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 1259

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	Crab Nebula	83.6449	22.0152	82.892626	21.982571	84.11016	-1.295832	184.56274906	-5.77473152	84.9987	53614.1083449074	2005-09-01 02:36:01	53614.1771759259	2005-09-01 04:15:08	100015030	2.1	5	2.1	2.1	2.1	2.1	1	1	1	1	1	0	0	2.3074	2.3074	5.9439	0	PROCESSED	57527.235150463	2016-05-19 05:38:37	54247	2007-05-27 00:00:00	54109.3966782407	2007-01-09 09:31:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000015		CALIBRATION	1	A	SWG		JAP	0	SWG	HXD boresight check with Crab		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015030/
2	E0102-72	15.9884	-72.0403	15.58329	-72.308299	314.593543	-65.036118	301.56673438	-45.05476105	119.5512	53595.2489236111	2005-08-13 05:58:27	53595.4618518518	2005-08-13 11:05:04	100001020	4.1598	10	4.1598	4.1598	4.1598	4.1598	1	1	1	2	0	0	0	0	0	0	0	PROCESSED	57520.6779861111	2016-05-12 16:16:18	54247	2007-05-27 00:00:00	54035.6312731482	2006-10-27 15:09:02	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000001	XIS door open with a SMC SNR E0102-72	CALIBRATION	1	A	SWG		JAP	0	SWG	XIS door open		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100001020/	Quick Look
3	N132D	81.2751	-69.6506	81.377584	-69.69262	312.405312	-85.522517	280.31335191	-32.77744994	53.3312	53598.2402777778	2005-08-16 05:46:00	53598.5140046296	2005-08-16 12:20:10	100002060	5.9635	7	5.9635	5.9635	5.9635	5.9635	1	1	1	1	0	0	0	0	0	0	0	PROCESSED	57520.6925115741	2016-05-12 16:37:13	54247	2007-05-27 00:00:00	54038.4700810185	2006-10-30 11:16:55	3.0.22.43	6	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000002	HXD HV ON WITH N132D, and 5 pointings with XIS	CALIBRATION	1	A	SWG		JAP	0	SWG	HXD HV ON WITH N132D		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100002060/	Quick Look
4	DEM_L71/N23	76.4474	-67.958	76.476582	-68.023213	338.826937	-84.59461	278.75859594	-34.83581885	70.5849	53598.5206365741	2005-08-16 12:29:43	53599.6042592593	2005-08-17 14:30:08	100003010	5.7897	40	5.7897	5.7897	5.7897	5.7897	2	2	2	2	0	0	0	0	0	93.6061	0	PROCESSED	57520.7098611111	2016-05-12 17:02:12	54247	2007-05-27 00:00:00	54035.7018171296	2006-10-27 16:50:37	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000003	LMC SNRs L71/N23	CALIBRATION	1	A	SWG		JAP	0	SWG	LMC SNRs		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100003010/	Quick Look
5	A 2052	229.2779	6.8766	228.662841	7.059342	224.77082	24.150691	9.31339919	49.96215441	281.2328	53602.4238078704	2005-08-20 10:10:17	53602.743287037	2005-08-20 17:50:20	100006010	13.9021	20	13.9021	13.9021	13.9021	13.9021	1	1	1	1	1	0	0	13.4163	13.4163	27.5839	0	PROCESSED	57520.7207407407	2016-05-12 17:17:52	53705	2005-12-01 00:00:00	53905.4607523148	2006-06-19 11:03:29	3.0.22.43	11	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000006		CALIBRATION	1	A	SWG		JAP	0	SWG	Outer region of A 2052		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006010/	Quick Look
6	A 2052	229.3237	7.1059	228.709513	7.288472	224.747048	24.38343	9.64711471	50.05514889	281.2373	53602.7440393518	2005-08-20 17:51:25	53603.3406944445	2005-08-21 08:10:36	100006020	25.7431	20	25.7431	25.7431	25.7431	25.7431	1	1	1	1	1	0	0	21.0642	21.0642	51.5199	0	PROCESSED	57520.7246527778	2016-05-12 17:23:30	53705	2005-12-01 00:00:00	53905.4610300926	2006-06-19 11:03:53	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000006		CALIBRATION	1	A	SWG		JAP	0	SWG	Outer region of A 2052		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006020/	Quick Look
7	A 2052	229.0933	7.1516	228.479191	7.335016	224.492199	24.361996	9.50335527	50.26933049	281.2093	53603.3412615741	2005-08-21 08:11:25	53603.6114351852	2005-08-21 14:40:28	100006030	12.969	20	12.969	12.969	12.969	12.969	1	1	1	1	1	0	0	13.1413	13.1413	23.3279	0	PROCESSED	57520.7271527778	2016-05-12 17:27:06	53705	2005-12-01 00:00:00	53905.4613310185	2006-06-19 11:04:19	3.0.22.43	9	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000006		CALIBRATION	1	A	SWG		JAP	0	SWG	Outer region of A 2052		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006030/	Quick Look
