459	120	121.2459	121.2459	0	121.2459	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.8106018518	2016-08-16 19:27:16	57362	2015-12-06 00:00:00	56995.6190162037	2014-12-04 14:51:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091501	Late-type galaxies in the Local Universe are missing over 70% of their baryonic mass, a large fraction of which is likely embedded in the extended, low density warm-hot gaseous halo. However, searches of hot diffuse halos around massive spiral galaxies found them to be relatively small and not very massive. The UV observations have shown that the baryonic halo mass depends on the specific star formation rate (sSFR) and not on the total mass of the galaxy. We propose to observe the halo emission of NGC3221 with very high sSFR. Detection and characterization of the hot halo around this galaxy will expand our understanding of the dependence of halo properties on galaxy properties, and advance our understanding of galaxy formation, feedback and metal enrichment proposed by theoretical models.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ANJALI GUPTA		USA	9	AO9	SEARCH FOR THE HOT GASEOUS HALO AROUND THE NEARBY SPIRAL GALAXY NGC3221	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809051010/	Quick Look
498	OFF-FIELD2	156.3941	20.5095	155.710931	20.763905	150.605485	9.917753	216.1857144	56.11255364	112.0717	56982.1681018518	2014-11-21 04:02:04	56983.2640046296	2014-11-22 06:20:10	809053010	39.8287	40	39.8287	39.8287	0	39.8287	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.8087847222	2016-08-16 19:24:39	57377	2015-12-21 00:00:00	57009.4169444444	2014-12-18 10:00:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091501	Late-type galaxies in the Local Universe are missing over 70% of their baryonic mass, a large fraction of which is likely embedded in the extended, low density warm-hot gaseous halo. However, searches of hot diffuse halos around massive spiral galaxies found them to be relatively small and not very massive. The UV observations have shown that the baryonic halo mass depends on the specific star formation rate (sSFR) and not on the total mass of the galaxy. We propose to observe the halo emission of NGC3221 with very high sSFR. Detection and characterization of the hot halo around this galaxy will expand our understanding of the dependence of halo properties on galaxy properties, and advance our understanding of galaxy formation, feedback and metal enrichment proposed by theoretical models.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ANJALI GUPTA		USA	9	AO9	SEARCH FOR THE HOT GASEOUS HALO AROUND THE NEARBY SPIRAL GALAXY NGC3221	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809053010/	Quick Look
499	MKW4-WN	181.4571	2.3391	180.816687	2.617439	180.402943	2.725316	277.2234025	62.91169747	110.2998	56994.5218865741	2014-12-03 12:31:31	56996.9723842593	2014-12-05 23:20:14	809062010	90.3652	100	90.3652	91.5172	0	91.5172	2	2	0	2	1	0	0	88.7385	88.7385	211.7057	1	PROCESSED	57617.4717361111	2016-08-17 11:19:18	56748	2014-04-01 00:00:00	57007.0908912037	2014-12-16 02:10:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091513	We propose to observe the nearby group MKW4 by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Four additional pointings, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variation. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUANYUAN SU		USA	9	AO9	PROBING A TYPICAL GALAXY GROUP TO ITS VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809062010/	Quick Look
500	FORNAX OFFSET1	54.5865	-35.7706	54.109381	-35.93292	38.512958	-53.072025	237.25707491	-53.65522298	45.0001	54662.3087962963	2008-07-15 07:24:40	54663.2106365741	2008-07-16 05:03:19	803006010	35.2402	30	35.2482	35.2402	0	35.2513	2	2	0	2	1	0	0	30.441	30.441	77.9179	0	PROCESSED	57543.0490393518	2016-06-04 01:10:37	55055	2009-08-12 00:00:00	54686.1787384259	2008-08-08 04:17:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030036	We proposeto observe 5 offset pointings of the Fornax cluster for 160 ks with Suzaku. The purpose of the observation is to determine O, Mg and Fe distribution of the intracluster medium up to 0.15-0.2 r180 and to study the origin of the metals.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	3	AO3	METAL DISTRIBUTION OF THE FORNAX CLUSTER UP TO 0.2R180.	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803006010/	Quick Look
501	PERSEUS OFFSET-E	49.943	41.2145	49.117489	41.033844	58.512606	22.054116	150.73941272	-13.51227041	269.9995	55615.1921180556	2011-02-23 04:36:39	55615.8335416667	2011-02-23 20:00:18	805045010	27.4595	25	27.4755	27.4595	0	27.4755	2	2	0	2	1	0	0	25.5296	25.5296	55.3919	0	PROCESSED	57601.0240856482	2016-08-01 00:34:41	55996	2012-03-10 00:00:00	55628.1301157407	2011-03-08 03:07:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050093	We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKAYUKI TAMURA		JAP	5	AO5	MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805045010/	Quick Look
502	FORNAX A W-LOBE S	50.358	-37.3109	49.88075	-37.489463	32.300433	-53.110983	240.40250552	-56.92779805	62.5011	55012.4989930556	2009-06-30 11:58:33	55013.9619675926	2009-07-01 23:05:14	804038010	52.4253	50	52.4333	52.4333	0	52.4253	2	2	0	2	1	0	0	11.7121	11.7121	36.36	1	PROCESSED	57547.7267013889	2016-06-08 17:26:27	55393	2010-07-16 00:00:00	55026.4458564815	2009-07-14 10:42:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040073	We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MAKOTO TASHIRO		JAP	4	AO4	X-RAY MAPPING OF THE FORNAX A WEST LOBE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804038010/	Quick Look
503	HCG62	193.274	-9.2022	192.623373	-8.930867	195.778851	-3.241931	303.62256693	53.66732525	113.6407	53755.3883333333	2006-01-20 09:19:12	53758.5002199074	2006-01-23 12:00:19	800013020	114.8488	100	114.8568	114.8488	114.8488	114.8568	2	2	2	2	1	0	0	98.7836	98.7836	268.8498	4	PROCESSED	57532.7777199074	2016-05-24 18:39:55	54247	2007-05-27 00:00:00	54040.4546064815	2006-11-01 10:54:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001057	We propose to obtain high-quality spectra of the X-ray brightest, compact group of galaxies HCG62 with Suzaku. The previous ASCA observation has reported that this group has a hard tail in the spectrum. With 100 ksec exposure, we can constrain the flux of the hard component above ~3 keV with much higher accuracy. This will give a great impact in understanding the origin of the hard emission and non-thermal populations in the IGM. Furhtermore determining the metal abundance, particularly Oxygen, in the central and outer regions will give us new, valuable information on metal enrichment processes in the group that is not dominated by a cD galaxy. Suzaku/XIS is the best-suited for our scientific objectives since it has a low background level and the unprecedented high sensitivity.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NAOMI OTA		JAP	0	SWG	MEASURING HARD TAILS AND METAL DISTRIBUTIONS IN THE GALAXY GROUP HCG62	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800013020/	Quick Look
504	RXCJ0605	91.2587	-35.3175	90.815345	-35.312478	91.987157	-58.750453	241.74700639	-24.18215725	309.9853	55322.2226041667	2010-05-06 05:20:33	55323.0307060185	2010-05-07 00:44:13	805065020	40.0231	40	40.0231	40.0231	0	40.0231	2	2	0	2	1	0	0	33.1762	33.1762	69.7899	0	PROCESSED	57551.4119097222	2016-06-12 09:53:09	55287	2010-04-01 00:00:00	55341.5093981482	2010-05-25 12:13:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805065020/	Quick Look
505	ABELL 2199 CENTER	247.1922	39.484	246.76294	39.592842	233.179095	60.039777	62.84241749	43.66620611	252.3681	54009.2972222222	2006-10-01 07:08:00	54009.8967361111	2006-10-01 21:31:18	801056010	24.9282	25	25.4799	24.9282	25.4799	25.4799	2	2	2	2	1	0	0	20.519	20.519	51.7939	1	PROCESSED	57535.7247453704	2016-05-27 17:23:38	54735	2008-09-26 00:00:00	54021.2246990741	2006-10-13 05:23:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010138	Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	1	AO1	PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801056010/	Quick Look
506	A3667_NW_17OFF	302.8177	-56.56	301.819585	-56.708877	291.523842	-35.547493	341.18808838	-33.22347241	74.1682	53861.293912037	2006-05-06 07:03:14	53861.7356944444	2006-05-06 17:39:24	801095010	17.2586	20	17.2826	17.2746	17.2666	17.2586	1	1	1	1	1	0	0	14.2555	14.2555	38.1519	1	PROCESSED	57533.636099537	2016-05-25 15:15:59	54735	2008-09-26 00:00:00	53913.7593518518	2006-06-27 18:13:28	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	013080	We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA	CRAIG SARAZIN	JUS	1	AO1	SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801095010/	Quick Look
507	A2142 OFFSET1	239.3897	27.3899	238.873146	27.532705	228.881511	46.554196	44.41448178	48.88746657	283.7323	54316.0523726852	2007-08-04 01:15:25	54317.0211226852	2007-08-05 00:30:25	802030010	37.6227	30	37.6307	37.6227	0	37.6307	2	2	0	2	1	0	0	29.6677	29.6677	83.6879	1	PROCESSED	57539.4231134259	2016-05-31 10:09:17	54723	2008-09-14 00:00:00	54347.3816087963	2007-09-04 09:09:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020076	We propose to search for redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in a large-scale filament outside of a massive merging cluster of galaxies A2142. This cluster is characterized by prominent cold fronts, elongated X-ray morphology, and Beppo-SAX detection of hard X-ray emission, which all point to a recent merger and the matter density outside should be high. The strong reason why we choose this target is its right redshift (z=0.909), in which XIS sensitivity for redshifted oxygen lines separated from the Galactic lines becomes the highest. We expect 3 times higher sensitivity than our previous attempt for A2218 (Takei et al. in press) where we set 5 times lower upper limit for OVII line intensity than the XMM reported levels in other clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKAYA OHASHI		JAP	2	AO2	WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802030010/	Quick Look
508	ANTLIA CLUSTER	157.5092	-35.3277	156.944615	-35.070958	175.726148	-40.891834	272.94647188	19.18131972	90.0004	54423.2458796296	2007-11-19 05:54:04	54425.0211111111	2007-11-21 00:30:24	802035010	65.9528	60	65.9608	65.9608	0	65.9528	2	2	0	2	1	0	0	58.1064	58.1064	153.3638	2	PROCESSED	57540.5835185185	2016-06-01 14:00:16	54801	2008-12-01 00:00:00	54433.3905092593	2007-11-29 09:22:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020101	Suzaku observation of the non-cD cluster Abell 1060 shows that temperature of intra-cluster medium (ICM) increases toward the center. This phenomenon is exact opposite of that of giant cD clusters, in which temperature of the ICM decreases toward the center. To explain this observation, we have proposed that galaxies moving through the ICM interact magnetohydrodynamically with the ICM. This scenario implies that the galaxies have lost some part of their kinetic energies, while the ICM received the released energies. As a result, the ICM have been efficiently heated near the center in which galaxy number density is high. To strengthen our scenario, we propose to observation and study temperature map of the Antlia cluster which is another non-cD, relaxed, and nearby (z=0.0087) cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKAO KITAGUCHI		JAP	2	AO2	SUZAKU OBSERVATION OF NON-CD ANTLIA CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802035010/	Quick Look
509	AWM7 EAST OFFSET	44.9753	41.5792	44.161968	41.380907	54.762228	23.48981	147.26183994	-15.14450792	259.3934	54492.7386458333	2008-01-27 17:43:39	54494.7016087963	2008-01-29 16:50:19	802044010	85.6177	80	85.6177	85.6177	0	85.6177	2	2	0	2	1	0	0	80.6003	80.6003	169.5838	1	PROCESSED	57541.4783333333	2016-06-02 11:28:48	54888	2009-02-26 00:00:00	54515.5758796296	2008-02-19 13:49:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020139	The bright east-to-west elongated cluster of galaxies AWM7 lies along the large-scale filament of the Pisces-Perseus supercluster, which extends more than 50 Mpc scale. In AO1, we proposed to probe the gas motion up to 27 arcmin from the cluster center, however no significant energy shift of Fe-K line was detected so far in our preliminary results. This implies a secular asymmetric structure of the dark matter halo. We plan to extend the observation to 60 arcmin radius, which corresponds to the 0.6 times the virial radius. By making the east- and south-offset observations each in 60 ks, we intend to conduct precise measurements of temperature and metal abundances over the half virial radius for the first time.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YOSHITAKA ISHISAKI		JAP	2	AO2	TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802044010/	Quick Look
510	NGC 2403	114.2007	65.5918	112.996594	65.703234	103.458828	43.277316	150.58117971	29.1798975	310.3004	53810.5896875	2006-03-16 14:09:09	53811.5884143518	2006-03-17 14:07:19	800021010	72.3687	70	72.3767	72.3687	72.3767	72.3767	2	2	2	2	1	0	0	59.3591	59.3591	86.2779	0	PROCESSED	57533.2480439815	2016-05-25 05:57:11	54247	2007-05-27 00:00:00	54042.0667708333	2006-11-03 01:36:09	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001101	We propose to observe NGC 2403, which is a nearby luminous normal spiral. Our main objective is to search and investigation of diffuse emission components. These include both rather soft (kT = 0.1 - 1 keV) ones already detected from a fair number of spirals, and hot (kT = a few keV) emission which, if established, may become an analogue to the Galactic ridge emission.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUO MAKISHIMA		JAP	0	SWG	A PROPOSAL FOR A 70 KSEC SUZAKU OBSERVATION OF THE NORMAL SPIRAL GALAXY NGC 2403	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800021010/	Quick Look
511	AWM7 SOUTH OFFSET	43.219	40.631	42.416618	40.42683	53.072384	23.000071	146.52769464	-16.61135361	257.3934	54494.7028703704	2008-01-29 16:52:08	54496.618275463	2008-01-31 14:50:19	802045010	31.2959	0	31.3039	31.3039	0	31.2959	2	2	0	2	1	0	0	78.2298	78.2298	165.4718	1	PROCESSED	57541.4808796296	2016-06-02 11:32:28	54888	2009-02-26 00:00:00	54515.1834837963	2008-02-19 04:24:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020139	The bright east-to-west elongated cluster of galaxies AWM7 lies along the large-scale filament of the Pisces-Perseus supercluster, which extends more than 50 Mpc scale. In AO1, we proposed to probe the gas motion up to 27 arcmin from the cluster center, however no significant energy shift of Fe-K line was detected so far in our preliminary results. This implies a secular asymmetric structure of the dark matter halo. We plan to extend the observation to 60 arcmin radius, which corresponds to the 0.6 times the virial radius. By making the east- and south-offset observations each in 60 ks, we intend to conduct precise measurements of temperature and metal abundances over the half virial radius for the first time.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YOSHITAKA ISHISAKI		JAP	2	AO2	TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802045010/	Quick Look
512	AWM7 45' SOUTH	43.6476	40.9695	42.841958	40.766746	53.522914	23.219545	146.6593781	-16.15981584	257.4009	55974.8888078704	2012-02-17 21:19:53	55975.6641087963	2012-02-18 15:56:19	806010010	34.3602	35	34.3602	34.3602	0	34.3602	2	2	0	2	1	0	0	32.0155	32.0155	66.978	1	PROCESSED	57604.6274768518	2016-08-04 15:03:34	56361	2013-03-10 00:00:00	55994.9866319444	2012-03-08 23:40:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060029	X-ray observations of cluster outskirts give us valuable information about star formation and metal enrichment histories in clusters. Here, we propose to observe three fields with total exposures of 100 ks, 45' east, 27' and 45' south from the center. With these observations, we will compare distributions of Fe and galaxies up to 0.6r180, and study metal-enrichment history in filaments of large-scale structure.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	6	AO6	DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM OF AWM7 CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806010010/	Quick Look
513	A426VIR S	48.9041	42.4908	48.073152	42.306326	58.095587	23.496379	149.35896709	-12.86322568	271.5007	56708.3862962963	2014-02-20 09:16:16	56709.0453009259	2014-02-21 01:05:14	808085010	26.26	25	26.284	26.276	0	26.26	2	2	0	2	1	0	0	21.0267	21.0267	56.9339	1	PROCESSED	57613.8719560185	2016-08-13 20:55:37	57086	2015-03-05 00:00:00	56720.6405902778	2014-03-04 15:22:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081526	Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ONDREJ URBAN		USA	8	AO8	SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808085010/	Quick Look
514	A2199_FE	248.2855	39.6383	247.85907	39.742227	234.702574	60.442801	63.09452591	42.82923772	143.2418	56662.5581597222	2014-01-05 13:23:45	56663.4606944444	2014-01-06 11:03:24	808051010	40.3548	40	40.3708	40.3548	0	40.3712	1	1	0	1	1	0	0	39.8119	39.8119	77.9679	1	PROCESSED	57613.7559490741	2016-08-13 18:08:34	57085	2015-03-04 00:00:00	56719.7506597222	2014-03-03 18:00:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080067	We propose to complete pointing observations to cover the entire region of Abell 2199 cluster. Suzaku has performed 21 pointing observations of Abell 2199 cluster (z=0.03), showing remarkable features in the temperature and entropy distributions with high physical resolution, as ``Suzaku AO-6 keyproject'' we proposed. Our target is the only cluster to cover the whole region, achieved solely by Suzaku/XIS among currently available facilities. Therefore, this project can provide us an exquisite, complete information of the cluster gas with the high physical resolution, which would be used as unsurpassed, legacy-type dataset in the X-ray cluster community.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KOSUKE SATO		JAP	8	AO8	COMPLETING THE SUZAKU LEGACY MOSAIC OF ABELL 2199 CLUSTER TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808051010/	Quick Look
515	3EGJ1234 1318_1	188.0173	-13.3363	187.367898	-13.060386	192.646727	-9.069223	295.70141073	49.26333697	109.7313	54081.3723032407	2006-12-12 08:56:07	54081.9273032407	2006-12-12 22:15:19	801031010	19.4098	20	19.4178	19.4178	0	19.4098	2	2	0	2	1	0	0	18.7228	18.7228	47.9499	1	PROCESSED	57536.3099768518	2016-05-28 07:26:22	54735	2008-09-26 00:00:00	54094.2359722222	2006-12-25 05:39:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010068	We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ?sim 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TOMONORI TOTANI		JAP	1	AO1	CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801031010/	Quick Look
516	3EGJ1234 1318_2	188.017	-13.0869	187.367769	-12.810986	192.545784	-8.84065	295.65674578	49.51103665	109.9322	54081.9277777778	2006-12-12 22:16:00	54082.7766087963	2006-12-13 18:38:19	801032010	30.9427	30	30.9667	30.9587	0	30.9427	2	2	0	2	1	0	0	26.083	26.083	73.3339	1	PROCESSED	57536.3393055556	2016-05-28 08:08:36	54735	2008-09-26 00:00:00	54094.2665740741	2006-12-25 06:23:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010068	We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ?sim 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TOMONORI TOTANI		JAP	1	AO1	CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801032010/	Quick Look
517	A3667_NW_17OFF	302.869	-56.6666	301.869632	-56.815685	291.522519	-35.657764	341.06051648	-33.2513141	258.9342	54038.8325578704	2006-10-30 19:58:53	54039.0106944444	2006-10-31 00:15:24	801095020	11.9634	10	11.9794	11.9794	11.9634	11.9714	1	1	1	1	1	0	0	8.724	8.724	15.3839	0	PROCESSED	57535.9848032407	2016-05-27 23:38:07	54735	2008-09-26 00:00:00	54056.1858796296	2006-11-17 04:27:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	013080	We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA	CRAIG SARAZIN	JUS	1	AO1	SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801095020/	Quick Look
518	NGC 3079	150.4972	55.6116	149.652795	55.852826	130.116379	40.274577	157.90048948	48.39234685	268.6689	54612.8709722222	2008-05-26 20:54:12	54615.4362731482	2008-05-29 10:28:14	803039020	102.34	100	102.348	102.34	0	102.348	2	2	0	2	1	0	0	102.0031	102.0031	221.6019	2	PROCESSED	57542.6909027778	2016-06-03 16:34:54	54999	2009-06-17 00:00:00	54633.7055439815	2008-06-16 16:55:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031303	We will determine whether AGN can drive galactic-scale winds by observing NGC 3079, the best nearby candidate for such a wind. The edge-on spiral NGC 3079 hosts a Compton-thick AGN and is surrounded by a 40 kpc-scale soft X-ray nebula, the largest manifestation of outflow activity also seen in the optical and radio. Proving the outflow is AGN-driven requires Suzaku's unique abilities. We will measure the AGN luminosity using the HXD in the 15-40 keV range and the 2-10 keV band reflection spectrum to assess whether the AGN can radiatively-or-mechanically power the observed superwind. We will determine the origin of the soft X-ray nebula using the relative elemental abundances in the plasma. We can also detect any significant starburst through the 6.7 keV line emission it would create.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DAVID STRICKLAND		USA	3	AO3	NGC 3079'S 40 KPC-SCALE OUTFLOW: AGN OR STARBURST-DRIVEN?	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803039020/	Quick Look
519	A3667_NW_RELIC	302.5617	-56.3599	301.565299	-56.507728	291.421165	-35.317169	341.42703548	-33.08195751	74.7123	53858.7409837963	2006-05-03 17:47:01	53861.2933449074	2006-05-06 07:02:25	801094010	94.3946	95	94.4026	94.3946	94.3946	94.4026	3	3	3	3	1	0	0	56.2506	56.2506	220.489	4	PROCESSED	57533.7274074074	2016-05-25 17:27:28	54394	2007-10-21 00:00:00	53913.7574189815	2006-06-27 18:10:41	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	013080	We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA	CRAIG SARAZIN	JUS	1	AO1	SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801094010/	Quick Look
520	M87N BRIGHT	187.7	12.7001	187.067492	12.976168	181.920384	14.695127	283.404729	74.78396174	297.7704	54625.0923263889	2008-06-08 02:12:57	54625.6259722222	2008-06-08 15:01:24	803070010	24.2485	20	24.2565	24.2485	0	24.2565	1	1	0	1	1	0	0	20.2709	20.2709	46.1039	1	PROCESSED	57542.7423263889	2016-06-03 17:48:57	55009	2009-06-27 00:00:00	54642.2018865741	2008-06-25 04:50:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032011	We propose to take advantage of Suzaku's low background and good collecting area to observe a strong surface brightness discontinuity, most likely a cold front, in the outskirts of M87. We will make accurate temperature and pressure profiles across this cold front, determine the energy associated with it, and compare this to the energy of known AGN-ICM interaction features in M87. With Suzaku's superior spectral redistribution function we will for the first time measure Mg and O in the M87 outskirts and improve constraints on relative contributions by SNIa and SNII. We will study abundance and abundance-ratio variations across the cold front and determine the role of gas sloshing in transporting metals produced by the central galaxy into the ICM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		EUR	3	AO3	THE ENERGETICS AND METAL ABUNDANCE PATTERNS IN THE OUTSKIRTS OF M87	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803070010/	Quick Look
521	A1689-OFFSET1	198.0484	-1.2633	197.406048	-0.99812	197.124113	5.910782	313.73996571	61.17214089	289.9985	54670.1962962963	2008-07-23 04:42:40	54671.3488773148	2008-07-24 08:22:23	803024010	47.0703	40	47.0703	47.0813	0	47.0783	2	2	0	2	1	0	0	36.3283	36.3283	99.5439	1	PROCESSED	57543.121412037	2016-06-04 02:54:50	55076	2009-09-02 00:00:00	54707.0796180556	2008-08-29 01:54:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030100	We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NOBUHIRO OKABE		JAP	3	AO3	UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803024010/	Quick Look
522	A2029_5	227.4808	5.8608	226.861375	6.050047	223.225848	22.663782	6.38223601	50.81650996	112.9567	55226.2508912037	2010-01-30 06:01:17	55226.875162037	2010-01-30 21:00:14	804024050	21.891	22	21.891	21.891	0	21.891	2	2	0	2	1	0	0	14.3419	14.3419	53.936	0	PROCESSED	57550.432337963	2016-06-11 10:22:34	55638	2011-03-18 00:00:00	55272.0370717593	2010-03-17 00:53:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040030	Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUZURU TAWARA		JAP	4	AO4	TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024050/	Quick Look
523	NGC741S2_P2	29.0179	5.3952	28.364923	5.150978	28.892288	-6.076565	150.99426375	-53.91742537	71.6631	55053.608287037	2009-08-10 14:35:56	55053.8425347222	2009-08-10 20:13:15	804055020	10.5481	10	10.5481	10.5481	0	10.5481	2	2	0	2	1	0	0	9.548	9.548	20.2299	0	PROCESSED	57548.1047800926	2016-06-09 02:30:53	55465	2010-09-26 00:00:00	55098.1704166667	2009-09-24 04:05:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804055020/	Quick Look
524	AWM7 EAST OFFSET	44.0318	41.5949	43.221288	41.393422	54.035202	23.723269	146.61375919	-15.47239178	90.4995	53952.2676967593	2006-08-05 06:25:29	53953.2398611111	2006-08-06 05:45:24	801036010	38.5361	40	38.5361	38.5361	38.5361	38.5361	1	1	1	1	1	0	0	37.541	37.541	83.9599	0	PROCESSED	57535.0870138889	2016-05-27 02:05:18	54394	2007-10-21 00:00:00	54020.7498726852	2006-10-12 17:59:49	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010076	The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKAYA OHASHI		JAP	1	AO1	SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801036010/	Quick Look
525	FJ0854+4908	133.7471	49.1347	132.871607	49.325626	121.634271	30.384389	170.1345398	40.07327965	275.4931	56775.9268865741	2014-04-28 22:14:43	56776.9669328704	2014-04-29 23:12:23	809038010	43.4713	45	43.4713	43.4713	0	43.4713	2	2	0	2	1	0	0	40.2119	40.2119	89.8479	1	PROCESSED	57615.0216666667	2016-08-15 00:31:12	57214	2015-07-11 00:00:00	56848.6454166667	2014-07-10 15:29:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090090	Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	IKUYUKI MITSUISHI		JAP	9	AO9	EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809038010/	Quick Look
526	A1914_OFFSET2	216.77	37.7885	216.258243	38.012199	196.723878	48.617689	66.91478771	67.27662817	134.0016	55565.7291203704	2011-01-04 17:29:56	55566.0216550926	2011-01-05 00:31:11	805092020	17.0912	12	17.0992	17.0912	0	17.1072	1	1	0	1	1	0	0	13.2058	13.2058	25.2719	0	PROCESSED	57600.5511689815	2016-07-31 13:13:41	56037	2012-04-20 00:00:00	55670.1137384259	2011-04-19 02:43:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	053087	We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA	ERIC MILLER	JUS	5	AO5	THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805092020/	Quick Look
527	AWM7 NW1	42.8658	41.9211	42.057041	41.715759	53.244699	24.307791	145.6578115	-15.59334332	257	56705.5358680556	2014-02-17 12:51:39	56705.8668287037	2014-02-17 20:48:14	808023010	14.8576	15	14.8896	14.8576	0	14.8736	1	1	0	1	1	0	0	11.0088	11.0088	28.5839	1	PROCESSED	57613.8366550926	2016-08-13 20:04:47	57085	2015-03-04 00:00:00	56719.7185532407	2014-03-03 17:14:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080034	We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	8	AO8	METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808023010/	Quick Look
528	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
529	COMA E5.5	196.6115	27.8944	196.012448	28.161547	183.085886	31.985086	46.75951976	86.58537166	280.0017	55730.7852546296	2011-06-18 18:50:46	55731.2738657407	2011-06-19 06:34:22	806035010	10.8791	15	10.8871	10.8871	0	10.8791	2	2	0	2	1	0	0	12.5597	12.5597	42.1979	0	PROCESSED	57602.3474537037	2016-08-02 08:20:20	55652	2011-04-01 00:00:00	55770.1742939815	2011-07-28 04:10:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806035010/	Quick Look
530	A2104E	235.1486	-3.297	234.495076	-3.136609	233.617797	15.850396	2.9252225	39.1285511	117.6908	54118.1261226852	2007-01-18 03:01:37	54118.6850231482	2007-01-18 16:26:26	801003010	22.7847	20	22.7847	22.7847	0	22.7847	2	2	0	2	1	0	0	17.7352	17.7352	48.2879	1	PROCESSED	57536.8549189815	2016-05-28 20:31:05	54735	2008-09-26 00:00:00	54132.8631365741	2007-02-01 20:42:55	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010012	We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO HATTORI		JAP	1	AO1	TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801003010/	Quick Look
531	A399/401 FILAMENT	44.7475	13.2485	44.061375	13.049612	46.15841	-3.573964	164.45015039	-39.12843885	74.1756	53966.1736921296	2006-08-19 04:10:07	53969.4641666667	2006-08-22 11:08:24	801020010	151.0601	150	151.0601	151.0681	151.0681	151.0681	2	2	2	2	1	0	0	142.2036	142.2036	284.2738	5	PROCESSED	57535.3984837963	2016-05-27 09:33:49	54526	2008-03-01 00:00:00	54021.1056944444	2006-10-13 02:32:12	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010063	Although warm-hot intergalactic medium (WHIM) is supposed to account for most of the baryon in the Universe, its detection is extremely difficult. Here, we propose to observe the cosmological filament between clusters A399 and A401 with Suzaku. We try to detect the OVII emission line and confirm the existence of WHIM in the filament. We expect that the density of the WHIM in the filament is high, and that the detection will be easier than that in other regions in the Universe. Moreover, since the redshift of the filament is relatively high, we can discriminate between the OVII mission from the WHIM and that from our Galaxy by studying the redshift of the line.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YUTAKA FUJITA		JAP	1	AO1	THE DETECTION OF WHIM IN THE A399/401 FILAMENT	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801020010/	Quick Look
532	ABELL 2204	248.0963	5.6404	247.481247	5.74563	245.314616	27.222606	21.10023438	33.35451369	261.3606	53995.3098958333	2006-09-17 07:26:15	53996.5098958333	2006-09-18 12:14:15	801091010	49.1113	55	49.1113	49.1113	49.1113	49.1113	2	2	2	2	1	0	0	51.9372	51.9372	103.6439	1	PROCESSED	57535.6038194444	2016-05-27 14:29:30	54526	2008-03-01 00:00:00	54020.8840277778	2006-10-12 21:13:00	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012018	Measurements of the intracluster gas temperatures out to large radii, where most of the cluster mass resides, are of the utmost importance for the use of clusters in precision cosmology and for studies of cluster physics. Previous attempts to measure temperatures at the cluster virial radius have failed. Here we show that such measurements appear feasible now for the first time with the Suzaku X-ray CCDs. Furthermore, we show that A2204 and A2163 are optimal targets for such an investigation. We, therefore, propose to observe A2204 for 55 ks and A2163 for 100 ks to measure the gas temperature to 10% and 15% accuracy (1-sigma), respectively, out to the cluster virial radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	THOMAS REIPRICH		EUR	1	AO1	A2204 AND A2163: GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801091010/	Quick Look