8	A 2052	229.3311	7.2632	228.717502	7.445744	224.705557	24.536292	9.85579143	50.13807877	91.2371	53762.482650463	2006-01-27 11:35:01	53762.9209953704	2006-01-27 22:06:14	100006050	22.366	20	22.366	22.366	22.366	22.366	2	2	2	2	1	0	0	20.388	20.388	37.8659	0	PROCESSED	57532.800162037	2016-05-24 19:12:14	54247	2007-05-27 00:00:00	54040.5318634259	2006-11-01 12:45:53	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000006		CALIBRATION	1	A	SWG		JAP	0	SWG	Outer region of A 2052	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006050/	Quick Look
9	NGC 4945	196.3681	-49.4152	195.638243	-49.147517	216.98939	-38.593586	305.27752827	13.39262005	96.1296	53750.3365625	2006-01-15 08:04:39	53752.9655092593	2006-01-17 23:10:20	100008030	95.0663	10	95.0817	95.1297	95.0663	95.1063	2	2	2	2	1	0	0	84.9813	84.9813	227.1157	2	PROCESSED	57532.7353240741	2016-05-24 17:38:52	54247	2007-05-27 00:00:00	54040.3587615741	2006-11-01 08:36:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000008		CALIBRATION	1	A	SWG		JAP	0	SWG	NGC 4945	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100008030/	Quick Look
10	PSR1509-58	228.4798	-59.0943	227.494741	-58.907902	243.862404	-39.360151	320.34145971	-1.12587132	287.6342	53605.36	2005-08-23 08:38:24	53606.8597569444	2005-08-24 20:38:03	100009010	65.1618	60	65.1618	65.3227	65.2427	65.2427	3	3	3	3	1	0	0	49.7357	49.7357	129.5298	4	PROCESSED	57526.9045486111	2016-05-18 21:42:33	53705	2005-12-01 00:00:00	53905.4622337963	2006-06-19 11:05:37	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000009	HXD spectrum and timing check	CALIBRATION	1	A	SWG		JAP	0	SWG	PSR1509-58		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100009010/	Quick Look
11	Crab Nebula	83.6267	22.0751	82.874095	22.042383	84.095945	-1.235244	184.50282132	-5.75691305	86.8655	53607.0070833333	2005-08-25 00:10:12	53607.1389814815	2005-08-25 03:20:08	100010010	2.9379	5	2.9379	2.9379	2.9379	2.9379	2	2	2	2	1	0	0	3.4387	3.4387	11.3819	0	PROCESSED	57526.8678703704	2016-05-18 20:49:44	54247	2007-05-27 00:00:00	54118.9886689815	2007-01-18 23:43:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010010/	Quick Look
12	Crab nebula	83.6336	21.9568	82.881657	21.924117	84.097114	-1.353715	184.60669551	-5.81484075	86.8687	53607.1394560185	2005-08-25 03:20:49	53607.2779282407	2005-08-25 06:40:13	100010020	3.6533	5	3.6533	3.6533	3.6533	3.6533	1	1	1	1	1	0	0	3.8067	3.8067	11.934	0	PROCESSED	57526.8772337963	2016-05-18 21:03:13	54247	2007-05-27 00:00:00	54118.9337615741	2007-01-18 22:24:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010020/	Quick Look
13	Crab nebula	83.6511	21.6763	82.900722	21.643705	84.100986	-1.634666	184.85366771	-5.95118505	86.8795	53607.5153125	2005-08-25 12:22:03	53607.7153472222	2005-08-25 17:10:06	100010040	9.5806	5	9.5806	9.5806	9.5806	9.5806	1	1	1	1	1	0	0	8.1783	8.1783	17.248	0	PROCESSED	57526.8981828704	2016-05-18 21:33:23	54247	2007-05-27 00:00:00	54118.943125	2007-01-18 22:38:06	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010040/	Quick Look
14	Crab nebula	83.5677	22.0135	82.815455	21.980499	84.038563	-1.294359	184.52566905	-5.83608695	86.8444	53607.9175810185	2005-08-25 22:01:19	53608.0695023148	2005-08-26 01:40:05	100010060	4.8779	5	4.8779	4.8779	4.8779	4.8779	1	1	1	1	1	0	0	5.0217	5.0217	13.076	0	PROCESSED	57526.9066087963	2016-05-18 21:45:31	54247	2007-05-27 00:00:00	54122.4195486111	2007-01-22 10:04:09	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010060/	Quick Look
15	Crab nebula	83.6922	22.0221	82.939876	21.989699	84.154283	-1.290862	184.58047361	-5.73399538	86.8671	53608.0699768518	2005-08-26 01:40:46	53608.2084027778	2005-08-26 05:00:06	100010070	4.0899	5	4.0899	4.0899	4.0899	4.0899	1	1	1	1	1	0	0	4.2283	4.2283	11.9259	0	PROCESSED	57526.9072222222	2016-05-18 21:46:24	54247	2007-05-27 00:00:00	54119.0149074074	2007-01-19 00:21:28	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010070/	Quick Look
16	Crab nebula	83.5807	22.8483	82.82374	22.81535	84.087744	-0.460898	183.82410841	-5.37832099	86.8677	53608.3175810185	2005-08-26 07:37:19	53608.5139583333	2005-08-26 12:20:06	100010090	6.716	5	6.716	6.716	6.716	6.716	1	1	1	1	1	0	0	6.3768	6.3768	16.9501	0	PROCESSED	57526.9164699074	2016-05-18 21:59:43	54247	2007-05-27 00:00:00	54119.0235648148	2007-01-19 00:33:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010090/	Quick Look