533	A1060_OFFSET	159.8425	-27.5312	159.252316	-27.270314	173.386883	-33.06567	270.15539037	26.80693828	96.4852	54425.0245486111	2007-11-21 00:35:21	54427.7988888889	2007-11-23 19:10:24	802028010	103.7993	100	103.7993	103.7993	0	103.7993	2	2	0	2	1	0	0	89.1119	89.1119	239.6797	2	PROCESSED	57540.6102662037	2016-06-01 14:38:47	54804	2008-12-04 00:00:00	54434.2515509259	2007-11-30 06:02:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020060	We propose to observe a 30' offset region of the cluster of galaxies Abell 1060 for 100 ksec to study the temperature and abundance profiles. The central region within ~0.3 times the virial radius, or 380 kpc, has been already observed as one of the SWG targets, and the temperature decrease and differnt profiles of metal abundances are clealy observed (Sato et al. 2006). This observation will reveal the temperature and abundance profiles to half the virial radius. Comparison of the abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the outer cluster region.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KOSUKE SATO		JAP	2	AO2	TEMPERATURE AND ABUNDANCE PROFILES IN THE OUTER REGION OF THE NON-CD CLUSTER A1060	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802028010/	Quick Look
534	A2142 OFFSET2	239.2185	27.5666	238.702662	27.710117	228.594218	46.67807	44.63617571	49.06945571	260.7114	54358.4806597222	2007-09-15 11:32:09	54360.0627893518	2007-09-17 01:30:25	802031010	57.7187	50	57.7187	57.7187	0	57.7187	1	1	0	1	1	0	0	52.5976	52.5976	136.6318	1	PROCESSED	57539.9791666667	2016-05-31 23:30:00	54751	2008-10-12 00:00:00	54371.4005208333	2007-09-28 09:36:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020076	We propose to search for redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in a large-scale filament outside of a massive merging cluster of galaxies A2142. This cluster is characterized by prominent cold fronts, elongated X-ray morphology, and Beppo-SAX detection of hard X-ray emission, which all point to a recent merger and the matter density outside should be high. The strong reason why we choose this target is its right redshift (z=0.909), in which XIS sensitivity for redshifted oxygen lines separated from the Galactic lines becomes the highest. We expect 3 times higher sensitivity than our previous attempt for A2218 (Takei et al. in press) where we set 5 times lower upper limit for OVII line intensity than the XMM reported levels in other clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKAYA OHASHI		JAP	2	AO2	WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802031010/	Quick Look
535	AWM7 SOUTH OFFSET	43.2198	40.6314	42.417413	40.427233	53.073147	23.000259	146.52805812	-16.61071542	257.3937	54519.4104861111	2008-02-23 09:51:06	54521.6112847222	2008-02-25 14:40:15	802045020	91.2272	80	91.2272	91.2272	0	91.2272	2	2	0	2	1	0	0	80.0285	80.0285	190.1139	2	PROCESSED	57541.7536111111	2016-06-02 18:05:12	54904	2009-03-14 00:00:00	54535.283599537	2008-03-10 06:48:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020139	The bright east-to-west elongated cluster of galaxies AWM7 lies along the large-scale filament of the Pisces-Perseus supercluster, which extends more than 50 Mpc scale. In AO1, we proposed to probe the gas motion up to 27 arcmin from the cluster center, however no significant energy shift of Fe-K line was detected so far in our preliminary results. This implies a secular asymmetric structure of the dark matter halo. We plan to extend the observation to 60 arcmin radius, which corresponds to the 0.6 times the virial radius. By making the east- and south-offset observations each in 60 ks, we intend to conduct precise measurements of temperature and metal abundances over the half virial radius for the first time.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YOSHITAKA ISHISAKI		JAP	2	AO2	TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802045020/	Quick Look
536	COMABKG	198.7472	31.648	198.161117	31.912033	183.000201	36.170261	75.72732699	83.16527783	295.0754	54272.0100347222	2007-06-21 00:14:27	54272.7015046296	2007-06-21 16:50:10	802083010	30.7831	30	30.7831	30.7831	0	30.7831	2	2	0	2	1	0	0	26.5058	26.5058	59.7399	0	PROCESSED	57539.0181597222	2016-05-31 00:26:09	54702	2008-08-24 00:00:00	54333.4315393518	2007-08-21 10:21:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	024438	Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JOEL BREGMAN	Yoh Takei	USJ	2	AO2	THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802083010/	Quick Look
537	N44 SB	80.6234	-67.9392	80.661581	-67.984502	334.827675	-86.129494	278.35092966	-33.30497245	311.8533	54565.7359143518	2008-04-09 17:39:43	54566.5084953704	2008-04-10 12:12:14	803036010	30.5568	30	30.5568	30.5568	0	30.5568	2	2	0	2	1	0	0	26.9118	26.9118	66.748	1	PROCESSED	57542.2791898148	2016-06-03 06:42:02	54946	2009-04-25 00:00:00	54580.4450810185	2008-04-24 10:40:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031238	Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 3 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 3 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	LARRY MADDOX		USA	3	AO3	A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803036010/	Quick Look
538	NGC 4406	186.5483	12.9401	185.91466	13.216832	180.759915	14.456271	279.08850556	74.63107328	294.6659	55001.7603125	2009-06-19 18:14:51	55004.4793287037	2009-06-22 11:30:14	803043010	101.7736	90	101.7736	101.7736	0	101.7736	2	2	0	2	1	0	0	86.5545	86.5545	234.8981	2	PROCESSED	57547.6610300926	2016-06-08 15:51:53	55384	2010-07-07 00:00:00	55015.2472569445	2009-07-03 05:56:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031404	We propose Suzaku observations of three elliptical galaxies, selected on brightness and the availability of XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. The low-energy sensitivity, spectral resolution, and low background of the Suzaku XIS enables the first accurate model-independent measurements of the abundance pattern while expanding the number of measurable temperature diagnostic features. Analysis of XIS spectra (critically, with SCI on), exclusively and in combination with RGS data, demonstrates the unique power of Suzaku to contribute to our understanding of the thermal and chemical properties of these systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MICHAEL LOEWENSTEIN		USA	3	AO3	UNCOVERING THE TRUE ABUNDANCES OF ELLIPTICAL GALAXIES WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803043010/	Quick Look
539	DEM L 192	81.4194	-67.497	81.444182	-67.538512	340.379487	-86.530508	277.77177426	-33.0775429	334.6993	54968.6808680556	2009-05-17 16:20:27	54971.0113310185	2009-05-20 00:16:19	804009010	87.3165	80	87.3245	87.3165	0	87.3245	2	2	0	2	1	0	0	80.0589	80.0589	201.3277	2	PROCESSED	57546.6405439815	2016-06-07 15:22:23	55356	2010-06-09 00:00:00	54987.4577314815	2009-06-05 10:59:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040009	The combined actions of fast stellar winds and core-collapse supernova explosions of the massive stars create large shell-like structures, called superbubbles (SBs), by sweeping up the ambient medium. Large tenuous cavities created inside the SB walls allow that the blast shocks of the interior supernova remnants (SNRs) expand rapidly without decelerating for a long time. Therefore, the timescale of efficient cosmic-ray acceleration can be much longer than that of most isolated SNRs. We propose the observations on DEM L 192 and DEM L 205, which are the SBs in the Large Magellanic Cloud, in order to search the large non-thermal SNR shells hidden inside the SBs. They are the strong candidates of the accelerators of the "knee energy" particles.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROYA YAMAGUCHI		JAP	4	AO4	DEM L 192 AND DEM L 205: SUPERBUBBLES IN THE LARGE MAGELLANIC CLOUD	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804009010/	Quick Look
540	FERMI_0281	197.9603	-34.4918	197.262031	-34.226396	210.309678	-24.734564	307.70107754	28.19093927	309.4896	55047.2059606482	2009-08-04 04:56:35	55048.3043287037	2009-08-05 07:18:14	804018010	39.9038	40	39.9038	39.9038	0	39.9038	2	2	0	2	1	0	0	35.5708	35.5708	94.8819	1	PROCESSED	57548.0705902778	2016-06-09 01:41:39	55423	2010-08-15 00:00:00	55060.7435763889	2009-08-17 17:50:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040014	We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JUN KATAOKA		JAP	4	AO4	SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804018010/	Quick Look
541	NGC 5174	202.3569	11.0203	201.73681	11.278322	196.356635	18.897363	333.76702191	71.58014685	102.4436	55219.0472685185	2010-01-23 01:08:04	55220.5835532407	2010-01-24 14:00:19	804048010	54.5151	50	54.5231	54.5151	0	54.5231	2	2	0	2	1	0	0	44.0362	44.0362	132.6979	0	PROCESSED	57550.3479050926	2016-06-11 08:20:59	55595	2011-02-03 00:00:00	55229.1361226852	2010-02-02 03:16:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041504	Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio: the Milky Way retained only 30% of its baryons while lower mass galaxies retain less than 10%. Probably, these baryons were expelled by intense galactic winds during the early star formation period at z = 1-3. These galactic winds can carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding two extremely massive spiral galaxies, with 6-8 times the stellar content of M31 and with v_rot = 370, 420 km/s. If successful, we will detect a significant fraction of the 3-4E11 Msun of the missing baryons as hot gas.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	JOEL BREGMAN		USA	4	AO4	THE BARYON CONTENT OF MASSIVE SPIRAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804048010/	Quick Look
542	FORNAX A W-LOBE N	50.5227	-36.9675	50.043813	-37.145451	32.738272	-52.85468	239.75066849	-56.83654313	27.8129	54991.7546875	2009-06-09 18:06:45	54992.8119675926	2009-06-10 19:29:14	804037010	60.7627	50	60.7707	60.7627	0	60.7707	2	2	0	2	1	0	0	54.817	54.817	91.3258	1	PROCESSED	57547.5602777778	2016-06-08 13:26:48	55367	2010-06-20 00:00:00	55001.1883912037	2009-06-19 04:31:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040073	We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MAKOTO TASHIRO		JAP	4	AO4	X-RAY MAPPING OF THE FORNAX A WEST LOBE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804037010/	Quick Look
543	A1795_FAR_SOUTHWEST	206.9673	26.3143	206.388758	26.56302	193.820617	34.636362	32.43951308	77.37921169	300.5685	55011.5565162037	2009-06-29 13:21:23	55012.4849537037	2009-06-30 11:38:20	804083010	38.3573	35	38.3573	38.6253	0	38.6333	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57598.4742013889	2016-07-29 11:22:51	55395	2010-07-18 00:00:00	55027.5898726852	2009-07-15 14:09:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041528	The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	4	AO4	ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804083010/	Quick Look
544	A2204_FIELD_1	248.3552	5.4547	247.739346	5.558766	245.63481	27.082232	21.05505633	33.03914402	261.0004	55440.0008217593	2010-09-01 00:01:11	55441.1467013889	2010-09-02 03:31:15	805056010	40.6674	40	40.6674	40.6674	0	40.6674	2	2	0	2	1	0	0	37.488	37.488	98.9941	1	PROCESSED	57553.2764699074	2016-06-14 06:38:07	55287	2010-04-01 00:00:00	55456.099849537	2010-09-17 02:23:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805056010/	Quick Look
545	NGC3402 OFF-CENTER	162.4923	-13.1954	161.871445	-12.930338	169.151232	-19.021161	262.91388856	40.05493452	124.5885	55557.4779513889	2010-12-27 11:28:15	55558.1231134259	2010-12-28 02:57:17	805070010	27.8664	30	27.8744	27.8744	0	27.8664	2	2	0	2	1	0	0	25.0294	25.0294	55.74	1	PROCESSED	57554.5274421296	2016-06-15 12:39:31	55961	2012-02-04 00:00:00	55595.0278703704	2011-02-03 00:40:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051512	Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	XINYU DAI		USA	5	AO5	BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805070010/	Quick Look
546	ABELL 115	13.9939	26.3802	13.320825	26.109701	23.360956	18.75409	124.19588168	-36.48041221	44.0022	55401.606087963	2010-07-24 14:32:46	55403.0529398148	2010-07-26 01:16:14	805077010	66.1556	65	66.1629	66.1556	0	66.1829	2	2	0	2	1	0	0	61.8298	61.8298	124.968	2	PROCESSED	57552.6853472222	2016-06-13 16:26:54	55780	2011-08-07 00:00:00	55414.1298148148	2010-08-06 03:06:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051521	We propose central and offset pointed observations of the strongly merging ``double'' cluster A115 to study the properties of the intracluster gas at the virial radius. Ultimately, the results can be compared with results from both relaxed and other merging systems to determine the effects of mergers on the extended gas halos of clusters (e.g., departures from hydrostatic equilibrium, and the level of non-thermal pressure support). Additionally, we will verify the presence of hard X-ray emission between the subclusters, marginally detected in Chandra observations, accurately measure its temperature, and determine its origin by confirming it as hot thermal (shock heated gas) or non-thermal (shock or turbulent accelerated particles) emission.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	SCOTT RANDALL		USA	5	AO5	THE EXTENDED ATMOSPHERES OF STRONGLY MERGING GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805077010/	Quick Look
547	ABELL 2537	347.0895	-2.1864	346.446208	-2.457426	347.265087	3.085071	73.83613509	-54.91382092	56.4647	55368.5295486111	2010-06-21 12:42:33	55371.9946875	2010-06-24 23:52:21	805090010	124.8232	129	124.8472	124.8232	0	124.8472	2	2	0	2	1	0	0	108.3908	108.3908	281.2176	1	PROCESSED	57552.4996412037	2016-06-13 11:59:29	55772	2011-07-30 00:00:00	55403.4592361111	2010-07-26 11:01:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052007	Robust and precise mass measurements for a large number of galaxy clusters represent the single most important step to prepare for dark energy cluster surveys to be performed, e.g., with eROSITA. Robustness and precision can best be achieved by a comparative and combined analysis of independent techniques. Here, we propose to use measurements from Suzaku, APEX-SZ, and wide-field optical telescopes to determine cluster masses up to the virial radius. X-ray, SZ, and gravitational lensing reductions and analyses will all be performed by experts at a single location. We demonstrate that we have selected the optimal targets for this study. Further, we show promising results from our Suzaku analysis of cluster outskirts, from our lensing pipeline, as well as from our combined SZ/X-ray method.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	THOMAS REIPRICH		EUR	5	AO5	COMBINED SUZAKU/APEX-SZ/LENSING MASS MEASUREMENTS OF THE GALAXY CLUSTER A2537	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805090010/	Quick Look
548	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
549	A1795_NEAR_WEST	206.9975	26.5902	206.419777	26.838853	193.705375	34.896895	33.70837645	77.38236805	300.5681	55009.4637962963	2009-06-27 11:07:52	55010.100162037	2009-06-28 02:24:14	804085010	24.2664	20	24.2664	24.5363	0	24.5203	5	2	0	2	1	0	0	9.9711	9.9711	22.7619	0	PROCESSED	57598.4788425926	2016-07-29 11:29:32	55386	2010-07-09 00:00:00	55020.3655555556	2009-07-08 08:46:24	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041528	The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	4	AO4	ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804085010/	Quick Look
550	FORNAX CLUSTER NORTH	54.7043	-35.2293	54.224181	-35.391159	39.001198	-52.608062	236.34100564	-53.57224957	244.9996	53741.5137847222	2006-01-06 12:19:51	53742.3336111111	2006-01-07 08:00:24	800002020	37.1921	80	37.1921	37.2161	37.2081	37.2001	2	2	2	2	1	0	0	39.2874	39.2874	70.8159	1	PROCESSED	57532.6432291667	2016-05-24 15:26:15	54247	2007-05-27 00:00:00	54039.8151041667	2006-10-31 19:33:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001018	The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	0	SWG	MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800002020/	Quick Look
551	NGC3628	170.0699	13.5986	169.41715	13.872528	165.514956	8.570385	240.83294046	64.7853987	100	55890.624212963	2011-11-25 14:58:52	55892.4070601852	2011-11-27 09:46:10	806018010	81.5115	80	81.5275	81.5115	0	81.5218	2	2	0	2	1	0	0	70.5925	70.5925	153.9938	1	PROCESSED	57603.996087963	2016-08-03 23:54:22	56269	2012-12-08 00:00:00	55901.2586689815	2011-12-06 06:12:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060082	We propose 80 ksec observations of edge-on nearby spiral starburst galaxies, NGC3628 and NGC891. We aim to obtain the temperature and the abundance pattern in both the disk and halo regions of two starburst galaxies and hopefully constrain the model of the interactions between not only disk and halo but also halo and intergalactic medium.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	IKUYUKI MITSUISHI		JAP	6	AO6	OBSERVATIONS OF AN EDGE-ON STARBURST GALAXIES NGC3628 & NGC891	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806018010/	Quick Look
552	AWM7 SE2	44.7376	40.9954	43.928492	40.796305	54.382202	22.988972	147.39655193	-15.74105021	257.0003	56707.1291319444	2014-02-19 03:05:57	56707.9132407407	2014-02-19 21:55:04	808026010	35.304	35	35.304	35.316	0	35.308	2	2	0	2	1	0	0	31.1778	31.1778	67.742	4	PROCESSED	57613.8746064815	2016-08-13 20:59:26	57085	2015-03-04 00:00:00	56719.7754398148	2014-03-03 18:36:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080034	We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	8	AO8	METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808026010/	Quick Look
553	COMA NW3.5	194.5289	28.7386	193.925957	29.008414	180.709004	31.910374	80.83345269	87.81635354	116.0021	55917.9522685185	2011-12-22 22:51:16	55918.5091898148	2011-12-23 12:13:14	806040020	16.7407	15	16.7407	16.7631	0	16.7487	2	2	0	2	1	0	0	15.8051	15.8051	48.1159	0	PROCESSED	57604.2115509259	2016-08-04 05:04:38	55652	2011-04-01 00:00:00	55972.6802662037	2012-02-15 16:19:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806040020/	Quick Look
554	A262 NE2	28.537	36.7219	27.798764	36.476514	39.918494	23.346467	136.69850182	-24.46778258	249.9995	56703.1881712963	2014-02-15 04:30:58	56703.8821643518	2014-02-15 21:10:19	808109010	32.9447	32	32.9527	32.9607	0	32.9447	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57613.8208564815	2016-08-13 19:42:02	57080	2015-02-27 00:00:00	56714.743275463	2014-02-26 17:50:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	083002	We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	NORBERT WERNER	JUS	8	AO8	OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808109010/	Quick Look
555	RXCJ0605	91.4642	-35.1179	91.019375	-35.111883	92.302761	-58.547808	241.59260677	-23.96271915	309.9856	55323.8555555556	2010-05-07 20:32:00	55324.6821412037	2010-05-08 16:22:17	805065040	43.6946	40	43.6946	43.6946	0	43.7106	2	2	0	2	1	0	0	39.3321	39.3321	71.4139	0	PROCESSED	57551.4409837963	2016-06-12 10:35:01	55287	2010-04-01 00:00:00	55341.5146990741	2010-05-25 12:21:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805065040/	Quick Look
556	COMA E3	195.8278	27.896	195.226801	28.164193	182.356899	31.675143	49.87218267	87.25778961	279.9974	55729.4896064815	2011-06-17 11:45:02	55729.6863078704	2011-06-17 16:28:17	806032010	7.9801	10	7.9801	7.9801	0	7.9801	1	1	0	1	1	0	0	5.764	5.764	16.9839	0	PROCESSED	57602.3229976852	2016-08-02 07:45:07	55652	2011-04-01 00:00:00	55770.1022453704	2011-07-28 02:27:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806032010/	Quick Look
557	FORNAX A LOBE BKG	50.9375	-37.5569	50.463091	-37.733287	32.824918	-53.528276	240.74738045	-56.44161041	91.6954	56510.6236458333	2013-08-06 14:58:03	56511.9333912037	2013-08-07 22:24:05	808044010	54.4545	50	54.4625	54.4545	0	54.4705	2	2	0	2	1	0	0	46.8925	46.8925	113.1478	1	PROCESSED	57612.1934837963	2016-08-12 04:38:37	56955	2014-10-25 00:00:00	56587.7940046296	2013-10-22 19:03:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080056	We propose Suzaku observations of the Fornax A east radio lobe and the background region. In previous cycles, we observed the west lobe and detected thermal extended gas for the first time, in addition to the non-thermal emission known for decades (Seta PhD thesis, 2012). In order to reveal the relation between the AGN jet and the thermal gas, the additional data in the opposite side of the lobe is critically important. We aim to detect the thermal gas in the eastern lobe, too, and investigate the spatial difference of its temperature and surface brightness.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROMI SETA		JAP	8	AO8	COMPLETING THE MAPPING OBSERVATION OF FORNAX A RADIO LOBE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808044010/	Quick Look
558	N103B	77.15	-68.7359	77.208253	-68.79772	330.089921	-84.667648	279.60217418	-34.399508	199.4598	55194.4728356482	2009-12-29 11:20:53	55200.6044560185	2010-01-04 14:30:25	804039010	223.8999	150	224.0108	223.8999	0	224.0028	2	2	0	2	1	0	0	46.096	46.096	129.9558	0	PROCESSED	57550.0511805556	2016-06-11 01:13:42	55584	2011-01-23 00:00:00	55218.4707060185	2010-01-22 11:17:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040080	We aim to detect very low abundance lines, Cr and Mn, from SNR N103B in the Large Magellanic Cloud which is a low metaricity galaxy. It is known that a mass ratio of Mn to Cr synthesized in Type Ia supernovae is strongly correrated with the metaricity of the progenitor white dwarf. In the early Suzaku observation, we already detected the Cr line with about 3-sigma confidence level. In this follow-up observation, we detect the Cr and Mn lines with significant confidence, and determine the metaricity of the progenitor of SNR N103B. This will be the first measurement of the white dwarf's metaricity in the extra-galactic object.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TORU TAMAGAWA		JAP	4	AO4	A MANGANESE LINE DETECTION FROM SNR N103B IN A LOW METARICITY GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804039010/	Quick Look
559	A478 OFFSET B	63.3675	10.7352	62.68015	10.608912	63.410539	-10.281556	182.20374123	-28.1098658	260.0004	55601.549849537	2011-02-09 13:11:47	55602.6897685185	2011-02-10 16:33:16	805002010	45.3211	45	45.3211	45.3211	0	45.3211	2	2	0	2	1	0	0	34.2117	34.2117	98.4779	1	PROCESSED	57600.9178935185	2016-07-31 22:01:46	55983	2012-02-26 00:00:00	55617.4110763889	2011-02-25 09:51:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050008	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 a representative regular cluster, Abell 478	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA	ANDREW FABIAN	JAP	5	AO5	DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805002010/	Quick Look
560	N49	81.5075	-66.0821	81.488489	-66.123294	4.042744	-86.564563	276.09278992	-33.24378088	327.2258	56056.8032986111	2012-05-09 19:16:45	56060.6898148148	2012-05-13 16:33:20	807007010	184.543	190	184.559	184.543	0	184.559	2	2	0	2	1	0	0	206.5829	206.5829	335.7558	3	PROCESSED	57605.4699189815	2016-08-05 11:16:41	56527	2013-08-23 00:00:00	56161.1703935185	2012-08-22 04:05:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070036	Recently, we discovered recombining plasma (RP) from several mixed-morphology (MM) SNRs in our galaxy, which provides us a new insight into the evolution of SNRs. On the other hand, the RP has not been detected yet from extragalactic SNRs, while many MM-SNRs exist also in extra galaxies. We investigated all the X-ray spectra obtained from previous observations with Suzaku, XMM-Newton and Chandra and found a clear signal of the RP from three LMC SNRs (N49, N23 and DEM L71). Long-time observations with Suzaku XIS will provide us a first evidence of RP from extra galaxies. We propose 2-pointing observations of three SNRs for 290ks.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROYUKI UCHIDA		JAP	7	AO7	FIRST INVESTIGATION OF RECOMBINING PLASMA FROM EXTRAGALACTIC SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807007010/	Quick Look
561	ABELL 3364	87.0888	-31.8215	86.620794	-31.836795	85.667368	-55.219752	236.92588426	-26.48475311	295.0036	55670.3589699074	2011-04-19 08:36:55	55670.9259027778	2011-04-19 22:13:18	806067020	29.9913	29.5	29.9993	29.9913	0	30.0073	1	1	0	1	1	0	0	26.718	26.718	48.9759	0	PROCESSED	57601.5361689815	2016-08-01 12:52:05	56067	2012-05-20 00:00:00	55691.2162037037	2011-05-10 05:11:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061524	Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	6	AO6	THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806067020/	Quick Look
562	CENTAURUS CLUSTER NW	191.8913	-40.8227	191.202719	-40.549873	208.557036	-32.526985	302.14149361	22.04310508	292.0001	56850.5075462963	2014-07-12 12:10:52	56854.4064236111	2014-07-16 09:45:15	809007010	147.8889	150	147.8889	148.5689	0	148.5689	2	2	0	2	1	0	0	14.6625	14.6625	46.016	1	PROCESSED	57615.4267476852	2016-08-15 10:14:31	57283	2015-09-18 00:00:00	56917.6316666667	2014-09-17 15:09:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090031	We propose to observe the north-west offset (20'--40' or 0.4--0.8 r500) of the Centaurus cluster with a 150 ks exposure. A previous Suzaku observation with a 10 ks exposure yielded a very low Fe abundance (0.0-0.1 solar) in the ICM. With a 150 ks exposure, we will detect the Fe-K line of He-like Fe and derive Fe abundance with an accuracy of 0.05 solar. Then, we will be able to study the validity of the Fe abundance derived from the Fe L lines from cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	9	AO9	COMPARISON OF THE FE ABUNDANCES FROM THE L AND K LINES FROM THE CLUSTER OUTSKIRTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809007010/	Quick Look
563	ABELL 3364	86.7248	-31.9341	86.257494	-31.951159	85.117761	-55.320671	236.9466602	-26.81319905	295.0042	55670.9264699074	2011-04-19 22:14:07	55671.5940162037	2011-04-20 14:15:23	806067030	30.7802	29.5	30.7802	30.7802	0	30.7802	2	2	0	2	1	0	0	30.2762	30.2762	57.6639	1	PROCESSED	57601.5516782407	2016-08-01 13:14:25	56059	2012-05-12 00:00:00	55692.1831018518	2011-05-11 04:23:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061524	Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	6	AO6	THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806067030/	Quick Look
564	A3526	191.5735	-40.3305	190.887021	-40.05737	208.034799	-32.201568	301.8706053	22.53064841	109.9984	55943.2367592593	2012-01-17 05:40:56	55943.6161574074	2012-01-17 14:47:16	806087010	14.4943	13	14.4943	14.4943	0	14.4943	2	2	0	2	1	0	0	10.3865	10.3865	32.7799	1	PROCESSED	57604.3860416667	2016-08-04 09:15:54	56332	2013-02-09 00:00:00	55964.1523148148	2012-02-07 03:39:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806087010/	Quick Look
565	A3526	191.429	-40.092	190.743483	-39.818735	207.789532	-32.040636	301.74515791	22.76656347	109.9976	55943.6166319444	2012-01-17 14:47:57	55943.9461111111	2012-01-17 22:42:24	806088010	15.0662	14	15.0702	15.0662	0	15.0662	2	2	0	2	1	0	0	14.8434	14.8434	28.458	1	PROCESSED	57604.3884490741	2016-08-04 09:19:22	56332	2013-02-09 00:00:00	55964.2169675926	2012-02-07 05:12:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806088010/	Quick Look
566	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
567	Z348	16.7077	1.0407	16.065796	0.773597	15.79467	-5.606239	131.03941429	-61.58850223	247.9196	54110.9286689815	2007-01-10 22:17:17	54111.5259722222	2007-01-11 12:37:24	801050010	22.6477	23	22.6477	22.6477	0	22.6477	2	2	0	2	1	0	0	21.3403	21.3403	51.589	1	PROCESSED	57536.8362384259	2016-05-28 20:04:11	54735	2008-09-26 00:00:00	54133.0321643518	2007-02-02 00:46:19	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010098	We propose to carry out the Suzaku/XIS observations of 4 massive clusters at low redshifts (z <0.3). Combining the X-ray data with the existing Subaru datasets that allow us to directly reconstruct the mass distribution from the gravitational lensing measurements, we will investigate the physical relations between the mass and gas distributions to understand the nature of cluster in a quantitative way.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TOSHIFUMI FUTAMASE		JAP	1	AO1	THE ULTIMATE GRAVITATIONAL LENSING STUDY OF GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801050010/	Quick Look
568	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
569	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
570	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
571	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
572	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
573	A2256BKG	259.0594	79.1323	259.847378	79.183226	99.226233	77.073038	111.31764948	31.03227987	219.8044	56236.1893865741	2012-11-05 04:32:43	56237.0696875	2012-11-06 01:40:21	807025010	39.6865	40	39.6865	39.6865	0	39.6865	2	2	0	2	1	0	0	48.9304	48.9304	76.0479	0	PROCESSED	57607.9668634259	2016-08-07 23:12:17	56630	2013-12-04 00:00:00	56264.5702199074	2012-12-03 13:41:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070058	We observe outskirts of the famous merging cluster of galaxies A2256 with 4 pointings (60ks for each), and obtain spatial distributions of temperature, electron density, pressure and entropy. In a recent study, the thermal profiles after a merger are thought to be similar to those at cluster formation age. By comparing the spatial distributions of A2256 with those of nearby relaxed clusters, we observationally study the evolution of thermal spatial properties of the ICM in the course of cluster evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MADOKA KAWAHARADA		JAP	7	AO7	THERMAL EVOLUTION OF THE ICM STUDIED WITH A2256	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807025010/	Quick Look
574	A1631_E	193.4806	-15.4427	192.82259	-15.171579	198.410093	-8.910855	303.81684947	47.4247798	113.0006	56305.0111226852	2013-01-13 00:16:01	56305.7231944445	2013-01-13 17:21:24	807005010	20.5236	20	20.5236	20.5236	0	20.5476	1	1	0	1	1	0	0	20.1111	20.1111	61.5119	1	PROCESSED	57608.4784143518	2016-08-08 11:28:55	56703	2014-02-15 00:00:00	56337.4913425926	2013-02-14 11:47:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070029	In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	7	AO7	PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807005010/	Quick Look
575	NGC6946	308.6989	60.1968	308.436769	60.023263	358.020745	71.889708	95.74917907	11.70533663	79.9968	56060.7040393518	2012-05-13 16:53:49	56063.8903935185	2012-05-16 21:22:10	807035010	198.879	200	198.879	198.8958	0	198.8948	2	2	0	2	1	0	0	182.1955	182.1955	275.2756	3	PROCESSED	57605.4921296296	2016-08-05 11:48:40	56442	2013-05-30 00:00:00	56075.3809027778	2012-05-28 09:08:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070098	Hot X-ray emitting interstellar medium (ISM) carries important information about the history of star formation and evolution of galaxies. However, the origin of hot ISM is still unclear. We investigate the property of hot ISM according to luminosity of infrared emission, which is good tracer of star formation rate. If the hot ISM depend on the present activity of star formation, there are correlation between hot ISM and infrared emission. We propose the observation of the spiral galaxy NGC 6946.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	SAORI KONAMI		JAP	7	AO7	CLARIFICATION OF THE ORIGIN OF HOT ISM IN SPIRAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807035010/	Quick Look