17	Crab nebula	83.5122	24.0135	82.748583	23.980205	84.077056	0.70598	182.80375415	-4.80497322	86.8675	53608.7179976852	2005-08-26 17:13:55	53608.930625	2005-08-26 22:20:06	100010110	9.4805	5	9.4805	9.4805	9.4805	9.4805	1	1	1	1	1	0	0	7.363	7.363	18.336	0	PROCESSED	57526.9265162037	2016-05-18 22:14:11	54247	2007-05-27 00:00:00	54118.98625	2007-01-18 23:40:12	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010110/	Quick Look
18	Crab nebula	83.6374	21.9009	82.885769	21.868236	84.09817	-1.409717	184.65605757	-5.84178049	86.8664	53608.9333217593	2005-08-26 22:23:59	53609.069525463	2005-08-27 01:40:07	100010120	4.7456	5	4.7456	4.7456	4.7456	4.7456	2	2	2	2	1	0	0	5.1787	5.1787	11.7579	1	PROCESSED	57526.9343287037	2016-05-18 22:25:26	54247	2007-05-27 00:00:00	54118.9946180556	2007-01-18 23:52:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010120/	Quick Look
19	Crab nebula	83.5044	22.0116	82.752181	21.978293	83.979835	-1.293628	184.49566519	-5.88665136	86.8658	53609.0701388889	2005-08-27 01:41:00	53609.2014583333	2005-08-27 04:50:06	100010130	4.222	5	4.222	4.222	4.222	4.222	1	1	1	1	1	0	0	4.3724	4.3724	11.3359	0	PROCESSED	57526.9346180556	2016-05-18 22:25:51	54247	2007-05-27 00:00:00	54119.0454282407	2007-01-19 01:05:25	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010130/	Quick Look
20	Galactic bulge	236.4313	-31.7013	235.648361	-31.545749	241.296308	-11.543137	340.99994533	17.99808229	283.5446	53609.4365856482	2005-08-27 10:28:41	53611.060625	2005-08-29 01:27:18	100011010	61.133	70	61.133	61.133	61.133	61.133	1	1	1	1	1	0	0	47.9834	47.9834	140.282	2	PROCESSED	57526.962037037	2016-05-18 23:05:20	54247	2007-05-27 00:00:00	54034.8288310185	2006-10-26 19:53:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000011		CALIBRATION	1	A	SWG		JAP	0	SWG	Galactic bulge		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100011010/	Quick Look
21	Eta Carinae	161.281	-59.6845	160.794333	-59.421136	202.162077	-58.916082	287.6040589	-0.62575348	343.8621	53611.0750347222	2005-08-29 01:48:03	53612.0627546296	2005-08-30 01:30:22	100012010	49.782	40	49.79	49.782	49.782	49.798	2	2	2	2	1	0	0	55.9607	55.9607	85.2529	0	PROCESSED	57526.9773032407	2016-05-18 23:27:19	53705	2005-12-01 00:00:00	53905.4648842593	2006-06-19 11:09:26	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000012		CALIBRATION	1	A	SWG		JAP	0	SWG	Eta Carinae		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100012010/	Quick Look
22	N103B	77.2315	-68.7507	77.290508	-68.812132	329.838884	-84.691105	279.61119012	-34.36730962	73.8586	53612.0740162037	2005-08-30 01:46:35	53613.0626273148	2005-08-31 01:30:11	100013010	33.0646	40	33.0646	33.0646	33.0646	33.0646	2	2	2	2	1	0	0	37.2814	37.2814	85.4059	1	PROCESSED	57526.9730324074	2016-05-18 23:21:10	54247	2007-05-27 00:00:00	54034.8733449074	2006-10-26 20:57:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000013		CALIBRATION	1	A	SWG		JAP	0	SWG	N103B		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100013010/	Quick Look
23	E0102-72	15.9813	-72.0378	15.57605	-72.305808	314.596715	-65.033076	301.56958331	-45.05740554	140.1798	53613.0710648148	2005-08-31 01:42:20	53613.7640509259	2005-08-31 18:20:14	100014010	24.3339	20	24.3339	24.3339	24.3339	24.3339	2	2	2	2	1	0	0	24.5144	24.5144	59.8639	2	PROCESSED	57511.5174884259	2016-05-03 12:25:11	53705	2005-12-01 00:00:00	53905.4615740741	2006-06-19 11:04:40	3.0.22.43	13	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000014		CALIBRATION	1	A	SWG		JAP	0	SWG	XIS monitor with E0102-72		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100014010/	Quick Look
24	Crab Nebula	83.6296	22.1792	82.876409	22.146495	84.103227	-1.131361	184.41590928	-5.69889955	84.9998	53613.9762152778	2005-08-31 23:25:45	53614.1077314815	2005-09-01 02:35:08	100015020	4.95	5	4.95	4.95	4.95	4.95	1	1	1	1	1	0	0	5.1178	5.1178	11.3599	0	PROCESSED	57527.2276388889	2016-05-19 05:27:48	54247	2007-05-27 00:00:00	54109.1090972222	2007-01-09 02:37:06	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000015		CALIBRATION	1	A	SWG		JAP	0	SWG	HXD boresight check with Crab		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015020/	Quick Look