576	FILAMENT JUNCTION A	165.6591	29.2454	164.978754	29.514668	155.086724	21.237285	201.46002358	65.98539565	289.5	56086.3001041667	2012-06-08 07:12:09	56088.1238425926	2012-06-10 02:58:20	807038010	69.1428	70	69.1588	69.1428	0	69.1588	2	2	0	2	1	0	0	62.2992	62.2992	157.5558	1	PROCESSED	57605.6780787037	2016-08-05 16:16:26	56543	2013-09-08 00:00:00	56176.2765046296	2012-09-06 06:38:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070105	We propose Suzaku observations of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey spectroscopic data. Because of the strong gravitational potential, it is likely to exist groups or clusters of galaxies with X-ray halo at filamentary junctions. However, there are many filaments where X-ray emission have not been detected. We will search faint X-ray halos are now growing with accreating baryons through shock heating.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	NORIO SEKIYA		JAP	7	AO7	EXPLORING INTERNAL STRUCTURE OF HALOES AT FILAMENTARY JUNCTIONS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807038010/	Quick Look
577	FILAMENT JUNCTION B	173.7402	21.0892	173.087159	21.365728	165.694635	16.835806	227.90630551	71.55824615	299.4979	56088.1275115741	2012-06-10 03:03:37	56089.3439814815	2012-06-11 08:15:20	807039010	50.1063	50	50.1189	50.1063	0	50.1269	1	1	0	1	1	0	0	40.9818	40.9818	105.0959	0	PROCESSED	57605.6509375	2016-08-05 15:37:21	56543	2013-09-08 00:00:00	56176.2814236111	2012-09-06 06:45:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070105	We propose Suzaku observations of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey spectroscopic data. Because of the strong gravitational potential, it is likely to exist groups or clusters of galaxies with X-ray halo at filamentary junctions. However, there are many filaments where X-ray emission have not been detected. We will search faint X-ray halos are now growing with accreating baryons through shock heating.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	NORIO SEKIYA		JAP	7	AO7	EXPLORING INTERNAL STRUCTURE OF HALOES AT FILAMENTARY JUNCTIONS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807039010/	Quick Look
578	A262 NE1	28.4051	36.5019	27.66806	36.256213	39.720751	23.183318	136.64990456	-24.70790073	250	56702.5986342593	2014-02-14 14:22:02	56703.187662037	2014-02-15 04:30:14	808108010	25.6102	24	25.6102	25.6102	0	25.6102	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57613.8178472222	2016-08-13 19:37:42	57080	2015-02-27 00:00:00	56714.742037037	2014-02-26 17:48:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	083002	We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	NORBERT WERNER	JUS	8	AO8	OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808108010/	Quick Look
579	IC 5157	330.8663	-34.934	330.129358	-35.176355	320.316602	-21.507496	10.02196464	-53.45455848	251.1985	56250.3323611111	2012-11-19 07:58:36	56251.6043287037	2012-11-20 14:30:14	807048010	65.5411	150	65.5411	65.5411	0	65.5411	3	2	0	2	1	0	0	67.764	67.764	109.8861	1	PROCESSED	57608.0722222222	2016-08-08 01:44:00	56018	2012-04-01 00:00:00	56275.5333333333	2012-12-14 12:48:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071503	The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	DAVID BUOTE		USA	7	AO7	THE MASS PROFILES OF ISOLATED ELLIPTICAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807048010/	Quick Look
580	FG30	259.5133	56.677	259.289115	56.728173	238.479728	78.961901	84.88085465	35.08331599	38.7622	56049.4885532407	2012-05-02 11:43:31	56049.7980671296	2012-05-02 19:09:13	807051010	13.9787	10	13.9867	13.9947	0	13.9787	2	2	0	2	1	0	0	15.579	15.579	26.7259	0	PROCESSED	57605.3190856482	2016-08-05 07:39:29	56465	2013-06-22 00:00:00	56099.2218171296	2012-06-21 05:19:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071511	Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ELENA D'ONGHIA		USA	7	AO7	SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807051010/	Quick Look
581	FG15	177.008	56.8964	176.342479	57.174256	146.620123	49.215769	139.35969999	58.16359998	300.5727	56073.7490856482	2012-05-26 17:58:41	56074.0586226852	2012-05-27 01:24:25	807057010	14.0757	15	14.0757	14.0757	0	14.0757	2	2	0	2	1	0	0	15.603	15.603	26.7399	1	PROCESSED	57605.5125578704	2016-08-05 12:18:05	56470	2013-06-27 00:00:00	56103.1467013889	2012-06-25 03:31:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071511	Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ELENA D'ONGHIA		USA	7	AO7	SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807057010/	Quick Look
582	FG24	233.4334	3.6096	232.807042	3.776669	230.06319	22.123365	8.88650115	44.69822064	290.4245	56136.3403935185	2012-07-28 08:10:10	56136.7487152778	2012-07-28 17:58:09	807058010	15.8231	15	15.8231	15.8231	0	15.8231	2	2	0	2	1	0	0	13.191	13.191	35.2759	0	PROCESSED	57606.6653819444	2016-08-06 15:58:09	56527	2013-08-23 00:00:00	56161.2328240741	2012-08-22 05:35:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071511	Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ELENA D'ONGHIA		USA	7	AO7	SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807058010/	Quick Look
583	RXJ1159+5531	179.9812	55.4402	179.338152	55.71852	149.981877	49.065325	137.66567163	60.1900448	115.1582	56268.8799768518	2012-12-07 21:07:10	56269.4140162037	2012-12-08 09:56:11	807064020	21.1432	20	21.1432	21.1512	0	21.1512	2	2	0	2	1	0	0	22.6001	22.6001	46.14	0	PROCESSED	57608.2013310185	2016-08-08 04:49:55	56646	2013-12-20 00:00:00	56279.6625925926	2012-12-18 15:54:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071513	With Chandra and Suzaku we recently constrained the hot gas and dark matter out to the virial radius (rvir=R108) in the fossil group/cluster RXJ1159+5531. Unlike some recent observations of cluster outskirts, the gas fraction is consistent with the cosmic value, and the entropy profile at rvir is consistent with gravity-only structure formation simulations. As a fossil group, RXJ1159+5531 may be unusually relaxed at large scales. If so, the gas properties should not vary much azimuthally. We propose a complementary Suzaku observation to explore this by measuring the gas in a different azimuthal region, more than doubling the current (~27%) azimuthal coverage. Our results will help determine if gas clumping, invoked to explain the outskirts of some clusters, is ubiquitous.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	PHILIP HUMPHREY		USA	7	AO7	RELAXED GAS AT THE VIRIAL RADIUS IN A FOSSIL GROUP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807064020/	Quick Look
584	RXJ1416.4+2315	214.0491	23.1704	213.474982	23.401811	202.508805	34.45187	25.95253376	70.44078356	293.1179	56125.9101736111	2012-07-17 21:50:39	56128.5008796296	2012-07-20 12:01:16	807065020	101.6938	100	101.7018	101.6938	0	101.7018	2	2	0	2	1	0	0	99.6763	99.6763	223.8209	2	PROCESSED	57606.7012037037	2016-08-06 16:49:44	56598	2013-11-02 00:00:00	56232.6190740741	2012-11-01 14:51:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071514	Our study of the fossil group RXJ 1159+5531 does not find the gas clumping invoked to explain unexpectedly flat entropy profiles and large gas fractions near r_vir in some clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation, which may reflect that hydrostatic equilibrium is very accurate in this highly evolved fossil group. To examine whether these results extend to other fossils and to more massive systems, we propose to observe the fossil cluster RXJ 1416.4+2315 (M_vir ~3 x 10^14 M_sun) to constrain its entropy and gas fraction out to r_vir (r_112). Since it is located at a redshift of 0.137, this target provides an efficient means to explore the outer ICM, where a large azimuthal portion (~80%) of r_vir can be observed in a single Suzaku field.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DAVID BUOTE		USA	7	AO7	RXJ1416.4+2315: A MASSIVE FOSSIL CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807065020/	Quick Look
585	ANTLIA E3	158.6143	-35.3303	158.046217	-35.07153	176.766294	-40.455458	273.75347644	19.66467309	278.5008	56093.5404166667	2012-06-15 12:58:12	56094.1877546296	2012-06-16 04:30:22	807068010	23.4861	23	23.5021	23.4861	0	23.5021	2	2	0	2	1	0	0	20.6862	20.6862	55.926	1	PROCESSED	57605.6943287037	2016-08-05 16:39:50	56476	2013-07-03 00:00:00	56110.5216550926	2012-07-02 12:31:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071521	We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	7	AO7	MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807068010/	Quick Look
586	ABELL 665	127.933	65.6581	126.801514	65.827031	110.986153	44.956941	149.97935617	34.81341699	289.9968	56028.5599537037	2012-04-11 13:26:20	56029.4036226852	2012-04-12 09:41:13	807072040	52.791	50	52.791	52.799	0	52.799	2	2	0	2	1	0	0	51.6671	51.6671	72.8859	0	PROCESSED	57605.1597569444	2016-08-05 03:50:03	56018	2012-04-01 00:00:00	56044.1843518518	2012-04-27 04:25:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072040/	Quick Look
587	RCS110104-0351.3	165.266	-3.8543	164.630074	-3.585449	167.943149	-9.357953	257.98650762	49.14106345	115.7008	56286.1353587963	2012-12-25 03:14:55	56287.8716898148	2012-12-26 20:55:14	807076010	76.1379	75	76.1539	76.1379	0	76.1539	2	2	0	2	1	0	0	67.4411	67.4411	150.0018	0	PROCESSED	57608.3704050926	2016-08-08 08:53:23	56690	2014-02-02 00:00:00	56324.5102314815	2013-02-01 12:14:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071525	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	7	AO7	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807076010/	Quick Look
588	SWCL J1403+3212	210.8847	32.2142	210.333728	32.453758	194.392634	41.437605	55.27159844	73.55798506	128.2493	56289.1009837963	2012-12-28 02:25:25	56290.2578587963	2012-12-29 06:11:19	807081010	52.1374	45	52.1374	52.143	0	52.1454	2	2	0	2	1	0	0	42.9868	42.9868	99.9358	0	PROCESSED	57608.4054050926	2016-08-08 09:43:47	56690	2014-02-02 00:00:00	56324.4837152778	2013-02-01 11:36:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071526	The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the formation and evolution of the hot gaseous halos. The scaling relations and their deviations from self-similar model predictions due to non-gravitational processes are also important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z~0.6 galaxy clusters, selected from the Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such the X-ray luminosity and temperature. With this sample, we are able to model the selection functions relatively easily and place cleaner and tighter constraints on the evolution of X-ray properties of galaxy clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	XINYU DAI		USA	7	AO7	X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807081010/	Quick Look
589	HYDRA A FAR SE	139.7	-12.375	139.09881	-12.163612	146.431142	-26.609663	243.28582967	25.05625041	300	56082.6736342593	2012-06-04 16:10:02	56083.9368981482	2012-06-05 22:29:08	807088010	40.939	40	40.947	40.939	0	40.947	2	2	0	2	1	0	0	37.9143	37.9143	109.1358	0	PROCESSED	57605.5894444444	2016-08-05 14:08:48	56464	2013-06-21 00:00:00	56096.2405208333	2012-06-18 05:46:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072020	Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DOMINIQUE ECKERT		EUR	7	AO7	MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807088010/	Quick Look
590	A2163BGD2	243.9063	-6.5323	243.237281	-6.40839	243.158854	14.509957	6.38161233	30.26602519	93.9997	57078.975787037	2015-02-25 23:25:08	57079.8335763889	2015-02-26 20:00:21	809011010	28.8166	30	28.8326	28.8166	0	28.8406	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6710763889	2016-08-17 16:06:21	57458	2016-03-11 00:00:00	57091.463587963	2015-03-10 11:07:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090032	Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	9	AO9	SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809011010/	Quick Look
591	G115.7+17.5	336.6801	78.3035	336.566813	78.048018	59.497327	68.492125	115.72297849	17.51053762	214.3075	56311.7506712963	2013-01-19 18:00:58	56313.7419328704	2013-01-21 17:48:23	807093010	97.8732	100	97.8892	97.8732	0	97.8892	2	2	0	2	1	0	0	94.3977	94.3977	172.0079	1	PROCESSED	57608.5818634259	2016-08-08 13:57:53	56708	2014-02-20 00:00:00	56342.5694097222	2013-02-19 13:39:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072021	We propose to observe 4 galaxy clusters from the first all-sky blind Sunyaev Zeldovich (SZ) effect cluster catalogue produced by the Planck satellite. This catalogue has revealed a new population of clusters previously undetected by X-ray surveys. The Planck SZ selected cluster sample consists of hot, massive, morphologically disturbed clusters that are under-luminous in the soft X-ray band. This exciting population has implications not only for understanding the thermodynamic state of the intracluster medium, but also for cluster cosmology where it represents an important area of phase space in the cluster mass function; it is a pointer to the dynamics of how clusters form through mergers, and to the true spatial density of cluster-mass structures not represented in X-ray surveys.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ANNA SCAIFE		EUR	7	AO7	CONSTRAINING THE THERMODYNAMIC STATE OF NEW PLANCK GALAXY CLUSTERS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807093010/	Quick Look
592	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
593	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
594	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
595	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
596	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
597	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
598	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
599	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
600	A399EAST	44.8284	12.9677	44.143216	12.769088	46.15453	-3.865608	164.75111172	-39.30361408	72.1818	56529.3727777778	2013-08-25 08:56:48	56530.5036921296	2013-08-26 12:05:19	808007010	50.2768	50	50.2928	50.2768	0	50.3008	2	2	0	2	1	0	0	46.3039	46.3039	97.684	0	PROCESSED	57612.4010069444	2016-08-12 09:37:27	56956	2014-10-26 00:00:00	56587.522349537	2013-10-22 12:32:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080004	To investigate (i)the influence of the merging event on IntraCluster Medium (ICM), We propose 40 ks+50 ks ~2 =140 ks observations of the linked region between Abell 399 and Abell 401. A399 (z=0.0724) and A401 (z=0.0737) are expected be in the initial phase of a cluster merger. With Suzaku fs high sensitivity observations, we will (i)determine the ICM physical conditions by measuring the temperature and density distribution, (ii) characterize the dynamical state of the cluster linked region, (iii) confirm the presence of a shock front predicted by numerical simulations. Our study will reveal the nature of initial phase of merging event of clusters of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHITAKA ISHISAKI		JAP	8	AO8	MORPHOLOGY AND PHYSICAL PROPERTIES OF SHOCKED GAS BY MAJOR MERGER IN THE LINKED REGION OF ABELL 399 AND ABELL 401	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808007010/	Quick Look
601	COMA CLUSTER	194.3893	26.9261	193.783242	27.196084	181.532075	30.236179	24.84225016	88.62234831	316.4746	55348.2119907407	2010-06-01 05:05:16	55350.6877199074	2010-06-03 16:30:19	805079010	101.7805	100	101.7805	101.7805	0	101.7805	2	2	0	2	1	0	0	77.4308	77.4308	213.8639	1	PROCESSED	57553.0722685185	2016-06-14 01:44:04	55731	2011-06-19 00:00:00	55365.54125	2010-06-18 12:59:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051523	The metal-enrichment mechanism of the hot gas in clusters of galaxies is still not completely understood, particularly at large (~virial) radii where current metallicity measurements are virtually non-existent. Yet a determinaton of elemental abundances of the gas at this radius will allow us to determine which enrichment mechanism (ram pressure stripping or galactic winds) is prevalant in the outskirts of clusters. We propose a 100 kec Suzaku observation of Coma at the virial radius to determine the Fe and S abundances at this location. The ratio of these two elements will allow us to discriminate among competing models for chemical enrichment.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JIMMY IRWIN		USA	5	AO5	THE DETERMINATION OF THE METALLICITY OF COMA AT THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805079010/	Quick Look
602	A1914_OFFSET3	216.2544	37.895	215.741562	38.120181	196.10746	48.514193	67.56094175	67.61680074	134.0009	55566.0223148148	2011-01-05 00:32:08	55566.4306365741	2011-01-05 10:20:07	805093020	12.8294	12	12.8294	12.8294	0	12.8294	2	2	0	2	1	0	0	13.721	13.721	35.2699	0	PROCESSED	57600.553599537	2016-07-31 13:17:11	55995	2012-03-09 00:00:00	55627.1328009259	2011-03-07 03:11:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	053087	We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA	ERIC MILLER	JUS	5	AO5	THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805093020/	Quick Look
603	A2744_NE	3.7189	-30.3078	3.087931	-30.585769	350.157324	-29.032997	9.14048559	-81.37985976	233.5002	56616.3325694445	2013-11-20 07:58:54	56618.5994791667	2013-11-22 14:23:15	808008010	82.773	80	82.781	82.781	0	82.773	2	2	0	2	1	0	0	71.7365	71.7365	195.8377	2	PROCESSED	57613.443900463	2016-08-13 10:39:13	56995	2014-12-04 00:00:00	56629.7456481482	2013-12-03 17:53:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080005	We propose an additional 80ks pointing to complete our mapping of A2744 out to large radii and constrain the thermodynamical history of the cluster growth. A2744 is a multiple merger, nicknamed Pandora's cluster. Our analysis of existing Suzaku data suggest that this cluster has an anisotropic temperature structure near the virial radius and there is not a simple correlation between temperature and surface mass density of member galaxies. With proposed observations, we can determine, for the first time, the temperature and entropy profiles near the radio relic in the northeast and further test a scenario of gas heating and shock propagation in the cluster outskirts. Suzaku is most suited for this study because of the lowest background and excellent sensitivity.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	NAOMI OTA		JAP	8	AO8	REVEALING THE THERMODYNAMICAL EVOLUTION IN THE PANDORA'S CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808008010/	Quick Look
604	COMA SUBHALO1	195.4003	29.028	194.800096	29.29674	181.356993	32.514724	73.80298118	87.06170231	296.7987	56451.3782638889	2013-06-08 09:04:42	56452.0681712963	2013-06-09 01:38:10	808018010	31.1826	30	31.1906	31.1826	0	31.1906	2	2	0	2	1	0	0	28.8197	28.8197	59.604	1	PROCESSED	57611.5003935185	2016-08-11 12:00:34	56869	2014-07-31 00:00:00	56503.6225462963	2013-07-30 14:56:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080023	We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NOBUHIRO OKABE		JAP	8	AO8	SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808018010/	Quick Look
605	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
606	A3627_NORTH	243.656	-60.6115	242.575411	-60.485559	253.80029	-38.641261	325.45745985	-6.96421785	306.0001	56545.808912037	2013-09-10 19:24:50	56546.5556828704	2013-09-11 13:20:11	808058010	51.8996	50	51.9316	51.9236	0	51.8996	3	2	0	2	1	0	0	43.0284	43.0284	64.5119	1	PROCESSED	57612.6119097222	2016-08-12 14:41:09	56956	2014-10-26 00:00:00	56588.8328935185	2013-10-23 19:59:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080097	We propose to observe the north-west region in nearby merging cluster Abell 3627. Suzaku observation in AO-3 found a subcluster colliding into the main body from the south-east direction and a hard X-ray component above 12 keV probably originated from the north-west region. The region has also peculiar structures such as long X-ray/radio tails, suggesting a relation with the cluster merging. In order to understand the process of cluster merging taking into accout the hard X-ray component and these peculiar structures, we will measure the temperature and pressure distributions in the north-west region using the low background of XIS. We will also study the non-thermal emission using HXD and investigate a possibililty of the particle acceleration in Abell 3627.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KATSUHIRO HAYASHI		JAP	8	AO8	OBSERVATION OF THE NORTH-WEST REGION IN NEARBY MERGING CLUSTER ABELL 3627	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808058010/	Quick Look
607	MKW4-W2	181.7129	1.8545	181.072483	2.132812	180.830723	2.382546	278.14148217	62.56052834	136.8029	56652.6158217593	2013-12-26 14:46:47	56655.3919097222	2013-12-29 09:24:21	808065010	102.6011	100	102.6011	102.6011	0	102.6011	2	2	0	2	1	0	0	88.6977	88.6977	239.8258	1	PROCESSED	57613.7424421296	2016-08-13 17:49:07	57079	2015-02-26 00:00:00	56700.7408449074	2014-02-12 17:46:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081512	We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUANYUAN SU		USA	8	AO8	PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808065010/	Quick Look
608	A133_FIELD_1	15.9453	-21.6335	15.33461	-21.90164	5.595502	-26.095488	150.67449532	-83.82895318	231.9994	56645.5063078704	2013-12-19 12:09:05	56646.6683449074	2013-12-20 16:02:25	808081010	53.6483	50	53.6643	53.6483	0	53.6643	2	2	0	2	1	0	0	52.6512	52.6512	100.3879	1	PROCESSED	57613.6155439815	2016-08-13 14:46:23	57061	2015-02-08 00:00:00	56695.6487152778	2014-02-07 15:34:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081525	We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ERIC MILLER		USA	8	AO8	A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808081010/	Quick Look
609	COMA E2	195.5294	27.8966	194.927658	28.165178	182.080007	31.557077	51.52244118	87.51055859	279.9995	55729.2687268518	2011-06-17 06:26:58	55729.4890856482	2011-06-17 11:44:17	806031010	9.1256	10	9.1336	9.1256	0	9.1416	1	1	0	1	1	0	0	8.9108	8.9108	19.0319	0	PROCESSED	57602.3188194444	2016-08-02 07:39:06	55652	2011-04-01 00:00:00	55770.1098958333	2011-07-28 02:38:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806031010/	Quick Look
610	FORNAX CLUSTER NORTH	54.7043	-35.2294	54.224181	-35.391259	39.001136	-52.608154	236.34117402	-53.57224789	244.9993	53749.1506134259	2006-01-14 03:36:53	53750.3265509259	2006-01-15 07:50:14	800002030	45.575	80	45.583	45.579	45.575	45.587	2	2	2	2	1	0	0	42.5713	42.5713	101.6	1	PROCESSED	57532.6714236111	2016-05-24 16:06:51	54247	2007-05-27 00:00:00	54039.9702777778	2006-10-31 23:17:12	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001018	The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	0	SWG	MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800002030/	Quick Look
611	CIZASOUTHPE	340.7756	52.9173	340.257126	52.654896	13.355059	54.189252	104.17197619	-5.21572392	71.9989	56461.8747800926	2013-06-18 20:59:41	56464.2467361111	2013-06-21 05:55:18	808092010	92.9595	99	92.9675	92.9675	0	92.9595	2	2	0	2	1	0	0	96.3125	96.3125	204.9216	2	PROCESSED	57611.5762268518	2016-08-11 13:49:46	56848	2014-07-10 00:00:00	56481.818287037	2013-07-08 19:38:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081530	The Sausage Cluster is a violent merging galaxy cluster that offers unique opportunities to study the physics of particle acceleration and shocks in the ICM. We propose Suzaku observations of the southern part of the Sausage Cluster to (i) measure the Mach number of a merger related shock and (ii) determine the temperature distribution in the entire cluster outskirts. These observations will provide the first complete view of a system of merger-induced radio shocks and therefore play a crucial role in (1) understanding the impacts of such shocks on the evolution of galaxy clusters, (2) determining the physics of particle acceleration at low Mach number shocks, and (3) providing vital input for modeling the merger event in detail.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	REINOUT VAN WEEREN		USA	8	AO8	SHOCK AND AWE: PARTICLE ACCELERATION IN THE SAUSAGE CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808092010/	Quick Look
612	PLCK G214.6-37.0	137.1752	14.6923	136.484307	14.895327	135.215425	-1.654352	214.5759479	36.9399481	287	56413.2455439815	2013-05-01 05:53:35	56416.322349537	2013-05-04 07:44:11	808101010	119.2637	120	119.2637	119.2637	0	119.2637	2	2	0	2	1	0	0	106.3127	106.3127	265.8039	5	PROCESSED	57611.2793981482	2016-08-11 06:42:20	56795	2014-05-18 00:00:00	56429.7933217593	2013-05-17 19:02:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082007	We propose a detailed investigation of the nature of PLCK G214.6-37.0, discovered in the Planck survey. We aim at constraining the presence and properties of filamentary structures connecting and surrounding the clusters. We will unveil the overall dynamics of this complex structure and establish its detailed pressure distribution that can be used for a better estimation of YX to be compared with YSZ. Thus, we will perform a direct search for structures in between identified supercluster components from a careful comparison with the Planck results. Furthermore, the distribution of the PLCK G214.6-37.0 components suggest that it is evolving accreting sub-clusters along the filaments. That makes this supercluster one of the to search for the WHIM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	LORENZO LOVISARI		EUR	8	AO8	TRACKING DOWN THE PLANCK SUPERCLUSTER PLCK G214.6-37.0	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808101010/	Quick Look
613	ABELL 3364	86.9739	-32.0342	86.50731	-32.050049	85.482586	-55.428799	237.12200328	-26.63960547	295.0051	55671.5944444444	2011-04-20 14:16:00	55672.2917939815	2011-04-21 07:00:11	806067040	31.8869	29.5	31.8949	31.8949	0	31.8869	2	2	0	2	1	0	0	29.6154	29.6154	60.2459	0	PROCESSED	57601.5617939815	2016-08-01 13:28:59	56067	2012-05-20 00:00:00	55692.2490277778	2011-05-11 05:58:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061524	Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	6	AO6	THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806067040/	Quick Look
614	UGC03957 EAST	115.9739	55.4967	114.966906	55.616404	107.333122	33.607468	162.19834712	29.35111138	294.9944	56008.1335648148	2012-03-22 03:12:20	56009.1717476852	2012-03-23 04:07:19	806094010	46.6221	45	46.6221	46.6221	0	46.6221	2	2	0	2	1	0	0	45.2608	45.2608	89.6879	1	PROCESSED	57604.9930324074	2016-08-04 23:49:58	56434	2013-05-22 00:00:00	56068.628900463	2012-05-21 15:05:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062024	Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	BRENDA MIRANDA OCEJO		EUR	6	AO6	MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806094010/	Quick Look
615	A3528-S OFFSET 2	193.9782	-29.6501	193.300361	-29.379506	204.778966	-21.736125	304.09397791	33.21155179	289.0026	56501.5292476852	2013-07-28 12:42:07	56502.3981481482	2013-07-29 09:33:20	808105010	42.3	40	42.3	42.3078	0	42.316	2	2	0	2	1	0	0	42.5258	42.5258	75.0659	2	PROCESSED	57612.0639583333	2016-08-12 01:32:06	56955	2014-10-25 00:00:00	56587.7982523148	2013-10-22 19:09:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082018	We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	LORENZO LOVISARI		EUR	8	AO8	TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808105010/	Quick Look
616	A2104S	235.0317	-3.4139	234.377731	-3.253044	233.528717	15.709214	2.71321412	39.14413145	117.9978	54120.3324884259	2007-01-20 07:58:47	54120.8266087963	2007-01-20 19:50:19	801004010	17.3234	20	17.3234	17.3234	0	17.3234	2	2	0	2	1	0	0	13.8291	13.8291	42.6819	1	PROCESSED	57536.8854166667	2016-05-28 21:15:00	54750	2008-10-11 00:00:00	54137.3891898148	2007-02-06 09:20:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010012	We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO HATTORI		JAP	1	AO1	TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801004010/	Quick Look
617	IIZW108	318.5228	2.5728	317.890055	2.365228	321.781705	17.722745	53.56011975	-29.86052353	77.7227	53864.5319791667	2006-05-09 12:46:03	53864.7883680556	2006-05-09 18:55:15	801075010	11.6052	11	11.6052	11.6052	11.6052	11.6052	2	2	2	2	1	0	0	9.632	9.632	22.1499	1	PROCESSED	57534.2579398148	2016-05-26 06:11:26	54401	2007-10-28 00:00:00	53913.9958564815	2006-06-27 23:54:02	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801075010/	Quick Look
618	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
619	A3627SE	243.9338	-61.0124	242.844844	-60.887647	254.085676	-39.001294	325.27404641	-7.34625911	86.273	54869.3739236111	2009-02-07 08:58:27	54870.87875	2009-02-08 21:05:24	803033010	52.6995	50	52.7395	52.6995	0	52.7235	2	2	0	2	1	0	0	48.1839	48.1839	129.9878	3	PROCESSED	57545.4958912037	2016-06-06 11:54:05	55330	2010-05-14 00:00:00	54881.3769212963	2009-02-19 09:02:46	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030117	We propsoe to observe the cluster of galaxies A3627, which has evidences of cluster merging, in order to detect hard X-rays from high energy particles acceralated in the cluster and also measure the doppler shift of the iron-K line. This cluster is a nearby bright cluster behind the Galactic plane, and thus so far X-ray studies have been poor. However, its proximity and relatively low temperature against other merging clusters enable us to constrain the hard X-ray emission more tightly.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	SHO NISHINO		JAP	3	AO3	OBSERVATION OF MERGING CLUSTER A3627, LOCATED AROUND THE CENTER OF THE GREAT ATTRACTOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803033010/	Quick Look
620	A1631_C	193.2396	-15.343	192.582019	-15.071616	198.154189	-8.910152	303.4747971	47.52714603	112.9996	56304.4910069444	2013-01-12 11:47:03	56305.0106944444	2013-01-13 00:15:24	807004010	23.8057	20	23.8137	23.8057	0	23.8057	1	1	0	1	1	0	0	19.9369	19.9369	44.8719	0	PROCESSED	57608.4757986111	2016-08-08 11:25:09	56704	2014-02-16 00:00:00	56337.5260300926	2013-02-14 12:37:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070029	In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	7	AO7	PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807004010/	Quick Look
621	A548W	86.2487	-25.8437	85.742711	-25.86316	84.832695	-49.218426	230.35478522	-25.32458233	240.9996	56337.0028819444	2013-02-14 00:04:09	56339.3300462963	2013-02-16 07:55:16	807033010	99.3707	100	99.3707	99.3707	0	99.3707	2	2	0	2	1	0	0	85.3446	85.3446	201.0437	2	PROCESSED	57610.6626041667	2016-08-10 15:54:09	56738	2014-03-22 00:00:00	56372.6069444445	2013-03-21 14:34:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070085	Abell 548 west is a near-by (z=0.0424) poor cluster with an X-ray temperature of 3.4 keV. It has two bright radio relic emission located to the north (Feretti et al. 2006), and a candidate shock-front located near the relics (Solovyeva et al. 2008). The cluster X-ray luminosity is more than an order of magnitude dimmer when plotted in the kT-Lx relation. Combined with its too high galaxy velocity dispersion, we consider this target as a critical merger of two group-sized systems, which is a very rare case in our vicinity. Using Suzaku, we will parametrize the low surface brightness candidate shock region, to identify the temperature jump, which cannot be detected with XMM. We will also investigate the IC emission from the relics to measure the lower limit of its magnetic field.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KAZUHIRO NAKAZAWA		JAP	7	AO7	SUZAKU OBSERVATION OF A MERGING GROUP CANDIDATE ABELL 548 WEST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807033010/	Quick Look
622	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