25	SN1006 SW BG	224.655	-42.4005	223.837497	-42.201017	234.783022	-24.341132	326.632731	14.54333558	310.4886	53624.9999189815	2005-09-11 23:59:53	53626.0071643518	2005-09-13 00:10:19	100019040	32.3334	50	32.3334	32.3494	32.3414	32.3414	2	2	2	2	1	0	0	24.6736	24.6736	87.0159	5	PROCESSED	57527.3647453704	2016-05-19 08:45:14	54247	2007-05-27 00:00:00	54035.4482638889	2006-10-27 10:45:30	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000019		CALIBRATION	1	A	SWG		JAP	0	SWG	SN1006 observation with XIS and HXD		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019040/	Quick Look
26	SN1006 SW BG	224.6468	-42.4025	223.829311	-42.202989	234.777387	-24.344913	326.62625739	14.54451897	100.3489	53761.7199652778	2006-01-26 17:16:45	53762.4752777778	2006-01-27 11:24:24	100019060	27.9813	50	27.9813	27.9893	27.9973	27.9973	2	2	2	2	1	0	0	29.5504	29.5504	65.2499	2	PROCESSED	57532.7989814815	2016-05-24 19:10:32	54247	2007-05-27 00:00:00	54040.5663541667	2006-11-01 13:35:33	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000019		CALIBRATION	1	A	SWG		JAP	0	SWG	SN1006 observation with XIS and HXD	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019060/	Quick Look
27	Fornax Cluster	54.6395	-35.4918	54.160816	-35.653913	38.755932	-52.830853	236.7850293	-53.61976834	103.5002	53626.0756018518	2005-09-13 01:48:52	53627.5002662037	2005-09-14 12:00:23	100020010	76.0782	100	76.0782	76.0782	76.0782	76.0782	2	2	2	2	1	0	0	71.1128	71.1128	123.0639	3	PROCESSED	57527.3377430556	2016-05-19 08:06:21	54247	2007-05-27 00:00:00	54035.4442013889	2006-10-27 10:39:39	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000020		CALIBRATION	1	A	SWG		JAP	0	SWG	Fornax Cluster		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100020010/	Quick Look
28	Crab Nebula	82.7325	21.9883	81.980613	21.951274	83.263643	-1.282782	184.12771921	-6.50224239	88.0978	53628.3006828704	2005-09-15 07:12:59	53628.5835416667	2005-09-15 14:00:18	100022020	10.9198	10	10.9198	10.9198	10.9198	10.9198	1	1	1	1	1	0	0	6.3401	6.3401	24.4	2	PROCESSED	57527.3262615741	2016-05-19 07:49:49	54247	2007-05-27 00:00:00	54109.1486342593	2007-01-09 03:34:02	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000022	Crab at 50arcmin off from the XIS aimpoint to study stray light.	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab at 50 arcmin off		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100022020/	Quick Look
29	Crab Nebula	84.5289	22.0469	83.776247	22.018539	84.930453	-1.297747	184.974122	-5.06424795	87.5879	53629.0921759259	2005-09-16 02:12:44	53629.368275463	2005-09-16 08:50:19	100022030	12.8244	10	12.8404	12.8324	12.8244	12.8484	2	2	2	2	1	0	0	10.3518	10.3518	23.824	1	PROCESSED	57527.3478009259	2016-05-19 08:20:50	54247	2007-05-27 00:00:00	54109.1621527778	2007-01-09 03:53:30	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000022	Crab at 50arcmin off from the XIS aimpoint to study stray light.	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab at 50 arcmin off		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100022030/	Quick Look
30	Crab Nebula	83.6282	22.0761	82.875589	22.04339	84.097378	-1.234306	184.5027205	-5.75520363	87.79	53628.5852199074	2005-09-15 14:02:43	53628.8265393518	2005-09-15 19:50:13	100023010	11.9978	10	11.9978	11.9978	11.9978	11.9978	1	1	1	1	1	0	0	10.5132	10.5132	20.8239	0	PROCESSED	57527.3355902778	2016-05-19 08:03:15	54247	2007-05-27 00:00:00	54109.2268287037	2007-01-09 05:26:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000023	Calibration of detector response at both of XIS/HXD nominal positions, together with an absolute flux confirmation with differnt hit-pattern widths.	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab at nominal positions		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100023010/	Quick Look
31	BD +30 3639	293.6887	30.5051	293.198078	30.394341	303.540216	51.224252	64.77556877	5.01383279	277.8713	53634.3814930556	2005-09-21 09:09:21	53635.2473842593	2005-09-22 05:56:14	100025010	35.2146	40	35.2306	35.2306	35.2146	35.2226	2	2	2	2	1	0	0	33.3728	33.3728	74.8039	1	PROCESSED	57527.3931597222	2016-05-19 09:26:09	54247	2007-05-27 00:00:00	54035.4664583333	2006-10-27 11:11:42	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000025	The proposed target, BD +30 3639, is a prototypical planetary nebula which emit diffuse X-rays; planetary nebulae represent the final evolutionary stage of low mass stars, and contain very rich information on the stellar nucleosynthesis. The Chandra ACIS spectrum of BD +30 3639 bears an amazingly strong Ne-K line, most certainly because the X-ray emitting material directly reflect the "onion-like structure" of elements insied evolved stars. However, the ACIS was not able to resolve C, N, O lines, which are of vital importance. The XMM RGS and Chandra LETG could do, but we need very long exposure. Using the Suzaku XIS-BI with the excellent low-energy performance, we can for the first time measure the C/N/O/Mg abundance ratios of this important object in a short time.	CALIBRATION	1	A	SWG		JAP	0	SWG	Observation of planetary nebula BD +30 3639		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100025010/	Quick Look
32	RXJ1713-3946-BKGD2	257.2742	-41.0338	256.397744	-40.970376	259.926088	-18.035902	345.80577047	-0.54060643	270.0033	53641.2980671296	2005-09-28 07:09:13	53642.1843055556	2005-09-29 04:25:24	100026030	37.5132	40	37.5372	37.5292	37.5132	37.5132	2	2	2	2	1	0	0	31.8982	31.8982	76.5659	0	PROCESSED	57527.4461574074	2016-05-19 10:42:28	54247	2007-05-27 00:00:00	54035.6187268518	2006-10-27 14:50:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000026	RXJ1713 is very important sources in which we can study particle accelerator in the universe. X-ray synchrotron spectrum suggest the existence of distribution of high energy electron. Very similar TeV and ASCA morphologies show close connection between these energy bands. The interaction with molecular cloud suggests that proton accelerator resides in this object. The photon index of RXJ1713 seems to be difficult in the frame work of standard diffusive shock scenario. To obtain precise spectrum in the hard X-ray region is therefore very important to determine the energy cut off and to study the mechanism that produce such high energy electrons.	CALIBRATION	1	A	SWG		JAP	0	SWG	Observation of RXJ1713.7-3946		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100026030/	Quick Look
33	M82-Wind	148.8893	69.7655	147.850184	70.002482	118.869306	52.161633	141.33880284	40.49464345	137.7608	53647.5072800926	2005-10-04 12:10:29	53648.1418287037	2005-10-05 03:24:14	100033010	32.3274	100	32.3274	32.3274	32.3274	32.3274	2	2	2	2	1	0	0	30.2224	30.2224	54.8021	0	PROCESSED	57527.5155092593	2016-05-19 12:22:20	54247	2007-05-27 00:00:00	54037.0057175926	2006-10-29 00:08:14	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000033	We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec.	CALIBRATION	1	A	SWG		JAP	0	SWG	Largely Extended Emission (~12kpc) around M82		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100033010/	Quick Look
34	Sgr_A_west	266.3057	-29.1697	265.509983	-29.149828	266.748763	-5.770252	359.75546849	-0.04768885	264.9601	53637.5953356482	2005-09-24 14:17:17	53638.7273032407	2005-09-25 17:27:19	100027020	42.8148	50	42.8148	42.8148	42.8148	42.8148	2	2	2	2	1	0	0	36.091	36.091	97.8	0	PROCESSED	57527.4293865741	2016-05-19 10:18:19	54247	2007-05-27 00:00:00	54035.5135532407	2006-10-27 12:19:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000027	We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.	CALIBRATION	1	A	SWG		JAP	0	SWG	Suzaku Observation of Galactic Center Region		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027020/	Quick Look
35	E0102-72	16.139	-72.1205	15.73725	-72.388297	314.467235	-65.111919	301.50933431	-44.97149935	119.4064	53593.3086458333	2005-08-11 07:24:27	53595.2485069444	2005-08-13 05:57:51	100001010	2.4068	70	2.4068	2.4068	2.4068	2.4068	1	1	1	1	0	0	0	0	0	0	0	PROCESSED	57520.6843287037	2016-05-12 16:25:26	54247	2007-05-27 00:00:00	54035.5925115741	2006-10-27 14:13:13	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000001	XIS door open with a SMC SNR E0102-72	CALIBRATION	1	A	SWG		JAP	0	SWG	XIS door open		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100001010/	Quick Look