623	3EGJ1234 1318_3	188.2697	-13.5708	187.619846	-13.295052	192.969415	-9.186347	296.11455637	49.05777767	113.9119	54445.0609375	2007-12-11 01:27:45	54445.8543171296	2007-12-11 20:30:13	802004010	1.602	30	1.602	29.7794	0	29.7794	1	2	0	2	1	0	0	26.3048	26.3048	68.5198	0	PROCESSED	57637.5213888889	2016-09-06 12:30:48	54999	2009-06-17 00:00:00	54633.6933217593	2008-06-16 16:38:23	3.0.22.44	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020007	We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ~ 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TOMONORI TOTANI		JAP	2	AO2	CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802004010/	Quick Look
624	3EGJ1234 1318_4	188.5214	-13.4715	187.871329	-13.195924	193.15662	-8.997759	296.47032219	49.18242085	113.9125	54445.8547453704	2007-12-11 20:30:50	54446.4655555556	2007-12-12 11:10:24	802005010	20.1392	20	0	20.1392	0	20.1552	0	2	0	2	1	0	0	20.0064	20.0064	52.7719	0	PROCESSED	57540.846875	2016-06-01 20:19:30	55000	2009-06-18 00:00:00	54633.6925347222	2008-06-16 16:37:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020007	We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ~ 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TOMONORI TOTANI		JAP	2	AO2	CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802005010/	Quick Look
625	ABELL 262 OFFSET2	28.0598	36.4356	27.324082	36.18913	39.413922	23.227924	136.37355079	-24.84408055	69.9996	54320.0778935185	2007-08-08 01:52:10	54321.2405555556	2007-08-09 05:46:24	802080010	54.7081	48	54.7241	54.7081	0	54.7241	2	2	0	2	1	0	0	50.1788	50.1788	100.3968	1	PROCESSED	57539.4536226852	2016-05-31 10:53:13	54730	2008-09-21 00:00:00	54347.6730671296	2007-09-04 16:09:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	023004	We propose to observe Abell 262. The temperature of the intracluster mediums of the cluster is 2 keV and therefore this cluster is between groups of galaxies and clusters of galaxies. The purpuse of the observation is to determine the distribution of O, Mg, Si and Fe f the intracluster medium upto 0.3 r180. The exposures are 30 ks for the central pointing and 40 ks for two offset pointings and the total exposure is 110ks.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	Fabio Gastaldello	JUS	2	AO2	O AND MG ABUNDANCES OF THE INTRACLUSTER MEDIUMS OF ABELL 262	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802080010/	Quick Look
626	A3627CENTER	243.5672	-60.8499	242.482666	-60.723566	253.815365	-38.883288	325.25917104	-7.10560665	129.9148	54905.9231597222	2009-03-15 22:09:21	54906.6072222222	2009-03-16 14:34:24	803032010	46.0339	50	46.0388	46.0419	0	46.0339	1	1	0	1	1	0	0	43.3969	43.3969	59.0959	0	PROCESSED	57545.823900463	2016-06-06 19:46:25	55330	2010-05-14 00:00:00	54917.2613657407	2009-03-27 06:16:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030117	We propsoe to observe the cluster of galaxies A3627, which has evidences of cluster merging, in order to detect hard X-rays from high energy particles acceralated in the cluster and also measure the doppler shift of the iron-K line. This cluster is a nearby bright cluster behind the Galactic plane, and thus so far X-ray studies have been poor. However, its proximity and relatively low temperature against other merging clusters enable us to constrain the hard X-ray emission more tightly.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	SHO NISHINO		JAP	3	AO3	OBSERVATION OF MERGING CLUSTER A3627, LOCATED AROUND THE CENTER OF THE GREAT ATTRACTOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803032010/	Quick Look
627	A3112SE	49.8254	-44.4068	49.393169	-44.587264	25.763903	-59.224971	253.09009544	-55.79916534	40.0009	56832.6869791667	2014-06-24 16:29:15	56834.034849537	2014-06-26 00:50:11	809026010	49.8443	45	49.8523	49.8443	0	49.8603	2	2	0	2	1	0	0	44.2246	44.2246	116.4418	0	PROCESSED	57615.347662037	2016-08-15 08:20:38	57212	2015-07-09 00:00:00	56846.5576273148	2014-07-08 13:22:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090061	We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KOSUKE SATO		JAP	9	AO9	ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809026010/	Quick Look
628	ZWCL 2341.1+0000	355.9117	0.3303	355.271077	0.05271	356.374003	1.928516	89.48591025	-58.06988626	66.2761	54644.6873148148	2008-06-27 16:29:44	54645.9258912037	2008-06-28 22:13:17	803001010	50.7413	40	50.7493	50.7413	0	50.7573	2	2	0	2	1	0	0	39.4767	39.4767	107.0018	0	PROCESSED	57542.9355671296	2016-06-03 22:27:13	55021	2009-07-09 00:00:00	54655.1925578704	2008-07-08 04:37:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030002	Recent advances in observational cosmology have revealed that the large-scale distribution of galaxies in the universe has a honeycomb-like structure. However it is still a mystery how such diverse structures emerge out of primeval density fluctuations that grew over time due to the effects of gravity. An important role in the structure-formation process is played by the large-scale shocks that form as the primordial density fluctuations become non-linear and the accretion flows on collapsing structures become supersonic. In order to understand cosmic-rays acceleration greater than 1000 TeV and the structure formation in the early universe, we propose a 40 ksec observation of the proto-cluster filament ZwCl 2341.1+0000 (z = 0.27) with Suzaku.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JUN KATAOKA		JAP	3	AO3	COSMIC-RAY ACCELERATION AND STRUCTURE FORMATION IN A MPC-SCALE FILAMENTARY NETWORK OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803001010/	Quick Look
629	A3112N	49.535	-43.9764	49.09877	-44.157944	25.831039	-58.74808	252.47008016	-56.12805661	40.0008	56831.1105439815	2014-06-23 02:39:11	56832.6863194444	2014-06-24 16:28:18	809027010	49.5323	45	49.5323	49.8923	0	49.8923	2	2	0	2	1	0	0	44.2405	44.2405	136.1356	2	PROCESSED	57615.3567476852	2016-08-15 08:33:43	57212	2015-07-09 00:00:00	56846.5678703704	2014-07-08 13:37:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090061	We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KOSUKE SATO		JAP	9	AO9	ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809027010/	Quick Look
630	PKS 0558-504 VIC 2	88.9376	-50.5474	88.635341	-50.553317	87.569877	-73.980493	257.96524127	-29.21937587	349.9999	56822.2473148148	2014-06-14 05:56:08	56824.093900463	2014-06-16 02:15:13	809035010	60.1523	60	60.1523	62.1728	0	62.1888	2	2	0	2	1	0	0	56.7476	56.7476	159.5318	2	PROCESSED	57615.2572800926	2016-08-15 06:10:29	57204	2015-07-01 00:00:00	56835.7714236111	2014-06-27 18:30:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090086	We have conducted joint analysis of absorption and emission lines toward several targets and successfully constrained temperatures, extents, and densities of the hot gas for each directions. The results are all consistent and indicate the disk-like hot gas with its height of a few kpc from the Galactic plane. However, other research group claimed that the hot gas extends to > 100 kpc and can be a reservoir of the missing baryon. We propose for an observation of the vicinities of PKS 0558-504 in order to limit an extent of the hot gas surrounding our Galaxy and to clinch an argument that the hot gas can be a huge reservoir of the missing baryon.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KAZUHIRO SAKAI		JAP	9	AO9	IS GALACTIC HOT GAS REALLY A HUGE RESERVOIR FOR THE MISSING BARYON?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809035010/	Quick Look
631	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
632	RXCJ0234.5-5830	38.6494	-58.5096	38.292773	-58.727647	354.405777	-65.806692	280.27566127	-53.84414378	249.7915	55212.1975115741	2010-01-16 04:44:25	55212.4794328704	2010-01-16 11:30:23	804003010	13.5665	10	13.5745	13.5665	0	13.5825	2	2	0	2	1	0	0	10.7771	10.7771	24.3559	0	PROCESSED	57550.1603125	2016-06-11 03:50:51	55594	2011-02-02 00:00:00	55228.0359722222	2010-02-01 00:51:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040005	We propose Suzaku observations of 8 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. With a total exposure time of 80 ksec, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	4	AO4	LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804003010/	Quick Look
633	NGC 6251	247.2266	82.6554	248.601394	82.760043	99.818913	73.103839	115.95247359	31.23340212	185.0319	55885.7751736111	2011-11-20 18:36:15	55887.7821875	2011-11-22 18:46:21	806015010	100.1571	100	100.1651	100.1571	0	100.1651	2	2	0	2	1	0	0	98.5943	98.5943	173.3759	1	PROCESSED	57603.983599537	2016-08-03 23:36:23	56264	2012-12-03 00:00:00	55897.1810300926	2011-12-02 04:20:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060045	Suzaku observations of lobes of Fanaroff-Riley Type-1 Radio Galaxies NGC 6251 and IC 4296 are proposed. Utilizing the high sensitivity for the diffuse sources of Suzaku, we propose precise measurement of the inverse-Compton X-rays form Fanaroff-Riley Type-1 Radio lobes to determine the electron energy density. Comparing the electron energy density with those of Fanaroff-Riley Type-2 Radio lobes, we examine an evolution model of the radio galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	HIROMI SETA		JAP	6	AO6	OBSERVATIONS OF LOBES OF FANAROFF-RILEY TYPE-1 RADIO GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806015010/	Quick Look
634	A1674_NE	196.3328	67.5805	195.880568	67.847887	143.656053	62.969177	120.89335151	49.49272287	327.6637	56799.3349189815	2014-05-22 08:02:17	56800.5487962963	2014-05-23 13:10:16	809042010	60.5303	40	0	60.5303	0	0	0	3	0	0	1	0	0	61.6512	61.6512	104.8597	2	PROCESSED	57615.1320023148	2016-08-15 03:10:05	57626	2016-08-26 00:00:00	56818.712650463	2014-06-10 17:06:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090114	A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KIYOSHI HAYASHIDA		JAP	9	AO9	HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809042010/	Quick Look
635	NGC 5044 SOUTH 30'	198.7482	-16.8629	198.081082	-16.598731	203.683963	-8.265963	311.00467544	45.63931299	110.0008	55222.2581365741	2010-01-26 06:11:43	55224.0190277778	2010-01-28 00:27:24	804014010	65.1766	60	65.1846	65.1766	0	65.1846	2	2	0	2	1	0	0	44.1628	44.1628	152.1218	1	PROCESSED	57550.4424768518	2016-06-11 10:37:10	55602	2011-02-10 00:00:00	55236.2169675926	2010-02-09 05:12:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040013	Why groups of galaxies contain smaller amount of metals than clusters of galaxies? To study metal sysnthesis history of galaxies in groups, we propose to observe two offset pointings of the NGC 5044 group and HCG 62 to derive metal distribution of intragroup medium up to 0.5 r180. Due to its low background, Suzaku enables us to study regions at low surface brightness.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KYOKO MATSUSHITA		JAP	4	AO4	METAL MASS TO LIGHT RATIOS OF GROUPS OF GALAXIES UP TO 0.5R180	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804014010/	Quick Look
636	A1674_Center	195.9709	67.5098	195.513873	67.777673	143.620899	62.81475	121.09709791	49.57408901	327.6687	56800.5493171296	2014-05-23 13:11:01	56801.6251736111	2014-05-24 15:00:15	809042020	56.0395	40	0	56.0395	0	0	0	2	0	0	1	0	0	56.0296	56.0296	92.9376	0	PROCESSED	57615.1546180556	2016-08-15 03:42:39	57626	2016-08-26 00:00:00	56862.7934837963	2014-07-24 19:02:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090114	A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KIYOSHI HAYASHIDA		JAP	9	AO9	HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809042020/	Quick Look
637	CIZASOUTHPW	340.5329	52.9469	340.016017	52.68489	13.195696	54.305912	104.05697228	-5.12002469	72.9252	56464.2477662037	2013-06-21 05:56:47	56466.5627777778	2013-06-23 13:30:24	808093010	98.4207	99	98.4287	98.4207	0	98.4287	2	2	0	2	1	0	0	99.1006	99.1006	200.0056	0	PROCESSED	57611.6015277778	2016-08-11 14:26:12	56848	2014-07-10 00:00:00	56481.8295486111	2013-07-08 19:54:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081530	The Sausage Cluster is a violent merging galaxy cluster that offers unique opportunities to study the physics of particle acceleration and shocks in the ICM. We propose Suzaku observations of the southern part of the Sausage Cluster to (i) measure the Mach number of a merger related shock and (ii) determine the temperature distribution in the entire cluster outskirts. These observations will provide the first complete view of a system of merger-induced radio shocks and therefore play a crucial role in (1) understanding the impacts of such shocks on the evolution of galaxy clusters, (2) determining the physics of particle acceleration at low Mach number shocks, and (3) providing vital input for modeling the merger event in detail.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	REINOUT VAN WEEREN		USA	8	AO8	SHOCK AND AWE: PARTICLE ACCELERATION IN THE SAUSAGE CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808093010/	Quick Look
638	A1674_Offset	196.9691	67.2995	196.521421	67.56601	144.467706	63.021341	120.47867852	49.75037622	328.362	56801.6258333333	2014-05-24 15:01:12	56802.7363541667	2014-05-25 17:40:21	809042030	67.4756	40	0	67.4756	0	0	0	2	0	0	1	0	0	63.4535	63.4535	95.9418	0	PROCESSED	57615.1567013889	2016-08-15 03:45:39	57626	2016-08-26 00:00:00	56818.7013541667	2014-06-10 16:49:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090114	A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KIYOSHI HAYASHIDA		JAP	9	AO9	HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809042030/	Quick Look
639	A1674_SW	195.6324	67.4673	195.171121	67.735617	143.543166	62.683089	121.29194244	49.62561755	325.0183	56802.7378472222	2014-05-25 17:42:30	56804.2224537037	2014-05-27 05:20:20	809042040	6.3772	40	6.3772	90.8498	0	6.3772	3	2	0	2	1	0	0	71.0768	71.0768	103.0788	1	PROCESSED	57615.185787037	2016-08-15 04:27:32	57626	2016-08-26 00:00:00	56818.7191203704	2014-06-10 17:15:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090114	A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KIYOSHI HAYASHIDA		JAP	9	AO9	HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809042040/	Quick Look
640	COMA RADIO RELIC	193.8629	27.2883	193.256096	27.558895	180.859214	30.350856	43.32885714	89.09337318	130.9989	54823.8794328704	2008-12-23 21:06:23	54829.0002777778	2008-12-29 00:00:24	803051010	205.062	140	205.07	205.07	0	205.062	2	2	0	2	1	0	0	170.6222	170.6222	442.3917	3	PROCESSED	57545.2371412037	2016-06-06 05:41:29	55218	2010-01-22 00:00:00	54851.5095949074	2009-01-20 12:13:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031431	We will observe the Coma cluster radio relic with the HXD/PIN to detect nonthermal Inverse Compton emission. This is the second brightest cluster radio relic known. The small PIN FOV will separate the Coma radio relic and halo. The PIN data will be a strong test of merger shock acceleration processes; a nondetection would be inconsistent with current theories. The data will allow the relic magnetic field, and nonthermal energy and pressure to be derived. The XIS observation of the relic will be used to detect the merger shock. The relic is associated with the merging NGC 4839 subgroup, which will also be observed. The 2 XIS observations will determine the dynamics of the merging subgroup. We will search for redshift differences between the Coma cluster, subgroup, and merger shock.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	CRAIG SARAZIN		USA	3	AO3	HARD X-RAY INVERSE COMPTON EMISSION FROM THE RADIO RELIC AND THE DYNAMICS OF THE MERGING SUBGROUP IN THE COMA CLUSTER	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803051010/	Quick Look
641	FG23	232.4567	44.1429	232.030206	44.313314	209.251166	59.914107	71.72776372	54.06523853	150.3369	57007.3108101852	2014-12-16 07:27:34	57008.1494791667	2014-12-17 03:35:15	809058010	38.4415	40	38.4415	38.4415	0	38.4415	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.5220601852	2016-08-17 12:31:46	57482	2016-04-04 00:00:00	57114.5765972222	2015-04-02 13:50:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091512	Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ELENA D'ONGHIA		USA	9	AO9	SCALING RELATIONS OF FOSSIL GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809058010/	Quick Look
642	THE MOON	135.7323	11.3866	135.051985	11.584787	134.824104	-5.224923	217.57839096	34.30376044	284.6998	56783.949849537	2014-05-06 22:47:47	56784.073125	2014-05-07 01:45:18	809001040	5.5556	45	5.5556	5.5714	0	5.5636	1	1	0	1	1	0	0	4.574	4.574	10.6479	0	PROCESSED	57615.0559606482	2016-08-15 01:20:35	57162	2015-05-20 00:00:00	56796.5928240741	2014-05-19 14:13:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001040/	Quick Look
643	CENTAURUS SE4	192.8602	-42.5262	192.164471	-42.254349	210.265844	-33.700282	302.93248329	20.34554874	294.0685	56854.4082407407	2014-07-16 09:47:52	56854.9480092593	2014-07-16 22:45:08	809068010	20.659	20	20.659	20.659	0	20.659	1	1	0	1	1	0	0	10.395	10.395	22.0319	0	PROCESSED	57615.3959606482	2016-08-15 09:30:11	57250	2015-08-16 00:00:00	56883.1729050926	2014-08-14 04:08:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091522	We propose here to observe the outskirts of the X-ray bright, nearby Centaurus cluster with good azimuthal coverage by adding 3 new arms with total exposure 204ks. This will extend our initial analysis in one direction to the north-west which has allowed our team to obtain high spatial resolution profiles of temperature, density and entropy. The XMM temperature map of the central 30 arcmins shows a complex temperature environment and deviations from spherical symmetry, and good azimuthal coverage is important to obtain an accurate understanding of the outskirts.Observations of the Perseus cluster have shown significant azimuthal variations in the ICM temperature and entropy. Centaurus is the best target for understanding the ICM in the outskirts of a relaxed, intermediate mass cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	CHRISTOPHER REYNOLDS		USA	9	AO9	OBSERVATIONS OF THE X-RAY BRIGHT, NEARBY CENTAURUS CLUSTER TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809068010/	Quick Look
644	RCS1102-0319	165.6362	-3.316	164.999495	-3.046688	168.075129	-8.718258	257.90567893	49.79184665	114.0911	54817.3259259259	2008-12-17 07:49:20	54817.9773611111	2008-12-17 23:27:24	803065010	26.3811	21	26.3811	26.3811	0	26.3811	2	2	0	2	1	0	0	13.9089	13.9089	56.27	0	PROCESSED	57544.9757407407	2016-06-05 23:25:04	55206	2010-01-10 00:00:00	54840.2609143518	2009-01-09 06:15:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031441	Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	3	AO3	COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803065010/	Quick Look
645	M87N FAINT	187.6988	12.9392	187.066448	13.215269	181.818448	14.91295	283.11850774	75.01113844	297.6812	54625.626400463	2008-06-08 15:02:01	54627.068275463	2008-06-10 01:38:19	803069010	65.2474	60	65.2474	65.2714	0	65.2554	2	2	0	2	1	0	0	57.9068	57.9068	124.5638	0	PROCESSED	57542.7828587963	2016-06-03 18:47:19	55009	2009-06-27 00:00:00	54642.2950694444	2008-06-25 07:04:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032011	We propose to take advantage of Suzaku's low background and good collecting area to observe a strong surface brightness discontinuity, most likely a cold front, in the outskirts of M87. We will make accurate temperature and pressure profiles across this cold front, determine the energy associated with it, and compare this to the energy of known AGN-ICM interaction features in M87. With Suzaku's superior spectral redistribution function we will for the first time measure Mg and O in the M87 outskirts and improve constraints on relative contributions by SNIa and SNII. We will study abundance and abundance-ratio variations across the cold front and determine the role of gas sloshing in transporting metals produced by the central galaxy into the ICM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		EUR	3	AO3	THE ENERGETICS AND METAL ABUNDANCE PATTERNS IN THE OUTSKIRTS OF M87	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803069010/	Quick Look
646	THE MOON	137.1548	11.8786	136.473781	12.081578	136.019585	-4.350943	217.75615417	35.77416951	105.7184	56975.0809490741	2014-11-14 01:56:34	56975.1987615741	2014-11-14 04:46:13	809001190	6.413	45	6.413	6.413	0	6.413	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.77	2016-08-16 18:28:48	57358	2015-12-02 00:00:00	56992.4097916667	2014-12-01 09:50:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001190/	Quick Look
647	RXCJ2157.4-0747 NE	329.3742	-7.8003	328.713545	-8.039068	328.756448	4.373785	49.81973283	-44.55901105	250.0004	56972.5422453704	2014-11-11 13:00:50	56973.0835069445	2014-11-12 02:00:15	809021010	18.63	20	18.646	18.63	0	18.646	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.764375	2016-08-16 18:20:42	57352	2015-11-26 00:00:00	56986.4078240741	2014-11-25 09:47:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090049	About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	9	AO9	PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809021010/	Quick Look
648	ABELL 98-NORTH	11.5751	20.8392	10.913914	20.566164	18.902329	14.584822	121.31617836	-42.01643069	67.4405	56841.1634490741	2014-07-03 03:55:22	56841.958599537	2014-07-03 23:00:23	809078020	23.888	100	24.68	23.888	0	24.9396	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.3618865741	2016-08-15 08:41:07	56748	2014-04-01 00:00:00	56875.6040393518	2014-08-06 14:29:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091525	We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	SCOTT RANDALL		USA	9	AO9	EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809078020/	Quick Look
649	A2029_2	227.8527	6.0108	227.233944	6.198717	223.562452	22.914786	6.92100367	50.6092725	112.9534	55224.3333912037	2010-01-28 08:00:05	55224.9794444444	2010-01-28 23:30:24	804024020	26.0185	22	26.0225	26.0185	0	26.0262	2	2	0	2	1	0	0	15.9033	15.9033	55.814	0	PROCESSED	57550.4048726852	2016-06-11 09:43:01	55637	2011-03-17 00:00:00	55271.0156365741	2010-03-16 00:22:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040030	Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUZURU TAWARA		JAP	4	AO4	TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024020/	Quick Look
650	A1246_CENTER	170.9992	21.4865	170.340675	21.761183	163.096496	16.147963	224.00399917	69.32667171	120.0006	55151.2043981482	2009-11-16 04:54:20	55152.274525463	2009-11-17 06:35:19	804028010	48.4564	40	48.4724	48.4564	0	48.4724	2	2	0	2	1	0	0	37.2156	37.2156	92.4339	0	PROCESSED	57549.4081018518	2016-06-10 09:47:40	55531	2010-12-01 00:00:00	55162.1616319445	2009-11-27 03:52:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040053	We propose 40 and 80 ksec observations of the central and offset regions of Abell 1246, respectively, to study the temperature and mass profiles out to the virial radius. This cluster is moderately distant (z=0.1902), and relaxed system (kT=5.7 keV), with a diameter of about 20'. The low background of the XIS instrument will enable us to observe the region around the virial radius. The dentity and temperature of ICM around the virial radius should directly reflect the process of gas infall and heating. The correct temperature curve is also vital to determine the gravitational mass distribution.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KOSUKE SATO		JAP	4	AO4	MASS AND TEMPERATURE PROFILES OF THE RELAXED CLUSTER A1246	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804028010/	Quick Look
651	FG34	359.5671	15.0896	358.927387	14.811234	5.724886	13.991032	104.34552863	-45.85455759	250.6856	56999.6725115741	2014-12-08 16:08:25	57000.6669328704	2014-12-09 16:00:23	809060010	38.5062	40	38.5062	38.5062	0	38.5062	2	2	0	2	1	0	0	35.0584	35.0584	85.8958	1	PROCESSED	57617.4968634259	2016-08-17 11:55:29	57377	2015-12-21 00:00:00	57010.1825925926	2014-12-19 04:22:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091512	Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ELENA D'ONGHIA		USA	9	AO9	SCALING RELATIONS OF FOSSIL GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809060010/	Quick Look
652	A1246_OFF	171.128	21.4191	170.469781	21.693883	163.239064	16.135503	224.30142226	69.41574013	120.0005	55163.0212152778	2009-11-28 00:30:33	55164.9606365741	2009-11-29 23:03:19	804029010	80.3804	80	80.3964	80.3804	0	80.391	2	2	0	2	1	0	0	55.158	55.158	167.5558	1	PROCESSED	57549.6578472222	2016-06-10 15:47:18	55549	2010-12-19 00:00:00	55181.239849537	2009-12-16 05:45:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040053	We propose 40 and 80 ksec observations of the central and offset regions of Abell 1246, respectively, to study the temperature and mass profiles out to the virial radius. This cluster is moderately distant (z=0.1902), and relaxed system (kT=5.7 keV), with a diameter of about 20'. The low background of the XIS instrument will enable us to observe the region around the virial radius. The dentity and temperature of ICM around the virial radius should directly reflect the process of gas infall and heating. The correct temperature curve is also vital to determine the gravitational mass distribution.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KOSUKE SATO		JAP	4	AO4	MASS AND TEMPERATURE PROFILES OF THE RELAXED CLUSTER A1246	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804029010/	Quick Look
653	ABELL 2877	17.5065	-45.9303	16.951425	-46.196287	351.939456	-47.942764	293.04607396	-70.83949903	47.4208	56809.9110532407	2014-06-01 21:51:55	56810.1181712963	2014-06-02 02:50:10	809100010	11.908	10	11.916	11.908	0	11.9306	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.1778240741	2016-08-15 04:16:04	57197	2015-06-24 00:00:00	56828.5915856482	2014-06-20 14:11:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809100010/	Quick Look
654	AWM7 45' EAST	44.4244	41.5971	43.612656	41.396941	54.340636	23.633961	146.87973673	-15.32937684	74.1373	55780.4446527778	2011-08-07 10:40:18	55781.3155208333	2011-08-08 07:34:21	806008010	36.8794	35	36.8794	36.8794	0	36.8794	1	1	0	1	1	0	0	35.7039	35.7039	75.2399	0	PROCESSED	57602.7523726852	2016-08-02 18:03:25	56169	2012-08-30 00:00:00	55802.4637384259	2011-08-29 11:07:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060029	X-ray observations of cluster outskirts give us valuable information about star formation and metal enrichment histories in clusters. Here, we propose to observe three fields with total exposures of 100 ks, 45' east, 27' and 45' south from the center. With these observations, we will compare distributions of Fe and galaxies up to 0.6r180, and study metal-enrichment history in filaments of large-scale structure.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA		JAP	6	AO6	DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM OF AWM7 CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806008010/	Quick Look
655	ABELL 2667	357.8478	-26.2362	357.201143	-26.514394	347.004245	-23.092849	33.32905605	-76.56526922	64.8822	55724.4201273148	2011-06-12 10:04:59	55725.7009490741	2011-06-13 16:49:22	806029030	52.2862	50	52.3022	52.2862	0	52.3102	1	1	0	1	1	0	0	42.9697	42.9697	110.6559	1	PROCESSED	57602.2711574074	2016-08-02 06:30:28	55652	2011-04-01 00:00:00	55757.6986458333	2011-07-15 16:46:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806029030/	Quick Look
656	COMA E3.5	195.93	27.9076	195.329276	28.17566	182.445576	31.726119	49.60850486	87.16763542	128.002	55917.6227314815	2011-12-22 14:56:44	55917.9487384259	2011-12-22 22:46:11	806032020	14.769	15	14.777	14.785	0	14.769	1	1	0	1	1	0	0	9.6169	9.6169	28.1599	1	PROCESSED	57604.2057175926	2016-08-04 04:56:14	55652	2011-04-01 00:00:00	55937.7819444444	2012-01-11 18:46:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806032020/	Quick Look
657	COMA E7	197.1143	27.885	196.516478	28.15145	183.559395	32.176347	45.24852034	86.15126123	280.0002	55732.0582291667	2011-06-20 01:23:51	55732.4446990741	2011-06-20 10:40:22	806038010	15.1175	15	15.1335	15.1175	0	15.1415	1	1	0	1	1	0	0	16.3295	16.3295	33.3039	0	PROCESSED	57602.3596643518	2016-08-02 08:37:55	55652	2011-04-01 00:00:00	55770.1779398148	2011-07-28 04:16:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806038010/	Quick Look
658	COMA NW1	194.8094	28.1686	194.206284	28.438076	181.270608	31.513632	64.44263169	87.98368038	319.9994	55732.4516550926	2011-06-20 10:50:23	55732.6453935185	2011-06-20 15:29:22	806039010	9.633	10	9.633	9.633	0	9.633	1	1	0	1	1	0	0	8.038	8.038	16.7279	0	PROCESSED	57602.3588310185	2016-08-02 08:36:43	55652	2011-04-01 00:00:00	55768.2335416667	2011-07-26 05:36:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806039010/	Quick Look
659	COMA NW5.5	194.2342	29.281	193.631324	29.551161	180.146914	32.276161	93.88493667	87.52983745	319.9944	55734.0685763889	2011-06-22 01:38:45	55734.4155439815	2011-06-22 09:58:23	806043010	15.6631	15	15.6631	15.6631	0	15.6631	2	2	0	2	1	0	0	16.384	16.384	29.9559	1	PROCESSED	57602.3741203704	2016-08-02 08:58:44	55652	2011-04-01 00:00:00	55768.2836458333	2011-07-26 06:48:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806043010/	Quick Look
660	SPT-CL J2337-5942	354.3472	-59.706	353.656399	-59.982964	322.211454	-50.57498	319.15808948	-55.0279039	35.9387	55674.1154282407	2011-04-23 02:46:13	55674.9342592593	2011-04-23 22:25:20	806073010	38.8415	35	38.8415	38.8415	0	38.8415	2	2	0	2	1	0	0	33.8423	33.8423	70.74	0	PROCESSED	57601.5793402778	2016-08-01 13:54:15	56067	2012-05-20 00:00:00	55692.2710069445	2011-05-11 06:30:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061531	We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ERIC MILLER		USA	6	AO6	THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806073010/	Quick Look
661	ABELL 3364	86.8402	-31.7251	86.371508	-31.741602	85.303796	-55.115651	236.7542178	-26.65907095	295.0034	55669.7134722222	2011-04-18 17:07:24	55670.3585416667	2011-04-19 08:36:18	806067010	30.0737	29.5	30.0897	30.0737	0	30.0897	2	2	0	2	1	0	0	28.5437	28.5437	55.7279	1	PROCESSED	57601.535787037	2016-08-01 12:51:32	56067	2012-05-20 00:00:00	55691.1662962963	2011-05-10 03:59:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061524	Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	6	AO6	THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806067010/	Quick Look
662	SPT-CL J0546-5345	86.64	-53.7518	86.378624	-53.768776	81.098351	-77.090454	261.46331102	-30.97881567	53.9016	55781.3261805556	2011-08-08 07:49:42	55782.8335763889	2011-08-09 20:00:21	806071010	99.7366	110	99.7366	99.7366	0	99.7366	2	2	0	2	1	0	0	78.9114	78.9114	130.2079	3	PROCESSED	57602.7921180556	2016-08-02 19:00:39	56169	2012-08-30 00:00:00	55802.4644907407	2011-08-29 11:08:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061531	We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ERIC MILLER		USA	6	AO6	THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806071010/	Quick Look
663	A1750N	202.8147	-1.6537	202.171177	-1.396479	201.71761	7.336429	322.93839507	59.66232121	293.5219	55744.8544444444	2011-07-02 20:30:24	55746.9911111111	2011-07-04 23:47:12	806096010	74.7134	80	74.7294	74.7134	0	74.7294	2	2	0	2	1	0	0	61.6402	61.6402	184.5979	1	PROCESSED	57602.5091435185	2016-08-02 12:13:10	56144	2012-08-05 00:00:00	55775.4134027778	2011-08-02 09:55:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	063019	We observe Abell 1750 which has three clusters of galaxies in a filamentary structure of the large-scale structure, with 4 pointing observations (80 x 3 + 40 ks). We reveal global spatial structures of temperature, density, and entropy in Abell 1750 for the first time. By a correlation with a galaxy map obtained from SDSS, and a comparison between thermal pressure and total pressure required by the total mass derived from weal lensing analysis, we explore the inflow of matter and evolutionary process in this system.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA	SCOTT RANDALL	JUS	6	AO6	SUZAKU OBSERVATION OF ABELL 1750 IN THE LARGE-SCALE STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806096010/	Quick Look
664	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
665	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
666	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
667	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
668	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
669	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
670	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
671	NGC 7796	359.7407	-55.4558	359.095869	-55.734273	329.790591	-49.001607	317.90399943	-60.12089491	60.4505	56078.2927430556	2012-05-31 07:01:33	56080.5001851852	2012-06-02 12:00:16	807047010	161.6136	150	161.6216	161.6216	0	161.6136	2	2	0	2	1	0	0	134.0432	134.0432	190.7118	0	PROCESSED	57605.6269328704	2016-08-05 15:02:47	56018	2012-04-01 00:00:00	56090.2424537037	2012-06-12 05:49:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071503	The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DAVID BUOTE		USA	7	AO7	THE MASS PROFILES OF ISOLATED ELLIPTICAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807047010/	Quick Look
672	A3376 EAST	90.8243	-39.9606	90.417011	-39.957602	91.41993	-63.398251	246.56739968	-25.79165375	80.8001	56549.3239699074	2013-09-14 07:46:31	56551.6953472222	2013-09-16 16:41:18	808028010	81.5734	81	81.5734	81.5734	0	81.5734	2	2	0	2	1	0	0	75.1814	75.1814	204.8578	2	PROCESSED	57612.6739467593	2016-08-12 16:10:29	56956	2014-10-26 00:00:00	56588.6883449074	2013-10-23 16:31:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080037	Abell 3376 (z=0.046) is a peculiar merging cluster with giant double radio relics. High sensitivity of the XIS will enable us (i) to determine the temperature and density distributions around the shock accompanying the east relic, and (ii) to examine how thermal and non-thermal energies separate and go into the respective particles. Wide coverage will allow us to compare the ICM properties along the shock and non-shock directions. The low redshift of the source will allow XIS data to resolve detailed shock-related structures.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKAYA OHASHI		JAP	8	AO8	SUZAKU OBSERVATION OF THE EAST MERGER SHOCK AND RADIO RELIC IN ABELL 3376	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808028010/	Quick Look
673	FG27	243.6269	26.7212	243.111772	26.845958	234.444811	46.957031	44.57695273	45.05698279	293.3995	56144.3018055556	2012-08-05 07:14:36	56144.5557638889	2012-08-05 13:20:18	807056010	11.2194	15	11.235	11.2194	0	11.235	1	1	0	1	1	0	0	10.9114	10.9114	21.9359	1	PROCESSED	57606.7546643518	2016-08-06 18:06:43	56533	2013-08-29 00:00:00	56167.1527893518	2012-08-28 03:40:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071511	Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ELENA D'ONGHIA		USA	7	AO7	SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807056010/	Quick Look
674	SDSS J0837+4414	129.4975	44.2566	128.645697	44.432041	120.139652	24.860483	176.37698799	37.1577345	110.1912	56213.8277083333	2012-10-13 19:51:54	56214.3515393518	2012-10-14 08:26:13	807061010	20.6219	20	20.6219	20.6219	0	20.6219	1	1	0	1	1	0	0	20.958	20.958	45.2399	0	PROCESSED	57607.7583796296	2016-08-07 18:12:04	56598	2013-11-02 00:00:00	56232.4985185185	2012-11-01 11:57:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071512	Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ERIC MILLER		USA	7	AO7	FINDING FOSSIL GROUPS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807061010/	Quick Look
675	HYDRA A OUT	139.8502	-12.6235	139.249709	-12.411636	146.680072	-26.793484	243.60142222	25.01758475	300.0034	56085.1461574074	2012-06-07 03:30:28	56085.6667824074	2012-06-07 16:00:10	807091010	20.3276	20	20.3516	20.3436	0	20.3276	2	2	0	2	1	0	0	16.5403	16.5403	44.9779	0	PROCESSED	57605.607349537	2016-08-05 14:34:35	56491	2013-07-18 00:00:00	56120.2321296296	2012-07-12 05:34:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072020	Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DOMINIQUE ECKERT		EUR	7	AO7	MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807091010/	Quick Look
676	G171.9-40.7	48.2433	8.3685	47.57264	8.181881	48.126521	-9.211403	171.97024112	-40.65556769	252.8031	56320.012025463	2013-01-28 00:17:19	56322.7126967593	2013-01-30 17:06:17	807092010	100.9825	100	100.9905	100.9825	0	100.9848	2	2	0	2	1	0	0	93.1617	93.1617	233.2957	0	PROCESSED	57608.6871527778	2016-08-08 16:29:30	56749	2014-04-02 00:00:00	56365.6023263889	2013-03-14 14:27:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072021	We propose to observe 4 galaxy clusters from the first all-sky blind Sunyaev Zeldovich (SZ) effect cluster catalogue produced by the Planck satellite. This catalogue has revealed a new population of clusters previously undetected by X-ray surveys. The Planck SZ selected cluster sample consists of hot, massive, morphologically disturbed clusters that are under-luminous in the soft X-ray band. This exciting population has implications not only for understanding the thermodynamic state of the intracluster medium, but also for cluster cosmology where it represents an important area of phase space in the cluster mass function; it is a pointer to the dynamics of how clusters form through mergers, and to the true spatial density of cluster-mass structures not represented in X-ray surveys.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ANNA SCAIFE		EUR	7	AO7	CONSTRAINING THE THERMODYNAMIC STATE OF NEW PLANCK GALAXY CLUSTERS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807092010/	Quick Look
677	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
678	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
679	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
680	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
681	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
682	A2199_NE	247.516	39.7841	247.089512	39.891486	233.470249	60.402163	63.26645529	43.42583068	143.5992	56661.6024074074	2014-01-04 14:27:28	56662.5572222222	2014-01-05 13:22:24	808050010	44.1631	40	44.1711	44.1631	0	44.1711	2	2	0	2	1	0	0	42.3531	42.3531	82.4919	1	PROCESSED	57613.7484953704	2016-08-13 17:57:50	57079	2015-02-26 00:00:00	56713.7287037037	2014-02-25 17:29:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080067	We propose to complete pointing observations to cover the entire region of Abell 2199 cluster. Suzaku has performed 21 pointing observations of Abell 2199 cluster (z=0.03), showing remarkable features in the temperature and entropy distributions with high physical resolution, as ``Suzaku AO-6 keyproject'' we proposed. Our target is the only cluster to cover the whole region, achieved solely by Suzaku/XIS among currently available facilities. Therefore, this project can provide us an exquisite, complete information of the cluster gas with the high physical resolution, which would be used as unsurpassed, legacy-type dataset in the X-ray cluster community.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KOSUKE SATO		JAP	8	AO8	COMPLETING THE SUZAKU LEGACY MOSAIC OF ABELL 2199 CLUSTER TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808050010/	Quick Look
683	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
684	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
685	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
686	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
687	ABELL 85 S2	10.6249	-9.681	9.992851	-9.954936	5.880188	-13.097469	115.61862408	-72.42570917	230.5003	56295.6322106482	2013-01-03 15:10:23	56296.8696064815	2013-01-04 20:52:14	807136010	53.603	50	53.611	53.611	0	53.603	2	2	0	2	1	0	0	51.8426	51.8426	106.8957	2	PROCESSED	57608.4325347222	2016-08-08 10:22:51	56702	2014-02-14 00:00:00	56336.5803240741	2013-02-13 13:55:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071791	We propose exposures with CHandra and Suzaku in Abell 85 to trace the impact of a galaxy group merging with a galaxy cluster at multiple scales. Existing observations of Abell 85 reveal an infalling galaxy group ~300 kpc to the south of the main cluster moving supersonically through the ICM. Stripped gas is observed trailing behind this group to distances of 2 Mpc. We will investigate interactions between this group and the main cluster by observing the shocks associated with the group's motion and the properties of stripped gas. We will be able to measure the properties of the stripped gas from the group's current location out to the virial radius by combining the data from both telescopes. These observations will provide key insights into how the largest structures form.	EXTRAGALACTIC DIFFUSE SOURCES	8	S	STEVEN ALLEN		USA	7	AO7	TRACING A MERGER FROM START TO FINISH IN ABELL 85	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807136010/	Quick Look
688	SHAPLEY B	201.6375	-31.8605	200.934316	-31.601045	212.201419	-21.080247	311.5766773	30.42117615	110.7883	56315.4877893518	2013-01-23 11:42:25	56316.3245138889	2013-01-24 07:47:18	807137010	30.5052	30	30.5132	30.5052	0	30.5203	2	2	0	2	1	0	0	26.1395	26.1395	72.2919	2	PROCESSED	57608.5939814815	2016-08-08 14:15:20	56709	2014-02-21 00:00:00	56342.5463888889	2013-02-19 13:06:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071848	29% of the baryon density measured at high redshift are unaccounted for at the present epoch. Since a persistent deficit would challenge our current understanding of the thermodynamics of structure formation and the effects of shocks and galactic outflows on the surrounding gas, resolving this deficit is critical for understanding low-redshift cosmology and galaxy formation. Simulations suggest these baryons emit soft X-rays and should reside along low density filaments in the cosmic web, the WHIM. We propose to combine Chandra ACIS-I with Suzaku XIS observations for 3 large scale filaments in the Shapley Supercluster, the largest overdensity of galaxies and clusters in the z<0.1 Universe, to identify galaxy groups in these filaments and search for X-ray emission from the WHIM.	EXTRAGALACTIC DIFFUSE SOURCES	8	S	MARIE MACHACEK		USA	7	AO7	MAPPING GALAXY GROUPS AND THE HOT WHIM IN SHAPLEY SUPERCLUSTER FILAMENTS WITH CHANDRA AND SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807137010/	Quick Look
689	SHAPLEY C	202.085	-31.0332	201.382602	-30.774544	212.227549	-20.169518	312.17140577	31.17563268	109.0374	56330.7851273148	2013-02-07 18:50:35	56331.4147453704	2013-02-08 09:57:14	807138010	30.8744	30	30.8904	30.8744	0	30.8904	2	2	0	2	1	0	0	31.966	31.966	54.392	0	PROCESSED	57610.5475694444	2016-08-10 13:08:30	56715	2014-02-27 00:00:00	56349.523287037	2013-02-26 12:33:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071848	29% of the baryon density measured at high redshift are unaccounted for at the present epoch. Since a persistent deficit would challenge our current understanding of the thermodynamics of structure formation and the effects of shocks and galactic outflows on the surrounding gas, resolving this deficit is critical for understanding low-redshift cosmology and galaxy formation. Simulations suggest these baryons emit soft X-rays and should reside along low density filaments in the cosmic web, the WHIM. We propose to combine Chandra ACIS-I with Suzaku XIS observations for 3 large scale filaments in the Shapley Supercluster, the largest overdensity of galaxies and clusters in the z<0.1 Universe, to identify galaxy groups in these filaments and search for X-ray emission from the WHIM.	EXTRAGALACTIC DIFFUSE SOURCES	8	S	MARIE MACHACEK		USA	7	AO7	MAPPING GALAXY GROUPS AND THE HOT WHIM IN SHAPLEY SUPERCLUSTER FILAMENTS WITH CHANDRA AND SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807138010/	Quick Look
690	A3627_WEST	243.1701	-60.6984	242.089882	-60.570358	253.528582	-38.78018	325.22376786	-6.86207305	306.0002	56546.5563425926	2013-09-11 13:21:08	56547.2535185185	2013-09-12 06:05:04	808059010	52.7998	50	52.7998	52.8237	0	52.8078	2	2	0	2	1	0	0	42.8968	42.8968	60.2319	0	PROCESSED	57612.5956481482	2016-08-12 14:17:44	56956	2014-10-26 00:00:00	56588.7134837963	2013-10-23 17:07:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080097	We propose to observe the north-west region in nearby merging cluster Abell 3627. Suzaku observation in AO-3 found a subcluster colliding into the main body from the south-east direction and a hard X-ray component above 12 keV probably originated from the north-west region. The region has also peculiar structures such as long X-ray/radio tails, suggesting a relation with the cluster merging. In order to understand the process of cluster merging taking into accout the hard X-ray component and these peculiar structures, we will measure the temperature and pressure distributions in the north-west region using the low background of XIS. We will also study the non-thermal emission using HXD and investigate a possibililty of the particle acceleration in Abell 3627.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KATSUHIRO HAYASHI		JAP	8	AO8	OBSERVATION OF THE NORTH-WEST REGION IN NEARBY MERGING CLUSTER ABELL 3627	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808059010/	Quick Look
691	FJ1336+3553_OFFSET	203.9396	35.8517	203.380018	36.106643	185.299819	41.923502	78.4395295	77.15761363	299.9998	56836.6568171296	2014-06-28 15:45:49	56837.6530092593	2014-06-29 15:40:20	809041010	43.307	45	43.307	45.5019	0	45.5179	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.3386458333	2016-08-15 08:07:39	57212	2015-07-09 00:00:00	56846.5938425926	2014-07-08 14:15:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090090	Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	IKUYUKI MITSUISHI		JAP	9	AO9	EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809041010/	Quick Look
692	A3528-S OFFSET 4	194.1847	-30.0435	193.505704	-29.773143	205.130736	-22.019409	304.29690153	32.8141993	288.9992	56503.6527199074	2013-07-30 15:39:55	56504.4071064815	2013-07-31 09:46:14	808107010	32.7752	30	32.7832	32.7752	0	32.7912	3	2	0	2	1	0	0	31.2585	31.2585	65.1599	0	PROCESSED	57612.0918634259	2016-08-12 02:12:17	56955	2014-10-25 00:00:00	56587.7238310185	2013-10-22 17:22:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082018	We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	8	AO8	TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808107010/	Quick Look
693	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
694	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
695	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
696	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
697	CEN_A_LOBE_N5	198.8206	-42.0777	198.100689	-41.813564	214.682372	-31.301214	307.6547721	20.57528449	295.9847	56865.6873032407	2014-07-27 16:29:43	56867.2502430556	2014-07-29 06:00:21	809006010	51.9392	50	51.9392	52.5746	0	52.5746	2	2	0	2	1	0	0	10.6586	10.6586	20.936	0	PROCESSED	57615.4722916667	2016-08-15 11:20:06	57267	2015-09-02 00:00:00	56898.3358449074	2014-08-29 08:03:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090021	In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROMI SETA		JAP	9	AO9	MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809006010/	Quick Look
698	THE MOON	134.2483	11.6812	133.56589	11.874254	133.339832	-5.352995	216.51758385	33.11115118	281.9606	56783.8139699074	2014-05-06 19:32:07	56783.948125	2014-05-06 22:45:18	809001030	6.4899	45	6.4979	6.4899	0	6.4979	1	1	0	1	1	0	0	7.02	7.02	11.5839	0	PROCESSED	57615.0497222222	2016-08-15 01:11:36	57162	2015-05-20 00:00:00	56793.5289930556	2014-05-16 12:41:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001030/	Quick Look
699	THE MOON	140.1926	10.5514	139.518228	10.7642	139.270066	-4.724239	220.86178985	37.88683751	291.2213	56784.325775463	2014-05-07 07:49:07	56784.4480555556	2014-05-07 10:45:12	809001070	6.405	45	6.405	6.405	0	6.405	2	2	0	2	1	0	0	6.677	6.677	10.5539	0	PROCESSED	57615.0674074074	2016-08-15 01:37:04	57218	2015-07-15 00:00:00	56852.581875	2014-07-14 13:57:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001070/	Quick Look
700	RXCJ2157.4-0747 SE	329.2877	-7.568	328.627588	-7.806552	328.755658	4.621414	50.03773919	-44.36639016	250.0002	56973.0839351852	2014-11-12 02:00:52	56973.6668055556	2014-11-12 16:00:12	809022010	25.9584	20	25.9744	25.9584	0	25.9824	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7636111111	2016-08-16 18:19:36	57352	2015-11-26 00:00:00	56986.4089351852	2014-11-25 09:48:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090049	About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	9	AO9	PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809022010/	Quick Look
701	RXCJ2157.4-0747 SW	329.5619	-7.7328	328.901524	-7.972036	328.954889	4.373264	50.03497203	-44.68420804	250.0004	56976.2027893518	2014-11-15 04:52:01	56976.7307175926	2014-11-15 17:32:14	809023010	20.9188	20	20.9188	20.9188	0	20.9188	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.786099537	2016-08-16 18:51:59	57361	2015-12-05 00:00:00	56993.4286921296	2014-12-02 10:17:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090049	About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	9	AO9	PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809023010/	Quick Look
702	A3112E	49.9177	-44.1055	49.483567	-44.285626	26.168536	-58.996914	252.54334877	-55.82694751	25.0007	56829.3656134259	2014-06-21 08:46:29	56830.3266435185	2014-06-22 07:50:22	809024010	33.435	45	33.435	34.195	0	34.219	2	2	0	2	1	0	0	30.293	30.293	82.9918	1	PROCESSED	57615.3104398148	2016-08-15 07:27:02	57239	2015-08-05 00:00:00	56873.1925	2014-08-04 04:37:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090061	We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KOSUKE SATO		JAP	9	AO9	ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809024010/	Quick Look
703	NGC 891	35.645	42.3416	34.858537	42.114299	47.830156	26.528514	140.39047988	-17.41940889	243.1772	57072.5035300926	2015-02-19 12:05:05	57073.2222916667	2015-02-20 05:20:06	809054010	28.8738	100	28.8738	28.8738	0	28.8738	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6291550926	2016-08-17 15:05:59	57626	2016-08-26 00:00:00	57087.4767013889	2015-03-06 11:26:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091502	The metallicity of the hot gas in the halos of isolated galaxies distinguishes between two models of galaxy formation, but few galaxies have bright enough halos to make this measurement. Metallicities measured in these systems are applied broadly and used in models, so it is important to understand the limits of the measurement. We address two ilimitations: we estimate the systematic error in the metallicity by comparing Suzaku and XMM-Newton observations, and we determine whether the bright, metal-enriched gas around starburst galaxies represents most of their mass.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	EDMUND HODGES-KLUCK		USA	9	AO9	MEASURING SYSTEMATIC UNCERTAINTY IN THE HALO METALLICITY OF NGC 891 AND NGC 4631	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809054010/	Quick Look
704	RXJ1159+5531 W	179.7493	55.5442	179.104587	55.822511	149.726184	49.068198	137.82331154	60.04203639	299.9575	56808.2513657407	2014-05-31 06:01:58	56809.8959490741	2014-06-01 21:30:10	809064010	95.109	100	95.109	96.041	0	96.033	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.1837731482	2016-08-15 04:24:38	57194	2015-06-21 00:00:00	56828.5942592593	2014-06-20 14:15:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091521	In contrast to some recent observations of cluster outskirts, for RXJ1159+5531, we obtain measurements of the gas fraction and entropy at the virial radius that are fully consistent with gravity-only structure formation simulations. Our preliminary Suzaku analysis of an opposite direction shows similar results. This encouraging consistency suggests that we may see little azimuthal variation in the gas properties for this unusually relaxed system. To verify and also benefit from the relaxed state of this benchmark system, we propose complementary Suzaku observations of RXJ1159+5531 in the other two directions. Simultaneously fitting these pointings would provide us the metal abundance ratios at large radii in order to place broad constrains on the enrichment history of group scale systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YUANYUAN SU		USA	9	AO9	MAPPING A BENCHMARK RELAXED POOR CLUSTER OUT TO ITS VIRIAL RADIUS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809064010/	Quick Look
705	ABELL 98-NORTH	11.5755	20.8389	10.914314	20.565865	18.902557	14.584397	121.31667052	-42.01674062	67.4405	56840.5909259259	2014-07-02 14:10:56	56841.1634375	2014-07-03 03:55:21	809078010	25.0582	100	0	0	0	25.0582	0	0	0	1	0	0	0	0	0	0	0	PROCESSED	57615.3531481482	2016-08-15 08:28:32	56748	2014-04-01 00:00:00	56855.7487268518	2014-07-17 17:58:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091525	We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	SCOTT RANDALL		USA	9	AO9	EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809078010/	Quick Look
706	ABELL 98-NORTH	11.5799	20.8287	10.918717	20.555669	18.902203	14.573403	121.32183614	-42.02704716	251.2557	57012.9175231482	2014-12-21 22:01:14	57014.2377430556	2014-12-23 05:42:21	809078030	49.5381	50	49.5381	51.7925	0	51.8085	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.5690509259	2016-08-17 13:39:26	56748	2014-04-01 00:00:00	57107.4424305556	2015-03-26 10:37:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091525	We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	SCOTT RANDALL		USA	9	AO9	EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809078030/	Quick Look
707	SWCL1313+0802	198.2492	8.0414	197.620834	8.306256	193.672615	14.576147	318.90135946	70.24184099	291.5304	56850.0041435185	2014-07-12 00:05:58	56850.5002199074	2014-07-12 12:00:19	809087010	20.2705	20	20.2705	20.2705	0	20.2705	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.3782986111	2016-08-15 09:04:45	57229	2015-07-26 00:00:00	56861.6452083333	2014-07-23 15:29:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091531	The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	XINYU DAI		USA	9	AO9	X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809087010/	Quick Look
708	SWCL1330+4206	202.7226	42.119	202.178472	42.376237	179.66908	46.823596	97.20252966	72.98152353	144.6477	56984.0225347222	2014-11-23 00:32:27	56985.3840740741	2014-11-24 09:13:04	809088010	15.8612	49	15.8612	15.8776	0	15.8692	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.8069212963	2016-08-16 19:21:58	57548	2016-06-09 00:00:00	57009.4143981482	2014-12-18 09:56:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091531	The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	XINYU DAI		USA	9	AO9	X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809088010/	Quick Look
709	ABELL 2151A	241.1446	17.7141	240.581846	17.849628	234.487601	37.662842	31.46236827	44.65865226	285.8808	56883.5616898148	2014-08-14 13:28:50	56883.843900463	2014-08-14 20:15:13	809098010	11.0268	10	11.0348	11.0348	0	11.0268	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.4947569444	2016-08-16 11:52:27	57270	2015-09-05 00:00:00	56910.6327893518	2014-09-10 15:11:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809098010/	Quick Look
710	RX J1347.5-1145	206.856	-11.8093	206.189594	-11.560184	209.147124	-0.679556	323.97916756	48.76108187	292.056	53916.7756597222	2006-06-30 18:36:57	53918.7600115741	2006-07-02 18:14:25	801013010	69.6611	75	69.6611	69.6611	69.6611	69.6611	2	2	2	2	1	0	0	60.982	60.982	171.3759	0	PROCESSED	57534.8555671296	2016-05-26 20:32:01	54394	2007-10-21 00:00:00	53926.4810300926	2006-07-10 11:32:41	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010014	We propose to obtain broad-band spectra of the most X-ray luminous cluster of galaxies RXJ1347.5-1145 at z=0.45. Our previous high-resolution Sunyaev-Zel'dovich obvervations of this cluster revealed that it exhibits an unusually violent merger activity. Its high X-ray luminosity ensures the unprecedented high-quality spectra with Suzaku. It is indeed a unique target to probe gas physics and particle acceleration mechanism associated with the violent mergers at high redshift. The continuum observations with HXD and XIS as well as the iron line spectroscopy will specify the physical states of both thermal and non-thermal components of the ICM. Combined with the Chandra and our SZ data, the Suzaku data will accomplish the first comprehensive modeling of a violent merger in distant clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	NAOMI OTA		JAP	1	AO1	BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801013010/	Quick Look
711	OPHIUCHUS CLUSTER 5	258.0184	-23.1077	257.261763	-23.048099	258.982957	-0.123527	0.73892155	9.49336651	88.7652	54181.8276736111	2007-03-22 19:51:51	54182.4890277778	2007-03-23 11:44:12	801026010	24.2557	15	24.2557	24.2557	0	24.2557	2	2	0	2	1	0	0	19.2271	19.2271	57.1359	0	PROCESSED	57537.9767013889	2016-05-29 23:26:27	54736	2008-09-27 00:00:00	54186.2070949074	2007-03-27 04:58:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010065	The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUTAKA FUJITA		JAP	1	AO1	PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801026010/	Quick Look
712	M87 CENTER	187.7366	12.4456	187.103964	12.721646	182.061198	14.477269	283.82387862	74.55209055	120.529	54068.9187037037	2006-11-29 22:02:56	54071.1266666667	2006-12-02 03:02:24	801038010	98.1831	100	98.1831	98.1831	0	98.1831	1	1	0	1	1	0	0	88.2503	88.2503	190.7308	2	PROCESSED	57536.2829050926	2016-05-28 06:47:23	54735	2008-09-26 00:00:00	54090.4156134259	2006-12-21 09:58:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010084	The black hole at the center of M87 is one of the most heaviest in the universe. Recently TeV-gamma ray emission from M87 was found. M87 is thus a very strong candidate for an accelerator of ultra-high energy cosmic rays. We aim at the detection of non-thermal hard X-rays from M87 to clarify the mechanism of the particle acceleration. The giant elliptical galaxy M87 is at the center of the Virgo cluster of galaxies, which is the nearest cluster. We can investigate the distribution of various metal elements. We will clarify how the metals, especially oxygen, diffuse to the intracluster space from the galaxy M87.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	HIRONORI MATSUMOTO		JAP	1	AO1	NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801038010/	Quick Look
713	PERSEUS CL OFFSET	49.6445	42.068	48.814215	41.886236	58.537476	22.936041	150.06631202	-12.92163855	65.996	53980.0800925926	2006-09-02 01:55:20	53980.7668287037	2006-09-02 18:24:14	801049010	29.2438	30	29.2559	29.2479	29.2518	29.2438	2	2	2	2	1	0	0	25.6729	25.6729	59.3299	1	PROCESSED	57535.4121296296	2016-05-27 09:53:28	54526	2008-03-01 00:00:00	54021.3135416667	2006-10-13 07:31:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010097	We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	1	AO1	MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049010/	Quick Look
714	PERSEUS CL OFFSET	50.2242	41.1004	49.398659	40.920786	58.698225	21.886134	150.98569591	-13.49005998	65.9967	53981.4552662037	2006-09-03 10:55:35	53982.1418287037	2006-09-04 03:24:14	801049030	32.8396	30	32.8556	32.8476	32.8396	32.8636	1	1	1	1	1	0	0	31.0313	31.0313	59.288	0	PROCESSED	57535.4291087963	2016-05-27 10:17:55	54526	2008-03-01 00:00:00	54020.8372106482	2006-10-12 20:05:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010097	We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	1	AO1	MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049030/	Quick Look
715	ABELL 2199 OFFSET 2	247.3619	39.6495	246.934152	39.757579	233.32636	60.237575	63.07626508	43.54039287	251.2564	54011.5284722222	2006-10-03 12:41:00	54012.1578587963	2006-10-04 03:47:19	801058010	22.7072	25	22.7232	22.7072	22.7232	22.7232	2	2	2	2	1	0	0	20.704	20.704	54.36	0	PROCESSED	57535.7442476852	2016-05-27 17:51:43	54735	2008-09-26 00:00:00	54024.6719907407	2006-10-16 16:07:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010138	Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	1	AO1	PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801058010/	Quick Look
716	M101	210.8841	54.3679	210.442342	54.607302	174.405989	59.838606	101.97854462	59.72940376	150.2959	54062.5790625	2006-11-23 13:53:51	54064.7182175926	2006-11-25 17:14:14	801063010	98.8522	100	98.8762	98.8522	0	98.8762	2	2	0	2	1	0	0	89.6125	89.6125	184.802	2	PROCESSED	57536.2145486111	2016-05-28 05:08:57	54455	2007-12-21 00:00:00	54088.707650463	2006-12-19 16:59:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011402	We wish to obtain a Suzaku spectrum of the diffuse X-ray emission in a typical galactic disk. The spectral resolution obtainable with Chandra/XMM does not allow the decomposition of the spectrum into more than two thermal components. The higher spectral resolution, better soft response, and lower instrumental background of Suzaku will allow the decomposition into at least three thermal components, and will place constraints on the number of thermal components and the distribution of temperatures and emission measures. The more refined fitting allowed by Suzaku spectra will allow a greater understanding of the sources of the X-ray emission. Given the Suzaku spatial resolution and detector size, M101 is the best observable example of a "typical" galactic disk.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	K. KUNTZ		USA	1	AO1	SOFT DIFFUSE X-RAY EMISSION FROM M101	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801063010/	Quick Look
717	SN 1987A	83.9013	-69.2655	83.9928	-69.294887	307.391677	-86.458548	279.69660922	-31.92548266	330.0004	53894.6930555556	2006-06-08 16:38:00	53895.6683449074	2006-06-09 16:02:25	801090010	39.6464	40	39.6464	39.6464	39.6464	39.6464	2	2	2	2	1	0	0	39.2519	39.2519	84.2399	0	PROCESSED	57534.6267592593	2016-05-26 15:02:32	54400	2007-10-27 00:00:00	53928.1346527778	2006-07-12 03:13:54	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012006	In an early Suzaku observation during the SWG time in November 2005 we have already obtained an excellent XIS spectrum. The flux of SN 1987A continues to rise exponentially with an e-folding time of ~800 days. The abundances in the ejecta could be measured with unprecedented accuracy. We confirm that Oxygen and Iron are significantly underabundant with respect to other elements, indicating the formation of dust, maybe even black rust grains (Fe3O4). We propose to monitor the chemical evolution of SN 1987A with Suzaku for 40 ksec in AO-1, where we expect about twice the previous flux. The exponential brightening and the chemical abundance is expected to change, when the full inner ring is engulfed. Simultaneously we can search for a periodic hard signal from the putative pulsar.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	G NTHER HASINGER		EUR	1	AO1	SN 1987A - A RUSTY REMNANT?	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801090010/	Quick Look