36	1E1743.1-2843(GC_BGD_3)	266.592	-28.6516	265.799503	-28.633124	266.987582	-5.246121	0.32828705	0.00813221	264.88	53638.7286111111	2005-09-25 17:29:12	53638.793275463	2005-09-25 19:02:19	100027050	1.9846	5	1.9846	1.9846	1.9846	1.9846	1	1	1	1	1	0	0	1.7934	1.7934	5.5679	0	PROCESSED	57527.4093055556	2016-05-19 09:49:24	54247	2007-05-27 00:00:00	53905.6343055556	2006-06-19 15:13:24	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000027	We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.	CALIBRATION	1	A	SWG		JAP	0	SWG	Suzaku Observation of Galactic Center Region		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027050/	Quick Look
37	HESS J1616-508	244.1248	-50.8971	243.177731	-50.773494	251.629905	-29.09136	332.40352084	-0.15000913	282.8476	53632.5000231482	2005-09-19 12:00:02	53633.8183333333	2005-09-20 19:38:24	100028010	41.352	50	41.352	41.376	41.352	41.368	2	2	2	2	1	0	0	35.3731	35.3731	113.8899	0	PROCESSED	57527.3838194444	2016-05-19 09:12:42	54247	2007-05-27 00:00:00	54035.4361111111	2006-10-27 10:28:00	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000028		CALIBRATION	1	A	SWG		JAP	0	SWG	New HESS sources and the Galactic ridge Background		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100028010/	Quick Look
38	HESS J1616-508_BGD1	243.666	-51.1742	242.717138	-51.048595	251.369654	-29.420684	332.00349288	-0.15039556	283.0062	53631.9497222222	2005-09-18 22:47:36	53632.4990856482	2005-09-19 11:58:41	100028020	19.3277	25	19.3277	20.63	19.36	19.6323	1	1	1	1	1	0	0	16.6426	16.6426	47.4479	0	PROCESSED	57527.3573148148	2016-05-19 08:34:32	54247	2007-05-27 00:00:00	54035.1692476852	2006-10-27 04:03:43	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000028		CALIBRATION	1	A	SWG		JAP	0	SWG	New HESS sources and the Galactic ridge Background		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100028020/	Quick Look
39	GRO J1655-40	253.5027	-39.8455	252.639975	-39.764411	256.800671	-17.156383	344.98315976	2.45489032	268.0237	53635.3140625	2005-09-22 07:32:15	53636.2968055556	2005-09-23 07:07:24	100029010	35.2228	40	0	35.2336	35.2228	35.2308	0	1	2	2	1	0	0	28.7315	28.7315	84.9019	1	PROCESSED	57527.3997337963	2016-05-19 09:35:37	54247	2007-05-27 00:00:00	54035.4940625	2006-10-27 11:51:27	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000029	We propose to observe GRO J1655-40, a transient galactic black hole candidate. With M=~7 Msolar and distinct radio lobes, GRO J1655-40 has been classified as a microquasar. It was highly variable during the first few years after its discovery while showing irregular flaring and a wide range of continuum states. Discrete Fe K absorption structure was observed with ASCA. In the summer of 1997 it entered an extended quiescence that lasted for ~8 years. In March 2005 it became active again and XMM & Chandra have observed it since. Only Suzaku can provide the broadband sensitivity required to map the Fe K structure and the continuum as they change. GRO J1655-40 is rapidly declining and must be observed soon before it reenters quiescence.	CALIBRATION	1	A	SWG		JAP	0	SWG	GRO J1655-40		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100029010/	Quick Look
40	NGC3516	166.7299	72.5779	165.877553	72.848305	123.367172	57.997458	133.2179652	42.40001774	148.9366	53655.5813541667	2005-10-12 13:57:09	53658.3801388889	2005-10-15 09:07:24	100031010	134.4696	150	134.5096	134.5956	134.5096	134.4696	2	2	2	2	1	0	0	122.818	122.818	241.6848	0	PROCESSED	57527.6243634259	2016-05-19 14:59:05	54247	2007-05-27 00:00:00	54036.4704976852	2006-10-28 11:17:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000031	NGC 3516 is one of the brightest Seyfert 1s seen in BAT currently visible to Suzaku. Recent BAT and RXTE observations show that this source is ~2-3 mCrb in the 2-10 keV band and ~4-5 mCrb in 15-100 keV. NGC 3516 is currently much brighter than when XMM observed it in 2000 (e.g., it has since returned to "typical" flux). This source's Fe K line and Compton reflection hump are both quite strong (e.g., as seen with SAX; R is ~1.8 in SAX data).	CALIBRATION	1	A	SWG		JAP	0	SWG	NGC 3516		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100031010/	Quick Look