718	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
719	A2142 OFFSET3	239.0356	27.7434	238.520462	27.887676	228.29172	46.798568	44.85726257	49.26078026	283.7312	54341.8454166667	2007-08-29 20:17:24	54342.3960532407	2007-08-30 09:30:19	802032010	23.7899	20	23.7899	23.7899	0	23.7899	2	2	0	2	1	0	0	14.2425	14.2425	47.5699	0	PROCESSED	57539.8930671296	2016-05-31 21:26:01	54724	2008-09-15 00:00:00	54356.294849537	2007-09-13 07:04:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020076	We propose to search for redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in a large-scale filament outside of a massive merging cluster of galaxies A2142. This cluster is characterized by prominent cold fronts, elongated X-ray morphology, and Beppo-SAX detection of hard X-ray emission, which all point to a recent merger and the matter density outside should be high. The strong reason why we choose this target is its right redshift (z=0.909), in which XIS sensitivity for redshifted oxygen lines separated from the Galactic lines becomes the highest. We expect 3 times higher sensitivity than our previous attempt for A2218 (Takei et al. in press) where we set 5 times lower upper limit for OVII line intensity than the XMM reported levels in other clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKAYA OHASHI		JAP	2	AO2	WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802032010/	Quick Look
720	NGC 1553	64.0253	-55.7788	63.753175	-55.901382	28.715493	-73.694617	265.63371114	-43.7014546	176.9406	54429.7042939815	2007-11-25 16:54:11	54431.9029976852	2007-11-27 21:40:19	802050010	98.7222	95	98.7222	98.7222	0	98.7222	2	2	0	2	1	0	0	87.7903	87.7903	189.9159	2	PROCESSED	57540.6454976852	2016-06-01 15:29:31	54806	2008-12-06 00:00:00	54438.4258101852	2007-12-04 10:13:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021401	As driving engines of metal enrichment, early-type galaxies provide vital laboratories to investigate how it operates. In our Chandra survey of galaxies, we found solar ISM abundances (Zfe), similar to the stars and implying enrichment homology from clusters to moderate-Lx galaxies. The only outlier was NGC1553, for which we found a tantalizing hint of very subsolar Zfe, inconsistent with simple models. Unlike other galaxies with recent reports of low Zfe, NGC1553 has a bright gas halo, so the results are insensitive to the modelling of unresolved LMXB. We propose an 80ks observation of NGC1553 to measure definitively the ISM abundances of Fe and other crucial diagnostic elements. These data will either confirm enrichment bimodality or provide a vital low-Lx data-point to anchor models.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	PHILIP HUMPHREY		USA	2	AO2	NGC 1553: PROOF OF BIMODAL METAL ENRICHMENT?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802050010/	Quick Look
721	BOOTES GROUP 7	217.7796	35.0938	217.258508	35.314562	199.66622	46.620571	59.62119131	67.30227758	316.719	54266.3117592593	2007-06-15 07:28:56	54267.3863310185	2007-06-16 09:16:19	802053010	42.1244	38	42.1324	42.1244	0	42.1324	2	2	0	2	1	0	0	37.3384	37.3384	92.8238	0	PROCESSED	57538.9915509259	2016-05-30 23:47:50	54695	2008-08-17 00:00:00	54322.4630324074	2007-08-10 11:06:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021424	We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MARSHALL BAUTZ		USA	2	AO2	SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802053010/	Quick Look
722	ABELL 2029	227.4644	6.0238	226.845557	6.213105	223.157402	22.814931	6.57368779	50.92713703	112.4532	54473.6848958333	2008-01-08 16:26:15	54478.0211226852	2008-01-13 00:30:25	802060010	169.2861	160	169.2861	169.2861	0	169.2861	2	2	0	2	1	0	0	150.7661	150.7661	374.6201	4	PROCESSED	57541.3859953704	2016-06-02 09:15:50	54860	2009-01-29 00:00:00	54490.7163657407	2008-01-25 17:11:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021433	The properties of clusters of galaxies in very distant regions encompassing the virial radius (r_vir) are poorly understood yet these regions are sites of very important processes for the cluster formation and evolution. The recent generation of X-ray satellites (Chandra and XMM) thanks to their fine spatial resolution and high sensitivity have provided so far detailed spectral information mainly in the inner bright regions but they have not been very helpful in background dominated regimes typical of cluster outskirts' observations because of their high background. Suzaku has the capabilities to target those regions. We propose to observe the outskirts of the very relaxed cluster of galaxies A2029 with XIS to measure for the first time temperature and metallicity of the ICM up to r_vir.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	LUCA ZAPPACOSTA		USA	2	AO2	EXPLORING THE OUTSKIRTS OF THE RELAXED CLUSTER ABELL 2029	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802060010/	Quick Look
723	ABEL 754	137.2113	-9.6361	136.602656	-9.432794	142.867226	-24.832228	239.25284371	24.7578079	295.1878	54249.7445833333	2007-05-29 17:52:12	54252.4495949074	2007-06-01 10:47:25	802063010	108.9779	100	108.9859	108.9859	0	108.9779	2	2	0	2	1	0	0	97.904	97.904	233.6958	2	PROCESSED	57538.8549537037	2016-05-30 20:31:08	54773	2008-11-03 00:00:00	54257.5596759259	2007-06-06 13:25:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021445	We propose a 100 ksec observation of Abell 754 and a 50 ksec observation of Triangulum Australis, in order to measure the spectral shape and flux of possible nonthermal emission from clusters of galaxies. They are bright clusters of galaxies in the BAT all sky survey sample, which is crucial for making good spectral measurements by the HXD. And their spectra have a significant hard excess (power-law component). We intend to constrain the power-law photon index of the nonthermal emission for the first time and to determine the size of hard X-ray emitting region by using both of the HXD and Swift BAT data. We are aiming to test the origin of the hard flux and see whether it originates from either diffuse inverse Compton scattering by relativistic cosmic-ray electrons or an AGN.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKASHI OKAJIMA		USA	2	AO2	OBSERVATIONS OF NONTHERMAL EMISSION FROM CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802063010/	Quick Look
724	RCS 1122+2423	170.6071	24.3899	169.945012	24.664262	161.499487	18.645294	215.72830536	69.79971375	120.0624	54421.3268518518	2007-11-17 07:50:40	54421.8891087963	2007-11-17 21:20:19	802070010	20.9729	18	20.9809	20.9809	0	20.9729	2	2	0	2	1	0	0	19.022	19.022	48.5679	0	PROCESSED	57540.5406828704	2016-06-01 12:58:35	54797	2008-11-27 00:00:00	54430.3244097222	2007-11-26 07:47:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021451	We propose Suzaku observations of a sample of 10 galaxy clusters at redshifts between 0.6 and 0.95 from the RCS-1 cluster survey. These objects represent the optically richest clusters at these redshifts from the 100 square degree survey using the red-sequence method of cluster detection. As such, they form a critical sample for calibrating the mass-richness relationship for high redshift cluster surveys. Our proposed observations will allow us to determine their X-ray luminosities, as a first guide to estimating their masses, and enable future studies to determine accurate masses from their X-ray properties. These studies are complimentary to mass calibration programs we are carrying out using estimates based on lensing, IR stellar mass and galaxy dynamics.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	2	AO2	A SUZAKU SNAPSHOT SURVEY OF HIGH-REDSHIFT GALAXY CLUSTERS FROM THE RCS SURVEY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802070010/	Quick Look
725	COMABKG2	194.3428	28.1403	193.738458	28.410336	180.855412	31.302815	70.87532192	88.34137752	297.3385	54272.7041550926	2007-06-21 16:53:59	54273.4897453704	2007-06-22 11:45:14	802084010	31.9731	30	31.9731	33.5956	0	33.5956	2	2	0	2	1	0	0	28.853	28.853	67.8501	1	PROCESSED	57539.0184143518	2016-05-31 00:26:31	54695	2008-08-17 00:00:00	54318.5135648148	2007-08-06 12:19:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	024438	Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JOEL BREGMAN	Yoh Takei	USJ	2	AO2	THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802084010/	Quick Look
726	NGC3556	167.883	55.6841	167.153795	55.95585	141.585681	45.289435	148.29932367	56.24590288	111.9355	54795.9750694444	2008-11-25 23:24:06	54797.8890162037	2008-11-27 21:20:11	803013010	84.1642	100	84.1702	84.1659	0	84.1642	2	2	0	2	1	0	0	60.3537	60.3537	165.2879	2	PROCESSED	57544.6094212963	2016-06-05 14:37:34	55175	2009-12-10 00:00:00	54811.7645717593	2008-12-11 18:20:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030058	We propose to observe NGC 3556, a nearby edge-on spiral galaxy, with 100 ks exposure. Galactic coronal X-ray emission in and around several spiral galaxies have been spatially resolved using Chandra and XMM instruments. The target is one of these galaxies showing relatively luminous X-ray emission. Due to limited spectral capability of these instruments, X-ray spectral properties of these diffuse emission have not yet been investigated. We use good spectral capability of the SUZAKU/XIS to investigate the temperature structure and constrain the metal abundance pattern for the first time in galactic corona. We study origin, heating mechanism, and chemical properties of these galactic corona.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKAYUKI TAMURA		JAP	3	AO3	GALACTIC CORONA IN AND AROUND THE EDGE-ON GALAXY NGC 3556	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803013010/	Quick Look
727	A2163_NE	244.026	-6.0591	243.359036	-5.935716	243.191505	14.996833	6.90407558	30.45267126	113.8304	54870.8869560185	2009-02-08 21:17:13	54872.1724421296	2009-02-10 04:08:19	803022010	51.7974	40	51.8054	51.8134	0	51.7974	2	2	0	2	1	0	0	43.861	43.861	111.0518	1	PROCESSED	57545.4990162037	2016-06-06 11:58:35	55330	2010-05-14 00:00:00	54895.5963888889	2009-03-05 14:18:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030094	We propose 2 pointing observations of a hot cluster A2163 (z=0.2). A2163 is an X-ray brightest object among the violent merger candidates, which possess a huge radio halo and a complex temperature structure. Thus it is a unique target to discover extremely hot (>20keV) gas produced via merger shock. Thanks to the unprecedent high-quality broad-band spectra of Suzaku we can accurately determine the temperature of the hot gas. Which, at the same time, leads to the detection of the buried non-thermal hard X-ray emission. Combining this observation with the high-resolution images of our thermal SZ effect and the XMM observation, we can obtain a spatial distribution of the extremely hot thermal gas in the merging cluster for the first time.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	3	AO3	BROAD-BAND SPECTROSCOPY OF THE HOTTEST ABELL GALAXY CLUSTER A2163	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803022010/	Quick Look
728	N154 SB	84.0182	-69.641	84.124614	-69.669786	303.069824	-86.201105	280.12884425	-31.83619967	313.3253	54583.7906944444	2008-04-27 18:58:36	54584.7849305556	2008-04-28 18:50:18	803037010	50.404	40	50.404	50.404	0	50.404	2	2	0	2	1	0	0	56.6171	56.6171	85.8878	1	PROCESSED	57542.411724537	2016-06-03 09:52:53	54964	2009-05-13 00:00:00	54598.4914699074	2008-05-12 11:47:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031238	Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 3 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 3 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	LARRY MADDOX		USA	3	AO3	A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803037010/	Quick Look
729	NGC 5846	226.6234	1.6025	225.988646	1.794814	223.667836	18.340527	0.42380195	48.79350498	287.2336	54675.6192939815	2008-07-28 14:51:47	54679.0008564815	2008-08-01 00:01:14	803042010	155.9331	150	155.9331	155.9331	0	155.9331	2	2	0	2	1	0	0	145.4704	145.4704	292.1519	2	PROCESSED	57543.2487152778	2016-06-04 05:58:09	55059	2009-08-16 00:00:00	54693.5527546296	2008-08-15 13:15:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031404	We propose Suzaku observations of three elliptical galaxies, selected on brightness and the availability of XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. The low-energy sensitivity, spectral resolution, and low background of the Suzaku XIS enables the first accurate model-independent measurements of the abundance pattern while expanding the number of measurable temperature diagnostic features. Analysis of XIS spectra (critically, with SCI on), exclusively and in combination with RGS data, demonstrates the unique power of Suzaku to contribute to our understanding of the thermal and chemical properties of these systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MICHAEL LOEWENSTEIN		USA	3	AO3	UNCOVERING THE TRUE ABUNDANCES OF ELLIPTICAL GALAXIES WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803042010/	Quick Look
730	A496 P-OUT	68.2513	-13.0087	67.67058	-13.113188	64.018052	-34.510238	209.22191803	-36.52315476	62.0525	54674.5225347222	2008-07-27 12:32:27	54675.6050231482	2008-07-28 14:31:14	803048010	37.5516	35	37.5516	37.5596	0	37.5596	2	2	0	2	1	0	0	33.1599	33.1599	93.4939	1	PROCESSED	57543.1577314815	2016-06-04 03:47:08	55055	2009-08-12 00:00:00	54689.4360416667	2008-08-11 10:27:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031424	A496 is a "normal" nearby cluster that has been the testbed for metal enrichment models in clusters and, more recently, of different mechanisms to generate cold fronts. Suzaku's excellent spectral resolution, low background and high effective area, combined with the moderate temperatures of this cluster allows us to probe, with two short exposures, into the large scale metal enrichment processes through determination of elemental abundance ratios out to half the virial radius for the first time.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	RENATO DUPKE		USA	3	AO3	LARGE SCALE METAL ENRICHMENT MECHANISMS IN ABELL 496	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803048010/	Quick Look
731	RCS2347-3535	356.9535	-35.5892	356.30102	-35.867184	341.527794	-31.116965	357.03141214	-74.03003146	61.6856	54617.4612384259	2008-05-31 11:04:11	54617.8890509259	2008-05-31 21:20:14	803057010	15.4812	11	15.4892	15.4892	0	15.4812	2	2	0	2	1	0	0	14.6376	14.6376	36.9599	0	PROCESSED	57542.6853703704	2016-06-03 16:26:56	54999	2009-06-17 00:00:00	54633.6966087963	2008-06-16 16:43:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031441	Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	3	AO3	COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803057010/	Quick Look
732	RCS1102-0340	165.6613	-3.6697	165.025025	-3.400357	168.238102	-9.034138	258.27932815	49.53254853	114.238	54817.9779282407	2008-12-17 23:28:13	54818.8987731482	2008-12-18 21:34:14	803064010	37.789	28	37.797	37.797	0	37.789	2	2	0	2	1	0	0	27.621	27.621	79.55	1	PROCESSED	57545.0002893518	2016-06-06 00:00:25	55206	2010-01-10 00:00:00	54840.5080439815	2009-01-09 12:11:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031441	Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	3	AO3	COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803064010/	Quick Look
733	A3558 WEST OFF	201.4503	-31.5856	200.748303	-31.325817	211.928183	-20.890972	311.44383739	30.71755895	288.4754	54657.5304513889	2008-07-10 12:43:51	54660.0225	2008-07-13 00:32:24	803072010	81.8162	80	81.8162	81.8162	0	81.8162	2	2	0	2	1	0	0	67.3941	67.3941	215.2857	1	PROCESSED	57543.1016898148	2016-06-04 02:26:26	55037	2009-07-25 00:00:00	54670.5540162037	2008-07-23 13:17:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	033089	We aim at the first significant detection of redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in the Shapley Supercluster. The system, located at z = 0.048, shows the richest concentration of X-ray clusters in the nearby universe. Previous ROSAT observation showed enhanced soft X-ray emission along the cluster connection. We propose to observe for 80 ksec a region between A3558 (the brightest central cluster) and A3556, separated by 0.9 virial radius from both clusters and along the line of cluster connection. A 40 ksec observation is also proposed at a 2-degree offest region to measure the foreground Galactic spectrum. Based on the ROSAT flux, we expect to detect redshifted OVII and OVII lines at more than 7 sigma confidence.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI	MASSIMILIANO GALEAZZAI	JUS	3	AO3	SEARCH FOR WHIM IN THE SHAPLEY SUPERCLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803072010/	Quick Look
734	FERMI_0265	187.7993	-14.1672	187.149588	-13.891145	192.78645	-9.915447	295.5292019	48.41340382	292.6305	55040.2233449074	2009-07-28 05:21:37	55041.5002777778	2009-07-29 12:00:24	804017020	52.6378	54	52.6378	52.9098	0	52.9018	3	2	0	2	1	0	0	48.06	48.06	110.3041	0	PROCESSED	57547.9908333333	2016-06-08 23:46:48	55422	2010-08-14 00:00:00	55050.4462384259	2009-08-07 10:42:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040014	We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JUN KATAOKA		JAP	4	AO4	SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804017020/	Quick Look
735	FERMI_0291	203.2955	51.017	202.790071	51.273115	172.022229	54.301955	107.38909593	64.83295576	302.8355	54983.4258680556	2009-06-01 10:13:15	54984.4725	2009-06-02 11:20:24	804019010	46.3536	40	46.3616	46.3536	0	46.3696	2	2	0	2	1	0	0	42.7073	42.7073	90.3858	1	PROCESSED	57547.4428703704	2016-06-08 10:37:44	55363	2010-06-16 00:00:00	54994.2756018518	2009-06-12 06:36:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040014	We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JUN KATAOKA		JAP	4	AO4	SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804019010/	Quick Look
736	NGC741MOSAICE_P3	29.6423	5.6966	28.988354	5.453848	29.583767	-6.010817	151.72656453	-53.38013742	71.7748	55054.3340509259	2009-08-11 08:01:02	55054.5765393518	2009-08-11 13:50:13	804052030	9.8918	10	9.8918	9.8918	0	9.9078	1	1	0	1	1	0	0	7.9599	7.9599	20.9439	1	PROCESSED	57548.1180555556	2016-06-09 02:50:00	55448	2010-09-09 00:00:00	55081.2008101852	2009-09-07 04:49:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052030/	Quick Look
737	NGC741MOSAICS_P2	29.298	4.8125	28.646295	4.568934	28.95035	-6.72009	151.84866444	-54.32564909	71.7104	55052.6950925926	2009-08-09 16:40:56	55052.9238310185	2009-08-09 22:10:19	804054020	11.4289	10	11.4529	11.4289	0	11.4529	1	1	0	1	1	0	0	6.3123	6.3123	19.7439	0	PROCESSED	57548.0884953704	2016-06-09 02:07:26	55451	2010-09-12 00:00:00	55085.0388425926	2009-09-11 00:55:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054020/	Quick Look
738	ABELL 426 E4	51.4246	41.5162	50.593046	41.341069	59.755665	22.042042	151.51141512	-12.63936589	90	55042.2912847222	2009-07-30 06:59:27	55042.7466898148	2009-07-30 17:55:14	804059010	21.8613	20	21.8613	21.8613	0	21.8613	1	1	0	1	1	0	0	19.707	19.707	39.336	0	PROCESSED	57547.9976736111	2016-06-08 23:56:39	55427	2010-08-19 00:00:00	55060.7938425926	2009-08-17 19:03:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804059010/	Quick Look
739	ABELL 426 E6	52.1705	41.5044	51.337024	41.332096	60.333006	21.882473	151.98723888	-12.32905015	86.9996	55043.2937847222	2009-07-31 07:03:03	55043.9501736111	2009-07-31 22:48:15	804061010	31.9431	30	31.9431	31.9431	0	31.9431	2	2	0	2	1	0	0	29.9436	29.9436	56.702	1	PROCESSED	57548.0213657407	2016-06-09 00:30:46	55427	2010-08-19 00:00:00	55060.7142013889	2009-08-17 17:08:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804061010/	Quick Look
740	ABELL 426 N1	49.7797	41.7196	48.951337	41.538337	58.536882	22.573374	150.34867405	-13.15794685	59.9997	55061.841099537	2009-08-18 20:11:11	55062.1397453704	2009-08-19 03:21:14	804063010	14.7276	10	14.7356	14.7276	0	14.737	1	1	0	1	1	0	0	13.1724	13.1724	25.7919	0	PROCESSED	57548.2770833333	2016-06-09 06:39:00	55441	2010-09-02 00:00:00	55075.0515740741	2009-09-01 01:14:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804063010/	Quick Look
741	ABELL2811-OFF	10.1781	-28.7333	9.563743	-29.007637	356.740152	-30.181509	358.19144602	-87.13859798	232.6526	53702.8821296296	2005-11-28 21:10:16	53703.731412037	2005-11-29 17:33:14	800006010	33.9494	25	33.9574	33.9654	33.9494	33.9498	2	2	2	2	1	0	0	30.9056	30.9056	73.3659	1	PROCESSED	57528.1125115741	2016-05-20 02:42:01	54247	2007-05-27 00:00:00	54038.6719560185	2006-10-30 16:07:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001025	We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYUKI TAMURA		JAP	0	SWG	THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800006010/	Quick Look
742	ABELL 2199 OFFSET 1	247.0269	39.6504	246.598636	39.759978	232.832467	60.158374	63.06766091	43.79825488	251.7923	54009.8973958333	2006-10-01 21:32:15	54010.4467476852	2006-10-02 10:43:19	801057010	24.6315	25	24.6315	24.6315	24.6315	24.6315	2	2	2	2	1	0	0	25.5343	25.5343	47.454	0	PROCESSED	57535.7339814815	2016-05-27 17:36:56	54735	2008-09-26 00:00:00	54021.2449189815	2006-10-13 05:52:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010138	Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	1	AO1	PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801057010/	Quick Look
743	ABELL 2199 OFFSET 3	247.3596	39.3165	246.92934	39.424595	233.528009	59.920137	62.61707687	43.53145251	252.4737	54012.1589351852	2006-10-04 03:48:52	54012.6786921296	2006-10-04 16:17:19	801059010	25.2467	25	25.2467	25.2467	25.2467	25.2467	1	1	1	1	1	0	0	20.505	20.505	44.8879	1	PROCESSED	57535.7507291667	2016-05-27 18:01:03	54735	2008-09-26 00:00:00	54025.4730092593	2006-10-17 11:21:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010138	Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	1	AO1	PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801059010/	Quick Look
744	N206 SB	82.6396	-71.0391	82.803839	-71.074403	297.258629	-84.798656	281.83986558	-32.08582418	315.5807	54584.7862384259	2008-04-28 18:52:11	54585.7640509259	2008-04-29 18:20:14	803038010	48.8345	40	48.8345	48.8345	0	48.8345	2	2	0	2	1	0	0	54.7297	54.7297	84.4678	1	PROCESSED	57542.434837963	2016-06-03 10:26:10	54964	2009-05-13 00:00:00	54598.4969444445	2008-05-12 11:55:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031238	Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 3 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 3 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	LARRY MADDOX		USA	3	AO3	A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803038010/	Quick Look
745	COMA OUTSKIRTS3	196.1692	28.7094	195.570451	28.977142	182.240031	32.536562	62.09765822	86.67565791	116.0002	55901.9229513889	2011-12-06 22:09:03	55902.7161342593	2011-12-07 17:11:14	806022010	31.22	30	31.244	31.22	0	31.22	2	2	0	2	1	0	0	28.7241	28.7241	68.5199	0	PROCESSED	57604.0669212963	2016-08-04 01:36:22	56284	2012-12-23 00:00:00	55915.1959837963	2011-12-20 04:42:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060099	In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKUYA SATO		JAP	6	AO6	STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806022010/	Quick Look
746	NGC741S2_P1	29.0961	5.1589	28.443649	4.91486	28.882528	-6.325199	151.28423043	-54.09870829	71.6444	55053.3762962963	2009-08-10 09:01:52	55053.6078587963	2009-08-10 14:35:19	804055010	8.6016	10	8.6176	8.6016	0	8.6256	1	1	0	1	1	0	0	8.748	8.748	19.984	1	PROCESSED	57548.1032291667	2016-06-09 02:28:39	55465	2010-09-26 00:00:00	55098.1609375	2009-09-24 03:51:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804055010/	Quick Look
747	ABELL 426 E7	52.5439	41.4965	51.709488	41.325623	60.621576	21.801638	152.22519414	-12.17349332	85.5	55043.9514814815	2009-07-31 22:50:08	55044.6843055556	2009-08-01 16:25:24	804062010	30.9516	30	30.9516	31.2216	0	31.2056	3	2	0	2	1	0	0	28.5449	28.5449	63.314	0	PROCESSED	57548.0327083333	2016-06-09 00:47:06	55427	2010-08-19 00:00:00	55060.8353703704	2009-08-17 20:02:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804062010/	Quick Look
748	A2204_FIELD_3	248.3129	5.7152	247.698224	5.819454	245.539745	27.332187	21.30307351	33.20188623	261.0004	55436.6750347222	2010-08-28 16:12:03	55437.758587963	2010-08-29 18:12:22	805058010	36.2307	40	36.2387	36.2307	0	36.2467	2	2	0	2	1	0	0	31.6564	31.6564	93.6018	2	PROCESSED	57553.2217361111	2016-06-14 05:19:18	55287	2010-04-01 00:00:00	55449.3168634259	2010-09-10 07:36:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805058010/	Quick Look
749	A2744_SW	3.5132	-30.5508	2.881732	-30.828827	349.850108	-29.168885	8.03425743	-81.13040471	233.4967	55540.2569791667	2010-12-10 06:10:03	55542.2883217593	2010-12-12 06:55:11	805015010	69.7763	65	69.7763	69.7763	0	69.7763	2	2	0	2	1	0	0	59.2396	59.2396	175.4817	0	PROCESSED	57554.4226851852	2016-06-15 10:08:40	55917	2011-12-22 00:00:00	55551.0433101852	2010-12-21 01:02:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050013	We propose Suzaku observations of two merging clusters of galaxies, A2744 and the Bullet Cluster, to map the entropy variation out to the virial radius. Recent numerical simulations indicate that the entropy generation occurs through two-shock propagations, which is to be markedly seen in the cluster outskirts. On the other hand, little observational testing has been done for this regime of merging systems. We thus request three additional pointings to cover regions of large-scale filaments discovered in the optical. This study can only be achieved by Suzaku because of the lowest background level and excellent sensitivity, and will bring us new constraints on the thermodynamical history of the clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	5	AO5	MAPPING THE GAS ENTROPY GENERATION IN A SEQUENCE OF MERGING CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805015010/	Quick Look
750	RXCJ0411.2-4819	62.816	-48.3247	62.453818	-48.452722	38.950898	-67.014001	255.63059498	-46.16240445	110.1457	55461.4637384259	2010-09-22 11:07:47	55461.7793865741	2010-09-22 18:42:19	805024010	11.3649	10	11.3649	11.3649	0	11.3649	3	2	0	2	1	0	0	10.396	10.396	27.264	0	PROCESSED	57553.4942361111	2016-06-14 11:51:42	55836	2011-10-02 00:00:00	55470.1084606482	2010-10-01 02:36:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050021	We propose Suzaku observations of 5 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. Since some of the targets are to be observed in the AO4, we request an additional exposure for the remaining clusters to complete the program. With a short exposure time of 10 ks per cluster, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NAOMI OTA		JAP	5	AO5	LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805024010/	Quick Look
751	NGC 4697	192.1513	-5.7906	191.50498	-5.518104	193.427288	-0.530434	301.63561999	57.07401872	112.9816	55575.4840277778	2011-01-14 11:37:00	55578.1905324074	2011-01-17 04:34:22	805041010	102.3091	100	102.3091	102.3091	0	102.3091	2	2	0	2	1	0	0	76.0471	76.0471	233.8161	1	PROCESSED	57600.7175462963	2016-07-31 17:13:16	55962	2012-02-05 00:00:00	55595.5109027778	2011-02-03 12:15:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050080	We propose the observation of the elliptical galaxy NGC 4697, whose temperature of interstellar medium is low, 0.3 keV. Hot X-ray emitting interstellar medium (ISM) carries important information about the history of star formation and evolution of galaxies. The different abundance pattern between S0 and elliptical galaxies was reported in recent study. To understand the formation process of early-type galaxies in more detail, it is very important to appreciate whether the different abundance pattern is due to morphology or temperature of system. The purpose of this proposal is to reveal the relation between abundance pattern, morphology, and temperature of system by investigating the abundance pattern of the elliptical galaxy, which has lower temperature.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	SAORI KONAMI		JAP	5	AO5	MEASUREMENT OF ABUNDANCE PATTERN IN LOW TEMPARTURE ISM OF ELLIPTICAL GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805041010/	Quick Look
752	A1413_FIELD_2	178.6363	23.4218	177.992083	23.700041	169.007568	20.85313	225.87600909	76.62442609	303.0004	55346.1403240741	2010-05-30 03:22:04	55347.1856828704	2010-05-31 04:27:23	805060010	40.9512	40	40.9592	40.9512	0	40.9512	1	1	0	1	1	0	0	34.5464	34.5464	90.2959	0	PROCESSED	57551.669837963	2016-06-12 16:04:34	55287	2010-04-01 00:00:00	55365.258912037	2010-06-18 06:12:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805060010/	Quick Look
753	A383_FIELD_1	42.1211	-3.4616	41.492043	-3.669137	38.559838	-18.768369	177.79816007	-53.37318565	60.9988	55388.2747337963	2010-07-11 06:35:37	55389.1376388889	2010-07-12 03:18:12	805062010	40.3915	40	40.4155	40.3915	0	40.4155	1	1	0	1	1	0	0	35.3721	35.3721	74.52	1	PROCESSED	57552.5965046296	2016-06-13 14:18:58	55287	2010-04-01 00:00:00	55411.2489467593	2010-08-03 05:58:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805062010/	Quick Look
754	A383_FIELD_3	41.9643	-3.6473	41.33581	-3.855343	38.341492	-18.895957	177.84591826	-53.61436812	60.9989	55390.0630902778	2010-07-13 01:30:51	55390.9764930556	2010-07-13 23:26:09	805064010	43.1968	40	43.1968	43.1968	0	43.1968	2	2	0	2	1	0	0	39.5929	39.5929	78.8959	1	PROCESSED	57552.6323842593	2016-06-13 15:10:38	55287	2010-04-01 00:00:00	55411.2967592593	2010-08-03 07:07:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805064010/	Quick Look
755	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
756	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
757	COMA E1	195.2288	27.9019	194.626316	28.170859	181.798966	31.442311	53.6887936	87.76083997	279.9992	55728.9920601852	2011-06-16 23:48:34	55729.2682523148	2011-06-17 06:26:17	806030010	9.184	10	9.2	9.184	0	9.2	2	2	0	2	1	0	0	10.2038	10.2038	23.858	0	PROCESSED	57602.3046296296	2016-08-02 07:18:40	55652	2011-04-01 00:00:00	55770.1007407407	2011-07-28 02:25:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806030010/	Quick Look
758	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
759	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
760	CENTAURUS B	206.7067	-60.4086	205.850027	-60.15889	231.235341	-45.192759	309.7224369	1.73083578	275.5009	55758.843912037	2011-07-16 20:15:14	55760.4932060185	2011-07-18 11:50:13	806017010	93.6172	120	93.645	93.6172	0	93.637	1	1	0	1	0	0	0	0	0	27.6959	0	PROCESSED	57602.5915625	2016-08-02 14:11:51	56152	2012-08-13 00:00:00	55830.7256134259	2011-09-26 17:24:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060070	X-ray observation of radio lobe is essential to reveal the particle acceleration mechanism in the lobe, because we can obtain magnetic field and electron energy density without assumption of equipartition. The radio lobe of FR I radio galaxy Centaurus B was previously detected by ASCA. For revealing the mechanism of particle acceleration in radio lobes, detailed multi-wavelength observations are very important. We propose a deep observation of the radio lobe by Suzaku, which has the advantage of low background and high sensitivity for diffuse X-ray. Good quality Suzaku data combined with a detailed modeling reveals particle acceleration mechanism working in the radio lobe.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YASUYUKI TANAKA		JAP	6	AO6	X-RAY OBSERVATION OF RADIO LOBE OF FR I RADIO GALAXY CENTAURUS B	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806017010/	Quick Look