41	M82-Wind	148.894	69.7643	147.854963	70.001295	118.872596	52.161537	141.33883884	40.49666381	146.246	53662.0401273148	2005-10-19 00:57:47	53662.9390393518	2005-10-19 22:32:13	100033020	40.3586	100	40.3586	40.3826	40.3586	40.3666	2	2	2	2	1	0	0	38.3533	38.3533	77.658	0	PROCESSED	57527.6127546296	2016-05-19 14:42:22	54247	2007-05-27 00:00:00	54036.4196296296	2006-10-28 10:04:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000033	We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec.	CALIBRATION	1	A	SWG		JAP	0	SWG	Largely Extended Emission (~12kpc) around M82		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100033020/	Quick Look
42	M82-Wind	148.8885	69.7652	147.849381	70.00218	118.869202	52.16123	141.33933547	40.4945935	137.7608	53670.4681134259	2005-10-27 11:14:05	53671.1002199074	2005-10-28 02:24:19	100033030	28.3638	100	28.3798	28.3798	28.3718	28.3638	2	2	2	2	1	0	0	25.8121	25.8121	54.604	1	PROCESSED	57527.6784606482	2016-05-19 16:16:59	54247	2007-05-27 00:00:00	54036.8639467593	2006-10-28 20:44:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000033	We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec.	CALIBRATION	1	A	SWG		JAP	0	SWG	Largely Extended Emission (~12kpc) around M82		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100033030/	Quick Look
43	Her X-1	254.465	35.3306	254.01442	35.406187	246.002276	57.482156	58.13562438	37.51514805	249.5714	53648.6450462963	2005-10-05 15:28:52	53649.4341898148	2005-10-06 10:25:14	100035010	36.1235	40	36.9235	36.1235	36.9235	36.9235	2	1	2	2	1	0	0	33.3229	33.3229	68.178	0	PROCESSED	57527.5593518518	2016-05-19 13:25:28	54247	2007-05-27 00:00:00	54036.0084375	2006-10-28 00:12:09	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000035		CALIBRATION	1	A	SWG		JAP	0	SWG	HXD Performance Verification using Her X-1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100035010/	Quick Look
44	Sgr_A_west	266.3063	-29.1685	265.51059	-29.148631	266.749258	-5.769039	359.75676556	-0.04750971	264.9604	53642.1914467593	2005-09-29 04:35:41	53643.187025463	2005-09-30 04:29:19	100037010	43.7412	50	43.7412	43.7492	43.7492	43.7492	2	2	2	2	1	0	0	39.3941	39.3941	86.0139	0	PROCESSED	57527.4581828704	2016-05-19 10:59:47	54247	2007-05-27 00:00:00	54035.6663310185	2006-10-27 15:59:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000037		CALIBRATION	1	A	SWG		JAP	0	SWG	Suzaku Obseration of Galactic Center region 2		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037010/	Quick Look
45	GRS1915+105	288.8014	10.9368	288.21144	10.848425	292.141211	32.943669	45.35928754	-0.22611181	260.5762	53659.6951967593	2005-10-16 16:41:05	53661.9724305556	2005-10-18 23:20:18	100039010	84.7777	80	85.0631	86.4305	85.0711	84.7777	3	3	3	3	1	0	0	68.8623	68.8623	196.7338	2	PROCESSED	57527.9188541667	2016-05-19 22:03:09	54247	2007-05-27 00:00:00	54043.8117476852	2006-11-04 19:28:55	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000039	This observation will be performed as a part of the big multiwavelength campain including Suzaku, VLA, Integral, RXTE, and Spitzer.	CALIBRATION	1	A	SWG		JAP	0	SWG	Campaign of coordinated observation of GRS 1915+105		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100039010/	Quick Look
46	RXJ1856.5-3754	284.1433	-37.91	283.291633	-37.976029	281.504649	-15.032837	358.59722216	-17.21146697	84.0127	53817.9388078704	2006-03-23 22:31:53	53819.4433217593	2006-03-25 10:38:23	100041020	79.169	80	79.177	79.169	79.177	79.177	2	2	2	2	1	0	0	53.2099	53.2099	129.9759	1	PROCESSED	57533.3325231482	2016-05-25 07:58:50	54247	2007-05-27 00:00:00	54042.2967824074	2006-11-03 07:07:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000041	We propose Suzaku observation of a nearby isolated neuron star RXJ1856.5-3754 for the low energy QE calibration of the XIS. Our main purpose is, however, using this source as a soft X-ray QE calibrator on the sky. We hope this source will be observed again in future to check possible contamination on the filter surface etc. Note that the calibration is not only for the BI-CCD(XIS1), but also for FI-CCDs or relative QE among them.	CALIBRATION	1	A	SWG		JAP	0	SWG	LOW ENERGY QE CALIBRATION OF XIS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100041020/	Quick Look