761	ABELL 426 N2	49.5875	41.9633	48.758073	41.781328	58.461538	22.847366	150.08864093	-13.03246307	59.9939	55062.1402662037	2009-08-19 03:21:59	55062.4716898148	2009-08-19 11:19:14	804064010	13.166	10	13.166	13.166	0	13.166	1	1	0	1	1	0	0	9.647	9.647	28.6239	0	PROCESSED	57548.2750578704	2016-06-09 06:36:05	55441	2010-09-02 00:00:00	55075.0035416667	2009-09-01 00:05:06	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804064010/	Quick Look
762	ABELL 426 N4	49.2103	42.4455	48.378755	42.262141	58.317611	23.388756	149.57911953	-12.77962749	59.999	55062.754837963	2009-08-19 18:06:58	55063.2460532407	2009-08-20 05:54:19	804066010	25.3046	20	25.3046	25.3065	0	25.3086	2	2	0	2	1	0	0	21.6295	21.6295	42.44	0	PROCESSED	57548.2829282407	2016-06-09 06:47:25	55441	2010-09-02 00:00:00	55075.0762384259	2009-09-01 01:49:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804066010/	Quick Look
763	ABELL 1068	160.4236	39.9791	159.703028	40.240763	145.773983	29.164286	178.96037586	60.29153459	130.001	55861.8826273148	2011-10-27 21:10:59	55863.1258564815	2011-10-29 03:01:14	806028020	52.0056	50	52.0136	52.0056	0	52.0196	2	2	0	2	1	0	0	43.2759	43.2759	107.4038	1	PROCESSED	57603.6533333333	2016-08-03 15:40:48	55652	2011-04-01 00:00:00	55874.1687615741	2011-11-09 04:03:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806028020/	Quick Look
764	A262 E1	28.6322	35.9862	27.896259	35.741034	39.692258	22.636644	136.99532529	-25.15665513	249.9998	56694.7928935185	2014-02-06 19:01:46	56695.3750694444	2014-02-07 09:00:06	808112010	25.9466	24	25.9546	25.9466	0	25.9626	3	3	0	3	0	0	0	0	0	0	0	PROCESSED	57613.7986226852	2016-08-13 19:10:01	57074	2015-02-21 00:00:00	56709.7127893518	2014-02-21 17:06:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	083002	We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KYOKO MATSUSHITA	NORBERT WERNER	JUS	8	AO8	OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808112010/	Quick Look
765	A76 EAST	10.1332	6.8374	9.486956	6.563068	11.989309	2.27755	118.09579875	-55.93191571	260.0024	55183.3444212963	2009-12-18 08:15:58	55183.8752199074	2009-12-18 21:00:19	804087010	23.621	15	23.637	23.621	0	23.629	1	1	0	1	1	0	0	18.6401	18.6401	45.8559	0	PROCESSED	57549.8965393518	2016-06-10 21:31:01	55575	2011-01-14 00:00:00	55209.4624652778	2010-01-13 11:05:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042018	In our flux limited survey of galaxy clusters in the ROSAT All-Sky Atlas we find that about 5 - 10 percent of the galaxy clusters have a diffuse, low X-ray surface brightness. These objects could possibly be explained as dynamically very young clusters, which have not yet formed a central core. Three such clusters in our XMM-Newton study of an unbiased sub-sample of 33 galaxy clusters, REXCESS, show suprisingly high entropies in their centers which does not readily support the early formation stage. To shed more light on the nature of these clusters we propose to observe two extremely low surface brightness clusters at low redshift, for which we also have detailed optical data. SUZAKU with its low background is ideally suited for this study.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	HANS BOEHRINGER		EUR	4	AO4	SHEDDING LIGHT ON THE NATURE OF EXTREMELY LOW SURFACE BRIGHTNESS CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804087010/	Quick Look
766	NGC5129 OFF-CENTER1	201.3141	14.0346	200.698603	14.294472	194.098163	21.268391	335.68408417	74.71314923	124.7585	55548.0427314815	2010-12-18 01:01:32	55548.7883101852	2010-12-18 18:55:10	805072010	30.2512	30	30.2512	30.2512	0	30.2512	2	2	0	2	1	0	0	24.4611	24.4611	64.4119	0	PROCESSED	57554.4566203704	2016-06-15 10:57:32	55960	2012-02-03 00:00:00	55592.9994444444	2011-01-31 23:59:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051512	Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	XINYU DAI		USA	5	AO5	BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805072010/	Quick Look
767	MKW 4-OFFSET2	181.4291	1.9058	180.78864	2.184142	180.549883	2.316727	277.53009765	62.50090006	114.4199	55530.2508101852	2010-11-30 06:01:10	55532.2286805556	2010-12-02 05:29:18	805082010	82.9361	80	82.9401	82.9361	0	82.9441	2	2	0	2	1	0	0	70.0619	70.0619	170.8541	2	PROCESSED	57554.329525463	2016-06-15 07:54:31	55910	2011-12-15 00:00:00	55544.2869328704	2010-12-14 06:53:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051525	We propose a set of two 19 arcmin offset observations for the galaxy groups MKW 4 to measure spatially resolved density, temperature and iron abundance out to r_{500}. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to its brightness, regularity and low temperature, the object is an ideal candidate for an offset observation of its peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	FABIO GASTALDELLO		USA	5	AO5	THE OUTSKIRTS OF MKW 4	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805082010/	Quick Look
768	PKS 0745-191	117.0925	-18.8008	116.536214	-18.67521	123.761788	-39.117935	236.11480248	3.4506494	113.9994	55514.1140625	2010-11-14 02:44:15	55515.1105324074	2010-11-15 02:39:10	805083010	37.2084	35	37.2164	37.2084	0	37.2164	1	1	0	1	1	0	0	31.5228	31.5228	86.0879	1	PROCESSED	57554.0728703704	2016-06-15 01:44:56	55903	2011-12-08 00:00:00	55537.2095486111	2010-12-07 05:01:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051526	Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MATTHEW GEORGE		USA	5	AO5	BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805083010/	Quick Look
769	PKS 0745-191	116.6522	-19.7838	116.101042	-19.660112	123.535239	-40.170782	236.7569882	2.59757333	114.0013	55515.1115162037	2010-11-15 02:40:35	55516.1335416667	2010-11-16 03:12:18	805087010	37.9286	35	37.9526	37.9446	0	37.9286	2	2	0	2	1	0	0	32.1037	32.1037	88.2858	2	PROCESSED	57554.1054976852	2016-06-15 02:31:55	55895	2011-11-30 00:00:00	55526.1606018518	2010-11-26 03:51:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051526	Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MATTHEW GEORGE		USA	5	AO5	BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805087010/	Quick Look
770	SNR 0519-69.0	79.8865	-69.038	79.962501	-69.086742	322.357221	-85.457085	279.70295655	-33.37204199	53.6181	55782.8380324074	2011-08-09 20:06:46	55789.4030555556	2011-08-16 09:40:24	806026010	347.5681	350	347.5681	347.5761	0	347.5761	2	2	0	2	1	0	0	355.0724	355.0724	395.8115	7	PROCESSED	57602.9665740741	2016-08-02 23:11:52	55652	2011-04-01 00:00:00	55802.468900463	2011-08-29 11:15:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061102	We propose two relatively deep observations of the young ejecta-dominated supernova remnants 0509-67.5 and 0519-69.0 in the Large Magellanic Cloud. Our goal is to seek line emission from the trace elements Mn and Cr in these remnants of Type Ia supernovae, and to measure the corresponding abundances using calculated atomic data. The relative masses of Mn and Cr produced in Type Ia supernovae are a diagnostic of the initial metallicity of the progenitor system. Of the supernovae that produced these two remnants, one had a normal luminosity, while the other was over-luminous. Together with existing data for another LMC Ia remnant, N103B, which shows evidence for circumstellar interactions, these observations will provide a broad sample of the variety seen in Ia events.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	UNA HWANG		USA	6	AO6-LP	ABUNDANCES OF CR AND MN AND THE PROGENITOR METALLICITY IN TWO TYPE IA MAGELLANIC CLOUD SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806026010/	Quick Look
771	ABELL 773	139.6885	51.8172	138.816003	52.028068	124.747961	34.198508	165.93230971	43.4884399	276.9986	55682.3638888889	2011-05-01 08:44:00	55683.2105902778	2011-05-02 05:03:15	806027010	42.5779	50	42.5859	42.5859	0	42.5779	1	1	0	1	1	0	0	32.7052	32.7052	73.1439	0	PROCESSED	57601.9080555556	2016-08-01 21:47:36	55652	2011-04-01 00:00:00	55697.2644560185	2011-05-16 06:20:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806027010/	Quick Look
772	ABELL 1068	159.9611	39.9499	159.238834	40.210787	145.421786	28.986121	179.20513519	59.95740225	130.001	55864.5464583333	2011-10-30 13:06:54	55865.764849537	2011-10-31 18:21:23	806028040	51.1493	50	51.1573	51.1493	0	51.1653	2	2	0	2	1	0	0	46.5701	46.5701	105.2498	0	PROCESSED	57603.6525810185	2016-08-03 15:39:43	55652	2011-04-01 00:00:00	55879.1651967593	2011-11-14 03:57:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806028040/	Quick Look
773	COMA E5	196.4286	27.8904	195.829087	28.157796	182.91784	31.908863	47.28907584	86.74411283	279.9981	55730.3360416667	2011-06-18 08:03:54	55730.7848726852	2011-06-18 18:50:13	806034010	18.2706	20	18.2706	18.2946	0	18.2786	1	1	0	1	1	0	0	15.0751	15.0751	38.7599	0	PROCESSED	57602.3384259259	2016-08-02 08:07:20	55652	2011-04-01 00:00:00	55770.1405324074	2011-07-28 03:22:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806034010/	Quick Look
774	COMA NW4	194.43	28.912	193.827069	29.181931	180.525216	32.025522	85.44172027	87.7408795	319.999	55732.9798611111	2011-06-20 23:31:00	55733.468912037	2011-06-21 11:15:14	806041010	21.1196	20	21.1236	21.1434	0	21.1196	2	2	0	2	1	0	0	21.5915	21.5915	42.246	0	PROCESSED	57602.3778819444	2016-08-02 09:04:09	55652	2011-04-01 00:00:00	55768.2688888889	2011-07-26 06:27:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806041010/	Quick Look
775	NGC5866	226.5977	55.7554	226.254302	55.947234	186.820283	67.076445	92.03719886	52.50531538	352.5583	55701.1230092593	2011-05-20 02:57:08	55703.3466898148	2011-05-22 08:19:14	806053010	101.8346	100	101.8426	101.8346	0	101.8426	2	2	0	2	1	0	0	94.7812	94.7812	192.0718	2	PROCESSED	57602.140787037	2016-08-02 03:22:44	56102	2012-06-24 00:00:00	55735.3197800926	2011-06-23 07:40:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061502	An existing Chandra observation indicates hot gas in the S0 galaxy NGC5866 has a supersolar iron abundance and an unusually low O/Fe ratio. The galaxy is also rich in molecular gas and shows distinct vertical dusty filaments, which most likely represent cold gas blown out by SNe from the disk. We herein propose a 100ks Suzaku observation of it to better measure the hot gas properties and its spatial distribution. The energy resolution and counting statistics of the observation will enable us to greatly improve the measurement of the abundances. By further comparing such measurements among galaxies of different cold gas contents, we will investigate the effect of cold/hot gas interaction on the dynamics of the hot gas, as well as its thermal and chemical properties.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JIANG-TAO LI		USA	6	AO6	X-RAY SPECTROSCOPY OF STELLAR FEEDBACK PROCESSES IN A COOL GAS-RICH S0 GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806053010/	Quick Look
776	SPT-CL J2341-5119	355.3013	-51.333	354.629905	-51.610408	330.126015	-44.109465	326.93544545	-62.39708341	56.9213	55703.3602662037	2011-05-22 08:38:47	55706.0800810185	2011-05-25 01:55:19	806072010	100.2347	100	100.2427	100.2347	0	100.2507	2	2	0	2	1	0	0	88.2081	88.2081	234.9799	3	PROCESSED	57602.1463310185	2016-08-02 03:30:43	56092	2012-06-14 00:00:00	55725.3016550926	2011-06-13 07:14:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061531	We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ERIC MILLER		USA	6	AO6	THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806072010/	Quick Look
777	RCS044406-2820.4	71.0221	-28.343	70.523595	-28.434713	63.530115	-50.056858	228.67801491	-39.02616141	99.3268	55827.6316319444	2011-09-23 15:09:33	55828.8751736111	2011-09-24 21:00:15	806080010	50.6723	50	50.6723	50.6723	0	50.6723	2	2	0	2	1	0	0	41.9027	41.9027	107.4318	3	PROCESSED	57603.2531134259	2016-08-03 06:04:29	56222	2012-10-22 00:00:00	55854.3160300926	2011-10-20 07:35:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061533	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AMALIA HICKS		USA	6	AO6	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806080010/	Quick Look
778	A3526	192.0509	-41.0558	191.361267	-40.783129	208.811762	-32.67802	302.27518183	21.81182444	109.9986	55942.2296990741	2012-01-16 05:30:46	55942.6807291667	2012-01-16 16:20:15	806084010	16.9645	10	16.9645	16.9645	0	16.9645	2	2	0	2	1	0	0	12.6605	12.6605	38.9639	0	PROCESSED	57604.361875	2016-08-04 08:41:06	56331	2013-02-08 00:00:00	55960.1781712963	2012-02-03 04:16:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806084010/	Quick Look
779	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
780	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
781	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
782	N4438 TAIL	186.7653	12.9509	186.13191	13.227515	180.954769	14.552434	279.81897455	74.71807646	119.2941	56636.4959259259	2013-12-10 11:54:08	56639.0884259259	2013-12-13 02:07:20	808045010	102.7738	100	102.7738	102.7738	0	102.7738	2	2	0	2	1	0	0	92.8342	92.8342	223.962	2	PROCESSED	57613.6203587963	2016-08-13 14:53:19	57016	2014-12-25 00:00:00	56650.8089583333	2013-12-24 19:24:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080059	We propose a 100 ks XIS observation to the Halpha/X-ray filament connecting N4438 and M86 in the Virgo cluster. Our main objective is to probe conclusively the OVII line which is marginally detected with the XMM-Newton. If established, by employing line diagnostic and non-equilibrium ionization analysis, we will be able to determine the ionization temperature and elapsed timescale of the multi-phase ISM stripped from N4438, and give constraint on the thermal conductivity and metal enrichment of the ICM.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	LIYI GU		JAP	8	AO8	A SUZAKU OBSERVATION OF ONGOING IONIZATION OF ISM IN THE VIRGO CLUSTER ICM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808045010/	Quick Look
783	SDSS J0906+0301	136.6571	3.0284	136.006	3.229773	138.178094	-12.954149	226.89088068	31.22930355	109.9836	56253.2318981482	2012-11-22 05:33:56	56253.846099537	2012-11-22 20:18:23	807059010	21.7148	20	21.7228	21.7148	0	21.7228	2	2	0	2	1	0	0	20.632	20.632	53.066	0	PROCESSED	57608.0815972222	2016-08-08 01:57:30	56702	2014-02-14 00:00:00	56336.4694328704	2013-02-13 11:15:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071512	Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ERIC MILLER		USA	7	AO7	FINDING FOSSIL GROUPS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807059010/	Quick Look
784	SDSS J1431+0047	217.7608	0.788	217.122744	1.009037	215.129123	14.8431	349.30444711	54.43383912	287.7594	56140.9857291667	2012-08-01 23:39:27	56141.454375	2012-08-02 10:54:18	807062010	22.3553	20	22.371	22.3553	0	22.363	1	1	0	1	1	0	0	16.5809	16.5809	40.4799	1	PROCESSED	57606.7190740741	2016-08-06 17:15:28	56528	2013-08-24 00:00:00	56162.1265972222	2012-08-23 03:02:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071512	Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ERIC MILLER		USA	7	AO7	FINDING FOSSIL GROUPS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807062010/	Quick Look
785	ABELL 2597	351.4175	-11.9496	350.767566	-12.224675	347.389222	-7.579212	65.78537526	-64.80325971	249.1017	56261.057650463	2012-11-30 01:23:01	56262.3299768518	2012-12-01 07:55:10	807073010	51.0526	50	51.0566	51.0674	0	51.0526	2	2	0	2	1	0	0	46.3613	46.3613	109.9139	1	PROCESSED	57608.180462963	2016-08-08 04:19:52	56018	2012-04-01 00:00:00	56278.743587963	2012-12-17 17:50:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073010/	Quick Look
786	HYDRA A FAR N	139.5397	-11.7599	138.936601	-11.549023	146.034406	-26.083857	242.64361193	25.31151573	300.0007	56083.9377430556	2012-06-05 22:30:21	56085.1452662037	2012-06-07 03:29:11	807089010	41.276	40	41.284	41.284	0	41.276	2	2	0	2	1	0	0	38.1727	38.1727	104.3117	1	PROCESSED	57605.6201851852	2016-08-05 14:53:04	56465	2013-06-22 00:00:00	56098.4661689815	2012-06-20 11:11:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072020	Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DOMINIQUE ECKERT		EUR	7	AO7	MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807089010/	Quick Look
787	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
788	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
789	A399&A401 FILAMENT	44.5739	13.3044	43.887717	13.104923	46.011939	-3.472452	164.23302583	-39.1861165	71.9992	56522.5065972222	2013-08-18 12:09:30	56523.421724537	2013-08-19 10:07:17	808005010	42.1655	40	42.1655	42.1655	0	42.1655	1	1	0	1	1	0	0	40.981	40.981	79.0638	2	PROCESSED	57612.3602083333	2016-08-12 08:38:42	56956	2014-10-26 00:00:00	56587.6829398148	2013-10-22 16:23:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080004	To investigate (i)the influence of the merging event on IntraCluster Medium (ICM), We propose 40 ks+50 ks ~2 =140 ks observations of the linked region between Abell 399 and Abell 401. A399 (z=0.0724) and A401 (z=0.0737) are expected be in the initial phase of a cluster merger. With Suzaku fs high sensitivity observations, we will (i)determine the ICM physical conditions by measuring the temperature and density distribution, (ii) characterize the dynamical state of the cluster linked region, (iii) confirm the presence of a shock front predicted by numerical simulations. Our study will reveal the nature of initial phase of merging event of clusters of galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHITAKA ISHISAKI		JAP	8	AO8	MORPHOLOGY AND PHYSICAL PROPERTIES OF SHOCKED GAS BY MAJOR MERGER IN THE LINKED REGION OF ABELL 399 AND ABELL 401	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808005010/	Quick Look
790	A2255_SE	258.2963	63.8192	258.210545	63.875842	203.735886	84.382935	93.63129587	34.92006939	200.0025	56613.9474537037	2013-11-17 22:44:20	56615.3084953704	2013-11-19 07:24:14	808040010	64.733	60	64.741	64.741	0	64.733	2	2	0	2	1	0	0	64.8865	64.8865	117.5879	1	PROCESSED	57613.3519097222	2016-08-13 08:26:45	57029	2015-01-07 00:00:00	56653.6890046296	2013-12-27 16:32:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080047	We propose to obtain high-quality X-ray spectra of two subcluster regions in A2255 aiming at detection of supersonic motion of the intracluster gas. Previous optical and X-ray observations suggest that A2255 is indeed in the process of merging and subclusters have high velocities relative to the main cluster. Utilizing the high-sensitivity Suzaku spectroscopy, the line-of-sight velocity of the X-ray emitting gas can be measured from the Doppler shift of iron-K lines. With additional 40ks/80ks observations of the NW/SE subclusters, we expect to detect significant bulk velocities for the first time in this cluster. This will enhance our understanding of the 3-dimensional structure of the object including line-of-sight gas velocities and the cluster dynamical evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	HIROKO YOSHIDA		JAP	8	AO8	MAPPING GAS MOTIONS IN THE MERGING CLUSTER A2255	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808040010/	Quick Look
791	3C390.3_VICINITY_2	284.1264	79.7065	284.963939	79.636578	79.391227	76.323687	111.42410994	26.43157038	239.9994	56608.493900463	2013-11-12 11:51:13	56609.4897222222	2013-11-13 11:45:12	808047010	52.8856	50	52.9066	52.8936	0	52.8856	2	2	0	2	1	0	0	48.4013	48.4013	86.0319	0	PROCESSED	57613.3036111111	2016-08-13 07:17:12	56991	2014-11-30 00:00:00	56625.7010648148	2013-11-29 16:49:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080060	We propose for observations of the vicinities of 3C 390.3 and Fairall 9, in order to constrain the origins of 'excess' emission in the soft X-ray diffuse background observed with Suzaku and to confirm its possible relation to high velocity clouds (HVCs). We have been observing blank-skies in many directions and studying a oxygen emission from the Galactic halo. Intensities of the emission show a uniform value in most of directions; however in some directions we can see an excess, which possibly originate to a blob-like high density gas and/or a distribution of HVCs. By conducting a joint analysis of absorption and emission lines, we can characterize the roots of the excess emission. Moreover, the joint analysis even constraints a density of the origins, which has never been done until now.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KAZUHIRO SAKAI		JAP	8	AO8	DO HIGH VELOCITY CLOUDS HEAT THE HALO OF OUR GALAXY?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808047010/	Quick Look
792	NGC1550_45OFFSET_E	65.5544	2.4106	64.903424	2.293944	64.093741	-18.859585	191.40103429	-31.31407553	260.0002	56696.1115393518	2014-02-08 02:40:37	56697.3543634259	2014-02-09 08:30:17	808060010	53.0496	50	53.0496	53.0496	0	53.0496	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57613.8049421296	2016-08-13 19:19:07	57075	2015-02-22 00:00:00	56709.7114351852	2014-02-21 17:04:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080110	We propose to study the entropy profile and the metal enrichment process of the fossil group, NGC 1550 with total 170 ksec observations. NGC 1550 is a bright nearby group (z=0.0124), and classified as a fossil group which has no bright galaxies except for a central elliptical galaxy. Fossil groups, therefore, are a very useful system for investigating how the ICM metals have been enriched from galaxies. On the other hand, it is known that the entropy of groups has a several times larger than that of clusters within ~0.2 r180, and has similar value to clusters at 0.5 r180. However, in r > 0.5 r180 region, the entropy profile of groups has not been observed yet, while those of clusters have shown a flatter slope than the expected value from simulations in the Suzaku results.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TORU SASAKI		JAP	8	AO8	STUDY OF THE ENTROPY PROFILE AND THE METAL ENRICHMENT PROCESS IN THE FOSSIL GROUP, NGC~1550	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808060010/	Quick Look
793	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
794	THE MOON	141.5744	9.879	140.90311	10.096072	140.776608	-4.942339	222.40545014	38.80103529	285.4041	56784.4506712963	2014-05-07 10:48:58	56784.5827662037	2014-05-07 13:59:11	809001080	5.6107	45	5.6107	5.6107	0	5.6107	1	1	0	1	1	0	0	5.507	5.507	11.3919	0	PROCESSED	57615.0708217593	2016-08-15 01:41:59	57220	2015-07-17 00:00:00	56854.5770717593	2014-07-16 13:50:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001080/	Quick Look
795	THE MOON	22.6503	9.5807	21.992046	9.323163	24.491955	0.094055	138.76659478	-52.08288303	73.7999	56856.8890277778	2014-07-18 21:20:12	56857.0196412037	2014-07-19 00:28:17	809001130	5.3017	45	5.3017	5.3017	0	5.3017	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.4036574074	2016-08-15 09:41:16	57267	2015-09-02 00:00:00	56902.5802314815	2014-09-02 13:55:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001130/	Quick Look
796	THE MOON	26.0744	9.9879	25.412732	9.737134	27.784882	-0.749126	143.76867514	-50.73288629	73.7996	56857.1528472222	2014-07-19 03:40:06	56857.2765856482	2014-07-19 06:38:17	809001150	3.9169	45	3.9169	3.9169	0	3.9169	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.4069097222	2016-08-15 09:45:57	57235	2015-08-01 00:00:00	56869.6125925926	2014-07-31 14:42:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001150/	Quick Look
797	THE MOON	147.1957	8.7504	146.531357	8.983511	146.407447	-4.210959	227.18440299	43.16589995	105.6994	56975.9388541667	2014-11-14 22:31:57	56976.0626388889	2014-11-15 01:30:12	809001260	6.33	45	6.33	6.442	0	6.442	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7804513889	2016-08-16 18:43:51	57359	2015-12-03 00:00:00	56992.418587963	2014-12-01 10:02:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001260/	Quick Look
798	THE MOON	333.6436	-6.6185	332.98809	-6.867271	333.149604	3.9961	54.50784287	-47.51853169	249.2061	56990.1023958333	2014-11-29 02:27:27	56990.2084837963	2014-11-29 05:00:13	809001300	3.8788	45	3.8828	3.8788	0	3.8868	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.4075115741	2016-08-17 09:46:49	57415	2016-01-28 00:00:00	57049.4536805556	2015-01-27 10:53:18	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001300/	Quick Look
799	THE MOON	339.1671	-5.6557	338.516198	-5.915354	338.624224	2.887463	60.63287277	-51.42821416	248.2317	56990.4856828704	2014-11-29 11:39:23	56990.608587963	2014-11-29 14:36:22	809001330	6.3646	45	6.3646	6.3646	0	6.3646	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.4115856482	2016-08-17 09:52:41	57415	2016-01-28 00:00:00	57006.4031018518	2014-12-15 09:40:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001330/	Quick Look
800	RXJ1159+5531 E	180.1946	55.5211	179.553068	55.799424	150.053445	49.203071	137.37799324	60.16358606	301.575	56806.5416550926	2014-05-29 12:59:59	56808.2502430556	2014-05-31 06:00:21	809063010	99.1618	100	99.1778	99.1618	0	99.1778	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.1713657407	2016-08-15 04:06:46	57234	2015-07-31 00:00:00	56866.7150925926	2014-07-28 17:09:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091521	In contrast to some recent observations of cluster outskirts, for RXJ1159+5531, we obtain measurements of the gas fraction and entropy at the virial radius that are fully consistent with gravity-only structure formation simulations. Our preliminary Suzaku analysis of an opposite direction shows similar results. This encouraging consistency suggests that we may see little azimuthal variation in the gas properties for this unusually relaxed system. To verify and also benefit from the relaxed state of this benchmark system, we propose complementary Suzaku observations of RXJ1159+5531 in the other two directions. Simultaneously fitting these pointings would provide us the metal abundance ratios at large radii in order to place broad constrains on the enrichment history of group scale systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YUANYUAN SU		USA	9	AO9	MAPPING A BENCHMARK RELAXED POOR CLUSTER OUT TO ITS VIRIAL RADIUS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809063010/	Quick Look
801	ABELL 98-CENTER	11.6247	20.5572	10.963731	20.284211	18.829002	14.307964	121.3687084	-42.29955696	80.8972	56837.6648726852	2014-06-29 15:57:25	56839.2014236111	2014-07-01 04:50:03	809077010	60.781	60	60.781	60.917	0	60.925	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.3554282407	2016-08-15 08:31:49	56748	2014-04-01 00:00:00	56854.7844212963	2014-07-16 18:49:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091525	We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	SCOTT RANDALL		USA	9	AO9	EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809077010/	Quick Look
802	ABELL 98-WEST	11.3131	20.6695	10.652564	20.396219	18.599995	14.528185	120.97936172	-42.17879703	80.8359	56841.9624537037	2014-07-03 23:05:56	56844.7606712963	2014-07-06 18:15:22	809079010	96.6924	100	96.6924	100.6438	0	100.6598	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.3882638889	2016-08-15 09:19:06	56748	2014-04-01 00:00:00	56881.441724537	2014-08-12 10:36:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091525	We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	SCOTT RANDALL		USA	9	AO9	EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809079010/	Quick Look
803	MKW8	220.1793	3.4582	219.549704	3.671881	216.616533	18.149831	355.49716412	54.76401984	291.2239	56859.4682986111	2014-07-21 11:14:21	56859.7009259259	2014-07-21 16:49:20	809101010	10.412	10	10.412	10.488	0	10.4956	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.4174305556	2016-08-15 10:01:06	57239	2015-08-05 00:00:00	56873.5532523148	2014-08-04 13:16:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809101010/	Quick Look
804	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
805	EN2-109	248.6774	40.3802	248.257276	40.482344	234.834061	61.240527	64.11782178	42.55568423	145.2754	55927.5063425926	2012-01-01 12:09:08	55929.8577314815	2012-01-03 20:35:08	806075010	108.616	100	108.632	108.616	0	108.64	2	2	0	2	1	0	0	0.571	0.571	0.5729	0	PROCESSED	57604.2767592593	2016-08-04 06:38:32	56065	2012-05-18 00:00:00	55946.1449537037	2012-01-20 03:28:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061532	We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	6	AO6	OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806075010/	Quick Look
806	ES1-230	9.1906	-44.1805	8.591944	-44.455632	346.325718	-43.236883	311.80619624	-72.69400023	239.5046	55907.020787037	2011-12-12 00:29:56	55907.8925694444	2011-12-12 21:25:18	806076010	44.8024	40	44.8024	44.8024	0	44.8024	2	2	0	2	1	0	0	52.0193	52.0193	75.3199	0	PROCESSED	57604.1212037037	2016-08-04 02:54:32	56065	2012-05-18 00:00:00	55920.9678587963	2011-12-25 23:13:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061532	We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	6	AO6	OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806076010/	Quick Look
807	FORNAX CLUSTER NORTH	54.7022	-35.2276	54.222066	-35.389468	38.999643	-52.605839	236.33819165	-53.57399329	245.0013	53740.3046990741	2006-01-05 07:18:46	53740.493275463	2006-01-05 11:50:19	800002010	7.7635	80	7.7635	7.7635	7.7635	7.7635	1	1	1	1	1	0	0	8.2708	8.2708	16.2719	0	PROCESSED	57532.6205324074	2016-05-24 14:53:34	54247	2007-05-27 00:00:00	54039.6718518518	2006-10-31 16:07:28	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001018	The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	0	SWG	MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800002010/	Quick Look
808	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
809	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
810	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
811	A262 NE4	28.8115	37.1901	28.070704	36.945344	40.33412	23.695949	136.79382783	-23.95810874	249.9999	56704.7992476852	2014-02-16 19:10:55	56705.5321064815	2014-02-17 12:46:14	808111010	30.9305	30	30.9625	30.9305	0	30.9625	1	1	0	1	1	0	0	27.8027	27.8027	63.3119	2	PROCESSED	57613.8474652778	2016-08-13 20:20:21	57085	2015-03-04 00:00:00	56719.7343981482	2014-03-03 17:37:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	083002	We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	NORBERT WERNER	JUS	8	AO8	OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808111010/	Quick Look
812	A1060 OFFSET	159.5124	-27.532	158.922997	-27.271679	173.074389	-33.196781	269.88117164	26.64663217	96.4857	53694.9817708333	2005-11-20 23:33:45	53696.6231365741	2005-11-22 14:57:19	800004010	52.4025	60	52.4025	53.2025	52.4185	52.5385	2	2	2	2	1	0	0	46.2039	46.2039	141.8018	1	PROCESSED	57528.0764583333	2016-05-20 01:50:06	54247	2007-05-27 00:00:00	54038.1216666667	2006-10-30 02:55:12	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001021	A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI		JAP	0	SWG	OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800004010/	Quick Look
813	COMA SUBHALO4	193.8668	27.5167	193.260337	27.78729	180.744108	30.556584	56.62578598	89.02439779	314.9971	56453.5916666667	2013-06-10 14:12:00	56454.1370717593	2013-06-11 03:17:23	808022010	23.8091	20	23.8091	23.8331	0	23.8171	2	2	0	2	1	0	0	19.6195	19.6195	47.1139	0	PROCESSED	57611.5223958333	2016-08-11 12:32:15	56830	2014-06-22 00:00:00	56464.6326041667	2013-06-21 15:10:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080023	We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NOBUHIRO OKABE		JAP	8	AO8	SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808022010/	Quick Look
814	A426VIR E	49.1256	42.621	48.293128	42.437331	58.306623	23.574763	149.42807458	-12.66566367	271.4976	56709.0457986111	2014-02-21 01:05:57	56709.5683101852	2014-02-21 13:38:22	808086010	25.3703	25	25.3823	25.3703	0	25.3703	2	2	0	2	1	0	0	24.322	24.322	45.14	1	PROCESSED	57613.8778935185	2016-08-13 21:04:10	57141	2015-04-29 00:00:00	56764.7643171296	2014-04-17 18:20:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081526	Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ONDREJ URBAN		USA	8	AO8	SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808086010/	Quick Look
815	A85	10.4739	-9.4292	9.841504	-9.703266	5.843917	-12.80705	115.23010576	-72.15810594	248.2856	54105.4020023148	2007-01-05 09:38:53	54108.0557175926	2007-01-08 01:20:14	801041010	99.2012	100	99.2012	99.2012	0	99.2012	2	2	0	2	1	0	0	84.8139	84.8139	229.2421	2	PROCESSED	57536.5180671296	2016-05-28 12:26:01	54735	2008-09-26 00:00:00	54132.9388773148	2007-02-01 22:31:59	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010088	We propose observations of A2199 and A85 clusters of galaxies with an each exposure time of 100 ks, in order to search for excess hard X-ray emission, to constrain the spectral shape, and to discuss the origin of the hard X-ray emission. Both are listed as the clusters which are detected non-thermal emission signal with 2 sigma confidence level by Beppo SAX PDS detector. In addition, these two clusters only have features of brighter X-ray flux, good size, relatively cool ICM temperature, and including no bright member AGNs. Therefore they are suitable target samples for our observational purpose about estimation photon index and flux for the excess hard X-ray emission with high significance wherever possible.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	RYO SHIBATA		JAP	1	AO1	SEARCH FOR EXCESS HARD X-RAY EMISSION FROM A2199 AND A85 GALAXY CLUSTERS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801041010/	Quick Look
816	PERSEUS OFFSET-G	50.3247	41.3807	49.497049	41.201455	58.859538	22.134977	150.89015689	-13.2150361	270.0001	55596.3541550926	2011-02-04 08:29:59	55596.8335648148	2011-02-04 20:00:20	805047010	19.6768	25	19.7008	19.6928	0	19.6768	2	2	0	2	1	0	0	13.192	13.192	41.4119	1	PROCESSED	57600.8412731482	2016-07-31 20:11:26	55979	2012-02-22 00:00:00	55613.0840856482	2011-02-21 02:01:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050093	We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TAKAYUKI TAMURA		JAP	5	AO5	MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805047010/	Quick Look
817	ABELL 115 OFFSET	13.7779	26.1853	13.1056	25.914555	23.090334	18.655077	123.95957255	-36.67911837	45.0019	55399.3766666667	2010-07-22 09:02:24	55401.6050115741	2010-07-24 14:31:13	805078010	101.8065	100	101.8065	101.8065	0	101.8065	2	2	0	2	1	0	0	91.1134	91.1134	192.5058	3	PROCESSED	57552.7084259259	2016-06-13 17:00:08	55779	2011-08-06 00:00:00	55413.4333449074	2010-08-05 10:24:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051521	We propose central and offset pointed observations of the strongly merging ``double'' cluster A115 to study the properties of the intracluster gas at the virial radius. Ultimately, the results can be compared with results from both relaxed and other merging systems to determine the effects of mergers on the extended gas halos of clusters (e.g., departures from hydrostatic equilibrium, and the level of non-thermal pressure support). Additionally, we will verify the presence of hard X-ray emission between the subclusters, marginally detected in Chandra observations, accurately measure its temperature, and determine its origin by confirming it as hot thermal (shock heated gas) or non-thermal (shock or turbulent accelerated particles) emission.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	SCOTT RANDALL		USA	5	AO5	THE EXTENDED ATMOSPHERES OF STRONGLY MERGING GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805078010/	Quick Look
818	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
819	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
820	ANTLIA EB	160.0852	-35.3304	159.51241	-35.06908	178.137624	-39.871032	274.84198608	20.29194272	279.6006	56096.5981828704	2012-06-18 14:21:23	56097.8197106482	2012-06-19 19:40:23	807071010	45.7475	45	45.7635	45.7475	0	45.7635	2	2	0	2	1	0	0	40.3619	40.3619	105.536	1	PROCESSED	57605.7231481482	2016-08-05 17:21:20	56477	2013-07-04 00:00:00	56111.1019328704	2012-07-03 02:26:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071521	We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	7	AO7	MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807071010/	Quick Look
821	J2218.2-0350	334.573	-3.8385	333.923892	-4.08927	335.019924	6.258076	58.63251599	-46.67973864	268.0005	56260.6621527778	2012-11-29 15:53:30	56261.0523148148	2012-11-30 01:15:20	807084010	15.7671	15	15.7751	15.7671	0	15.7831	2	2	0	2	1	0	0	11.9145	11.9145	33.7079	0	PROCESSED	57608.1412384259	2016-08-08 03:23:23	56644	2013-12-18 00:00:00	56275.6610300926	2012-12-14 15:51:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072018	We propose to observe the three clusters of galaxies J2218.2-0350, J2218.6-0346 and J2218.8-0258 with exposure times of 15, 25 and 35 ks respectively. These clusters are part of a structure of four linearly aligned clusters, separated from each other by 4 to 10 Mpc. We will accurately determine their masses and orientation. This will allow us to fully map the tidal force field of the structure, which is the prime force behind the formation of filaments in the cosmic web. We will study the effects of cluster mass, separation and mutual orientation on the filamentary structure of the cosmic web and on the evolution of galaxies therein.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	E.G. PATRICK BOS		EUR	7	AO7	CLUSTERS AND THE COSMIC WEB	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807084010/	Quick Look
822	FORNAX A EAST LOBE	51.0149	-37.2799	50.539015	-37.455999	33.113805	-53.302729	240.23704173	-56.41225665	91.5022	56506.6358564815	2013-08-02 15:15:38	56510.623125	2013-08-06 14:57:18	808043010	151.4626	150	151.4866	151.4626	0	151.4946	2	2	0	2	1	0	0	134.0942	134.0942	344.4353	3	PROCESSED	57612.2277777778	2016-08-12 05:28:00	56955	2014-10-25 00:00:00	56587.7734259259	2013-10-22 18:33:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080056	We propose Suzaku observations of the Fornax A east radio lobe and the background region. In previous cycles, we observed the west lobe and detected thermal extended gas for the first time, in addition to the non-thermal emission known for decades (Seta PhD thesis, 2012). In order to reveal the relation between the AGN jet and the thermal gas, the additional data in the opposite side of the lobe is critically important. We aim to detect the thermal gas in the eastern lobe, too, and investigate the spatial difference of its temperature and surface brightness.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROMI SETA		JAP	8	AO8	COMPLETING THE MAPPING OBSERVATION OF FORNAX A RADIO LOBE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808043010/	Quick Look
823	ABELL 3112	49.4972	-44.2507	49.062824	-44.43238	25.520697	-58.972198	252.95338075	-56.0704995	43.5006	56468.5418171296	2013-06-25 13:00:13	56469.5834259259	2013-06-26 14:00:08	808068020	65.3977	200	65.4057	65.4057	0	65.3977	2	2	0	2	1	0	0	54.0744	54.0744	89.9838	1	PROCESSED	57611.633912037	2016-08-11 15:12:50	56848	2014-07-10 00:00:00	56481.7677083333	2013-07-08 18:25:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081522	The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ESRA BULBUL		USA	8	AO8	CHEMICAL EVOLUTION HISTORY OF A COOL CORE CLUSTER A3112 OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808068020/	Quick Look
824	THE MOON	148.554	8.0651	147.892313	8.301757	147.907786	-4.401986	228.92553687	43.99318882	105.699	56976.0638541667	2014-11-15 01:31:57	56976.1876388889	2014-11-15 04:30:12	809001270	5.9536	45	5.9536	5.9616	0	5.9616	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7826967593	2016-08-16 18:47:05	57359	2015-12-03 00:00:00	56992.4196527778	2014-12-01 10:04:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001270/	Quick Look
825	CEN_A_LOBE_N3	200.614	-42.0794	199.886702	-41.818146	216.080144	-30.721221	309.06646515	20.4225822	293.3211	56862.6955439815	2014-07-24 16:41:35	56864.2709722222	2014-07-26 06:30:12	809004010	51.4894	50	51.4894	51.4894	0	51.4894	2	2	0	2	1	0	0	10.6384	10.6384	21.48	0	PROCESSED	57615.4562384259	2016-08-15 10:56:59	57242	2015-08-08 00:00:00	56875.2082175926	2014-08-06 04:59:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090021	In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	HIROMI SETA		JAP	9	AO9	MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809004010/	Quick Look
826	CENCL OFFSET1	192.2015	-41.4461	191.510562	-41.173577	209.146138	-32.971575	302.40210867	21.42294125	106.2765	53732.1811689815	2005-12-28 04:20:53	53733.2502199074	2005-12-29 06:00:19	800015010	44.8802	40	44.8962	44.9042	44.8802	44.9196	2	2	2	2	1	0	0	37.2267	37.2267	92.3478	2	PROCESSED	57532.5827893518	2016-05-24 13:59:13	54247	2007-05-27 00:00:00	54039.5403472222	2006-10-31 12:58:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001070	A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	0	SWG	OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800015010/	Quick Look
827	N1550_CENTER	64.9488	2.4105	64.297881	2.291179	63.464463	-18.753248	191.00239213	-31.81480775	89.9981	54694.185474537	2008-08-16 04:27:05	54696.3009143518	2008-08-18 07:13:19	803017010	83.2702	80	83.7102	83.2702	0	83.7102	2	2	0	2	1	0	0	64.8874	64.8874	182.756	4	PROCESSED	57543.367974537	2016-06-04 08:49:53	55080	2009-09-06 00:00:00	54713.2652546296	2008-09-04 06:21:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030070	We propose 80 and 40 ksec observations of the central and 30' offset regions of fossil group, NGC 1550, respectively, to study metal abundance distributions of O to Fe to the ~0.2 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. A comparison of O to Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. In addition, a comparison of the metal distributions of the nominal group of galaxies and fossil group will show us how much metal production and diffusion processes differ with system.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KOSUKE SATO		JAP	3	AO3	OBSERVATIONS OF METAL DISTRIBUTIONS IN FOSSIL GROUP: NGC1550	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803017010/	Quick Look
828	A262 NE3	28.6712	36.9514	27.931716	36.706321	40.12197	23.517818	136.74540455	-24.21802206	250.0003	56703.8826388889	2014-02-15 21:11:00	56704.7987731482	2014-02-16 19:10:14	808110010	40.4903	40	40.5134	40.4903	0	40.4966	2	2	0	2	1	0	0	34.2624	34.2624	69.899	1	PROCESSED	57613.8476041667	2016-08-13 20:20:33	57081	2015-02-28 00:00:00	56715.76	2014-02-27 18:14:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	083002	We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA	NORBERT WERNER	JUS	8	AO8	OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808110010/	Quick Look
829	A963E	154.4148	39.0556	153.674896	39.305871	141.440839	26.400688	182.51717965	55.95361494	109.3314	54427.8082060185	2007-11-23 19:23:49	54428.4745833333	2007-11-24 11:23:24	802011010	29.0825	25	29.0825	29.0825	0	29.0825	2	2	0	2	1	0	0	24.4699	24.4699	57.5679	0	PROCESSED	57540.5746412037	2016-06-01 13:47:29	54804	2008-12-04 00:00:00	54434.1859837963	2007-11-30 04:27:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020018	We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 10% precision in a few arcmin scale, which has not been done before to any cluster. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO HATTORI		JAP	2	AO2	TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802011010/	Quick Look
830	NGC 253 OFFSET	12.0926	-25.0475	11.478671	-25.320084	0.364314	-27.643554	104.44696227	-87.8082396	247.2843	54829.0152430556	2008-12-29 00:21:57	54830.2502430556	2008-12-30 06:00:21	803004010	56.7104	50	56.7104	56.7104	0	56.7104	2	2	0	2	1	0	0	51.3026	51.3026	106.6718	1	PROCESSED	57545.0814351852	2016-06-06 01:57:16	55213	2010-01-17 00:00:00	54847.4571296296	2009-01-16 10:58:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030027	Suzaku observations of a hot halo of nearby, edge-on starburst galaxy NGC 253 are proposed. The low background and high energy resolution of Suzaku XIS is the best tool to study the low surface brightness emission like halo emission around galaxies. In addition, we will eliminate the contamination from the the point source by XMM-Newton and the Galactic hot emission by an offset observation. The temperature and pressure structure and the chemical composition in the bright halo will reveal the physical condition and the dynamics of the galaxy outflow to the intergalactic space.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORIKO YAMASAKI		JAP	3	AO3	SUZAKU OBSERVATION OF A BRIGHTEST STARBURST GALAXY NGC 253	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803004010/	Quick Look
831	NGC 1550-OFFSET1	65.1493	2.6086	64.497489	2.490158	63.709607	-18.593747	190.9426677	-31.53770965	265.5852	54901.8171875	2009-03-11 19:36:45	54903.699525463	2009-03-13 16:47:19	803046010	66.8274	62	66.8274	66.8274	0	66.8274	2	2	0	2	1	0	0	60.9307	60.9307	162.6001	2	PROCESSED	57545.8588541667	2016-06-06 20:36:45	55329	2010-05-13 00:00:00	54917.3952314815	2009-03-27 09:29:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031422	We propose a set of two 19 arcmin offset observations of the galaxy groups NGC 1550 and MKW 4 to measure spatially resolved densities, temperatures and iron abundances out to r_500. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to their brightness, regularity and low temperature, the two objects are ideal candidates for an offset observation of their peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	FABIO GASTALDELLO		USA	3	AO3	THE OUTSKIRTS OF NGC 1550 AND MKW 4	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803046010/	Quick Look
832	NGC741MOSAICE_P2	29.9595	5.5362	29.305812	5.294206	29.82553	-6.270862	152.32010482	-53.38732445	71.7775	55054.083912037	2009-08-11 02:00:50	55054.3334837963	2009-08-11 08:00:13	804052020	12.7341	10	12.7341	12.7421	0	12.7421	1	1	0	1	1	0	0	12.0159	12.0159	21.5599	0	PROCESSED	57548.1149884259	2016-06-09 02:45:35	55448	2010-09-09 00:00:00	55081.2532060185	2009-09-07 06:04:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052020/	Quick Look
833	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
834	A1750R	202.8691	-2.0415	202.224847	-1.784379	201.912931	6.996197	322.80853082	59.27632496	111.4517	55918.5150810185	2011-12-23 12:21:43	55918.843912037	2011-12-23 20:15:14	806098020	16.062	13	16.062	16.062	0	16.062	1	1	0	1	1	0	0	11.964	11.964	28.4079	0	PROCESSED	57604.214375	2016-08-04 05:08:42	56311	2013-01-19 00:00:00	55972.6764236111	2012-02-15 16:14:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	063019	We observe Abell 1750 which has three clusters of galaxies in a filamentary structure of the large-scale structure, with 4 pointing observations (80 x 3 + 40 ks). We reveal global spatial structures of temperature, density, and entropy in Abell 1750 for the first time. By a correlation with a galaxy map obtained from SDSS, and a comparison between thermal pressure and total pressure required by the total mass derived from weal lensing analysis, we explore the inflow of matter and evolutionary process in this system.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA		JUS	6	AO6	SUZAKU OBSERVATION OF ABELL 1750 IN THE LARGE-SCALE STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806098020/	Quick Look
835	A3391&A3395 FILAMENT	96.6913	-54.1225	96.432969	-54.090694	107.900065	-77.146986	262.85175229	-25.18315788	316.4875	56791.0860532407	2014-05-14 02:03:55	56792.4794328704	2014-05-15 11:30:23	809033010	88.6134	92	88.6134	88.6134	0	88.6134	2	2	0	2	1	0	0	15.2448	15.2448	23.346	0	PROCESSED	57615.0916319445	2016-08-15 02:11:57	57227	2015-07-24 00:00:00	56861.4967361111	2014-07-23 11:55:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090082	To investigate hot gas properties of a large scale filament, we propose Suzaku observation (92 ks) of a filamentary structure between Abell 3391 and Abell 3395. A3391 and A3395 are located in Horologium supercluster and expected to be in an initial phase of a cluster merger. With Suzaku fs high sensitivity observation, we will (i) determine the physical conditions of IntraCluster Medium by measuring the temperature and density distribution, (ii) unveil the origin of the filamentary structure from distribution of abundance, pressure and entropy. Our study will reveal the formation history of the filament and provide a useful information for the future Sunyaev-Zeldovich effect observations.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YOSHITAKA ISHISAKI		JAP	9	AO9	INVESTIGATION OF THE ORIGIN OF THE FILAMENTARY STRUCTURE BETWEEN ABELL 3391 AND ABELL 3395	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809033010/	Quick Look
836	RXCJ0605	91.4958	-35.4837	91.05364	-35.477523	92.366503	-58.913023	241.98342334	-24.04647163	309.0856	55321.4301041667	2010-05-05 10:19:21	55322.221712963	2010-05-06 05:19:16	805065010	40.9762	40	40.9762	40.9762	0	40.9762	2	2	0	2	1	0	0	35.5095	35.5095	68.3681	0	PROCESSED	57551.3998032407	2016-06-12 09:35:43	55287	2010-04-01 00:00:00	55341.4983217593	2010-05-25 11:57:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805065010/	Quick Look
837	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
838	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
839	BOOTES_GROUP_32	217.4805	33.2976	216.950847	33.519259	200.513031	44.906456	55.13369931	67.90745799	91.5977	54868.4415740741	2009-02-06 10:35:52	54869.3619675926	2009-02-07 08:41:14	803045010	40.7287	40	40.7447	40.7287	0	40.7447	2	2	0	2	1	0	0	34.6563	34.6563	79.4878	2	PROCESSED	57545.4809490741	2016-06-06 11:32:34	55328	2010-05-12 00:00:00	54880.5918518518	2009-02-18 14:12:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031411	Galaxy groups are vital to our understanding of structure formation, cluster evolution, and galaxy evolution, yet they are difficult to study at even moderate redshift. We have undertaken a project to observe a flux-limited sample of intermediate-redshift groups identified by the XBootes Chandra survey, and here we propose Suzaku/XIS observations of two targets to continue this program. With the unique multiwavelength coverage of the XBootes field, we aim to understand the physical connection between the X-ray and optical properties of groups, and to probe the evolution of group X-ray emission in order to constrain the non-gravitational physics affecting the energetics of the intragroup medium.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ERIC MILLER		USA	3	AO3	UNDERSTANDING GROUP EVOLUTION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803045010/	Quick Look
840	BOOTES_GROUP_37	216.3696	32.9366	215.835617	33.161488	199.570858	44.168282	54.59315934	68.88543442	308.8196	54640.4539467593	2008-06-23 10:53:41	54641.6898611111	2008-06-24 16:33:24	803044010	52.9034	40	52.9114	52.9114	0	52.9034	2	2	0	2	1	0	0	47.6527	47.6527	106.7658	2	PROCESSED	57542.9257638889	2016-06-03 22:13:06	55020	2009-07-08 00:00:00	54651.1591319444	2008-07-04 03:49:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031411	Galaxy groups are vital to our understanding of structure formation, cluster evolution, and galaxy evolution, yet they are difficult to study at even moderate redshift. We have undertaken a project to observe a flux-limited sample of intermediate-redshift groups identified by the XBootes Chandra survey, and here we propose Suzaku/XIS observations of two targets to continue this program. With the unique multiwavelength coverage of the XBootes field, we aim to understand the physical connection between the X-ray and optical properties of groups, and to probe the evolution of group X-ray emission in order to constrain the non-gravitational physics affecting the energetics of the intragroup medium.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ERIC MILLER		USA	3	AO3	UNDERSTANDING GROUP EVOLUTION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803044010/	Quick Look
841	ABELL 2259	259.8931	27.621	259.395788	27.671022	255.818642	50.564036	50.28820146	31.27138653	102.8681	57093.1224305556	2015-03-12 02:56:18	57094.3141203704	2015-03-13 07:32:20	809081040	43.027	42.5	43.027	43.027	0	43.5266	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.7751736111	2016-08-17 18:36:15	57475	2016-03-28 00:00:00	57108.4150578704	2015-03-27 09:57:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091526	Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	9	AO9	REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809081040/	Quick Look
842	ABELL 426 N5	49.0181	42.6863	48.185508	42.502238	58.244167	23.659861	149.32374876	-12.65326208	59.9992	55063.2465740741	2009-08-20 05:55:04	55063.8238310185	2009-08-20 19:46:19	804067010	23.6074	20	23.6314	23.6074	0	23.6394	2	2	0	2	1	0	0	21.1435	21.1435	49.8659	1	PROCESSED	57548.2975115741	2016-06-09 07:08:25	55441	2010-09-02 00:00:00	55075.0347685185	2009-09-01 00:50:04	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804067010/	Quick Look
843	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
844	A1750R	202.8633	-2.0722	202.218991	-1.815068	201.918925	6.965529	322.77954726	59.24881782	293.5198	55748.0658796296	2011-07-06 01:34:52	55750.0419097222	2011-07-08 01:00:21	806098010	66.5035	80	66.5115	66.5035	0	66.5115	3	2	0	2	1	0	0	54.7821	54.7821	170.7128	3	PROCESSED	57602.5535763889	2016-08-02 13:17:09	56311	2013-01-19 00:00:00	55795.163912037	2011-08-22 03:56:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	063019	We observe Abell 1750 which has three clusters of galaxies in a filamentary structure of the large-scale structure, with 4 pointing observations (80 x 3 + 40 ks). We reveal global spatial structures of temperature, density, and entropy in Abell 1750 for the first time. By a correlation with a galaxy map obtained from SDSS, and a comparison between thermal pressure and total pressure required by the total mass derived from weal lensing analysis, we explore the inflow of matter and evolutionary process in this system.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MADOKA KAWAHARADA	SCOTT RANDALL	JUS	6	AO6	SUZAKU OBSERVATION OF ABELL 1750 IN THE LARGE-SCALE STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806098010/	Quick Look
845	COMA E6	196.7721	27.8867	196.173433	28.153627	183.239501	32.041991	46.15941504	86.44797144	279.9997	55731.2742013889	2011-06-19 06:34:51	55731.589837963	2011-06-19 14:09:22	806036010	12.4586	15	12.4666	12.4586	0	12.4666	1	1	0	1	1	0	0	12.2065	12.2065	27.2519	0	PROCESSED	57602.3498263889	2016-08-02 08:23:45	55652	2011-04-01 00:00:00	55770.1165046296	2011-07-28 02:47:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806036010/	Quick Look
846	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
847	THE MOON	132.8593	12.3218	132.173537	12.509929	131.851232	-5.111118	215.15290673	32.14399459	282.2504	56783.6861921296	2014-05-06 16:28:07	56783.8127083333	2014-05-06 19:30:18	809001020	4.6445	45	4.6445	4.6445	0	4.6605	1	1	0	1	1	0	0	4.9299	4.9299	10.9199	0	PROCESSED	57615.0434143518	2016-08-15 01:02:31	57162	2015-05-20 00:00:00	56793.5180324074	2014-05-16 12:25:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090016	The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YOSHIHIRO UEDA		JAP	9	AO9	USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001020/	Quick Look
848	ABELL 3411	130.503	-17.558	129.929319	-17.378234	138.643901	-34.411415	242.03718903	14.84069283	105.0003	56964.4121759259	2014-11-03 09:53:32	56967.3091898148	2014-11-06 07:25:14	809082010	126.6792	130	126.6792	131.2712	0	131.2632	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.749525463	2016-08-16 17:59:19	57358	2015-12-02 00:00:00	56982.4526273148	2014-11-21 10:51:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091528	Galaxy cluster mergers trigger Mpc-scale shocks in the ICM, which can accelerate particles to relativistic energies to form arc-shaped radio relics. Last year, we discovered a spectacular radio relic in the Planck cluster A3411. The relic has a complex, fragmentary morphology, at odds with the arc-shaped shocks predicted by hydrodynamical simulations. In light of this unexpected discovery, we propose for a 169-ks Suzaku observation to characterize the ICM properties at the radio relic in A3411. The combination of high-quality X-ray and radio data will provide a unique opportunity to (1) measure the shock properties and relate them to the radio structures; (2) explore the reason for the fragmentation of the relic; (3) model the merger event; and (4) test different shock acceleration models.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	REINOUT VAN WEEREN		USA	9	AO9	ABELL 3411: PARTICLE RE-ACCELERATION AND A COMPLEX SHOCK GEOMETRY?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809082010/	Quick Look
849	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
850	ABELL2804	9.8968	-28.9096	9.281885	-29.184169	356.393467	-30.22696	357.98440451	-86.83577265	234.7036	53706.3688078704	2005-12-02 08:51:05	53707.166875	2005-12-03 04:00:18	800007010	31.6129	25	31.6129	31.6129	31.6129	31.6129	2	2	2	2	1	0	0	26.9145	26.9145	68.95	2	PROCESSED	57532.3559259259	2016-05-24 08:32:32	54247	2007-05-27 00:00:00	54038.8727893518	2006-10-30 20:56:49	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001025	We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYUKI TAMURA		JAP	0	SWG	THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800007010/	Quick Look
851	A2142	239.5312	27.2879	239.014287	27.430116	229.09968	46.49364	44.29837206	48.74478569	138.1624	54104.1546990741	2007-01-04 03:42:46	54105.3891666667	2007-01-05 09:20:24	801055010	51.4525	60	51.4605	51.4525	0	51.4605	2	2	0	2	1	0	0	49.2098	49.2098	106.632	1	PROCESSED	57536.4705555556	2016-05-28 11:17:36	54735	2008-09-26 00:00:00	54111.417037037	2007-01-11 10:00:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010106	We propose to reveal the formation and evolution of dense core with cold fronts with SUZAKU/XIS. Our strategy of observation is based on the results of Chandra, ROSAT and weak lensing analysis. A2142 is a galaxy cluster which has contact discontinuities, "cold fronts", between cold-dense cores and hot-thin surrounding gas. We have carried out "weak lensing analysis" and derived mass map in A2142. We measure the bulk velocity via Fe-K line in the central region. We derive the merger velocity by observing the temperatures of the heating and non-heating which are expected by our observational results. It leads to understand the formation and evolution of dense core with cold fronts, since the merger and core velocities are closely related to the evolution of dense cores with cold fronts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NOBUHIRO OKABE		JAP	1	AO1	REVEALING COLD FRONTS AND DENSE CORES IN GALAXY CLUSTER A2142	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801055010/	Quick Look
852	PKS 0745-191	116.6543	-19.2063	116.100315	-19.082609	123.362638	-39.608686	236.25768919	2.88874721	294.0002	54231.8221180556	2007-05-11 19:43:51	54232.5001041667	2007-05-12 12:00:09	802062020	31.2266	30	31.2266	31.2266	0	31.2266	2	2	0	2	1	0	0	25.967	25.967	58.5739	1	PROCESSED	57538.6330208333	2016-05-30 15:11:33	54695	2008-08-17 00:00:00	54238.8889814815	2007-05-18 21:20:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021440	PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ANDREW YOUNG		USA	2	AO2	PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062020/	Quick Look
853	RCS 1104-0445	166.1645	-4.748	165.529365	-4.478046	169.133755	-9.830173	259.90521833	48.99506028	108.5039	54420.9087037037	2007-11-16 21:48:32	54421.3210532407	2007-11-17 07:42:19	802068010	19.335	15	19.335	19.335	0	19.335	1	1	0	1	1	0	0	15.1627	15.1627	35.6159	0	PROCESSED	57540.5367013889	2016-06-01 12:52:51	54797	2008-11-27 00:00:00	54430.2980787037	2007-11-26 07:09:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021451	We propose Suzaku observations of a sample of 10 galaxy clusters at redshifts between 0.6 and 0.95 from the RCS-1 cluster survey. These objects represent the optically richest clusters at these redshifts from the 100 square degree survey using the red-sequence method of cluster detection. As such, they form a critical sample for calibrating the mass-richness relationship for high redshift cluster surveys. Our proposed observations will allow us to determine their X-ray luminosities, as a first guide to estimating their masses, and enable future studies to determine accurate masses from their X-ray properties. These studies are complimentary to mass calibration programs we are carrying out using estimates based on lensing, IR stellar mass and galaxy dynamics.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	2	AO2	A SUZAKU SNAPSHOT SURVEY OF HIGH-REDSHIFT GALAXY CLUSTERS FROM THE RCS SURVEY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802068010/	Quick Look
854	NGC741MOSAICS_P3	28.9813	4.9712	28.329333	4.726893	28.70862	-6.461023	151.24323938	-54.31718683	71.7124	55052.9243981482	2009-08-09 22:11:08	55053.1529976852	2009-08-10 03:40:19	804054030	9.4013	10	9.4093	9.4013	0	9.415	1	1	0	1	1	0	0	7.0683	7.0683	19.72	0	PROCESSED	57548.0955671296	2016-06-09 02:17:37	55451	2010-09-12 00:00:00	55085.0001736111	2009-09-11 00:00:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054030/	Quick Look
855	FG14	176.6962	9.8632	176.052451	10.141025	173.028517	7.733182	258.4262435	66.96745764	295.6185	56076.7125925926	2012-05-29 17:06:08	56077.2168171296	2012-05-30 05:12:13	807055010	12.4926	10	12.5006	12.495	0	12.4926	2	2	0	2	1	0	0	13.535	13.535	43.5539	1	PROCESSED	57605.5555671296	2016-08-05 13:20:01	56452	2013-06-09 00:00:00	56086.1554861111	2012-06-08 03:43:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071511	Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ELENA D'ONGHIA		USA	7	AO7	SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807055010/	Quick Look
856	HYDRA A SE	139.5641	-12.2366	138.96256	-12.025643	146.239045	-26.524458	243.07517911	25.03717361	300.0006	56085.6674421296	2012-06-07 16:01:07	56086.2926388889	2012-06-08 07:01:24	807087010	21.4898	20	21.4898	21.4898	0	21.4898	2	2	0	2	1	0	0	20.3651	20.3651	54.012	0	PROCESSED	57605.6279976852	2016-08-05 15:04:19	56465	2013-06-22 00:00:00	56099.0036921296	2012-06-21 00:05:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072020	Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DOMINIQUE ECKERT		EUR	7	AO7	MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807087010/	Quick Look
857	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
858	SWCL0759+3244	119.7517	32.7514	118.954635	32.88785	115.246831	11.881047	188.23731341	27.65711067	99.0622	56961.3067708333	2014-10-31 07:21:45	56962.2286574074	2014-11-01 05:29:16	809085010	42.3039	41	42.3039	42.3039	0	42.3039	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7390277778	2016-08-16 17:44:12	57345	2015-11-19 00:00:00	56979.4492708333	2014-11-18 10:46:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091531	The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	XINYU DAI		USA	9	AO9	X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809085010/	Quick Look

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