47	Crab nebula	83.6399	21.8519	82.888543	21.819249	84.098328	-1.458773	184.69891686	-5.86604099	86.8683	53604.3898263889	2005-08-22 09:21:21	53604.4890972222	2005-08-22 11:44:18	100007030	2.7861	5	2.7861	2.7861	2.7901	2.7861	1	1	1	1	1	0	0	2.1927	2.1927	8.5541	0	PROCESSED	57520.7416203704	2016-05-12 17:47:56	54247	2007-05-27 00:00:00	54105.2865393518	2007-01-05 06:52:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000007	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Nebula		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100007030/	Quick Look
48	Crab nebula	83.9887	22.0345	83.236236	22.00353	84.429494	-1.290207	184.71743044	-5.49499441	86.8666	53608.5155902778	2005-08-26 12:22:27	53608.7153472222	2005-08-26 17:10:06	100010100	9.694	5	9.694	9.694	9.694	9.694	1	1	1	1	1	0	0	7.5812	7.5812	17.2479	0	PROCESSED	57526.9259606482	2016-05-18 22:13:23	54247	2007-05-27 00:00:00	54122.4242939815	2007-01-22 10:10:59	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010100/	Quick Look
49	Vega	279.2264	38.7699	278.806278	38.72626	285.283614	61.72204	67.43212753	19.23869014	301.7896	53615.367349537	2005-09-02 08:48:59	53615.603587963	2005-09-02 14:29:10	100017010	11.3985	10	11.4065	11.4065	11.4065	11.3985	2	2	2	2	1	0	0	11.5751	11.5751	20.4039	0	PROCESSED	57527.2607407407	2016-05-19 06:15:28	54247	2007-05-27 00:00:00	53906.0764814815	2006-06-20 01:50:08	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000017		CALIBRATION	1	A	SWG		JAP	0	SWG	XIS OBF check with Vega		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100017010/	Quick Look
50	A0535+026	84.7243	26.3189	83.946776	26.291426	85.267864	2.964757	181.44092218	-2.64422146	83.608	53627.5694907407	2005-09-14 13:40:04	53628.0418865741	2005-09-15 01:00:19	100021010	21.761	20	21.761	21.761	21.761	21.761	2	2	2	2	1	0	0	21.2572	21.2572	40.7839	1	PROCESSED	57527.3122337963	2016-05-19 07:29:37	54247	2007-05-27 00:00:00	54035.0644444444	2006-10-27 01:32:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000021	We propose to observe the X-ray binary pulsar A0535+26. The main objectives is measuring changes in the cyclotron resonance energy in an outburst decay.It is known from another X-ray pulsar 4U0115+63 that the cyclotron resonance energy increased from 11 keV to 16 keV, as the luminosity decreased across a threshold luminosity of 4x10^37 erg/s. The flare of A0535+26 is a chance to know whether this behavior is the RULE among binary pulsars or an EXCEPTION. A0535+26 is fading down and will reach 30mCrab (5-100keV) on September 17, which is 5x10^36 erg/s. It is better to be observed as soon as possible, before it fades out.	CALIBRATION	1	A	SWG		JAP	0	SWG	TOO Observation of A0535+026		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100021010/	Quick Look
51	Crab nebula	83.7552	22.0249	83.002845	21.992803	84.212769	-1.290605	184.60948321	-5.68314749	86.8656	53609.2022106482	2005-08-27 04:51:11	53609.3125810185	2005-08-27 07:30:07	100010140	3.419	5	3.419	3.419	3.419	3.419	1	1	1	1	1	0	0	3.7554	3.7554	9.5319	0	PROCESSED	57526.9383217593	2016-05-18 22:31:11	54247	2007-05-27 00:00:00	54118.9983796296	2007-01-18 23:57:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010140/	Quick Look
52	Crab Nebula	83.6309	22.0151	82.87863	21.982404	84.097185	-1.295359	184.55585082	-5.78574816	87.8466	53628.8269212963	2005-09-15 19:50:46	53629.0904976852	2005-09-16 02:10:19	100023020	12.5271	10	12.5311	12.5271	12.5364	12.5351	2	2	2	2	1	0	0	13.3529	13.3529	22.764	1	PROCESSED	57527.3409143518	2016-05-19 08:10:55	54247	2007-05-27 00:00:00	54109.193599537	2007-01-09 04:38:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000023	Calibration of detector response at both of XIS/HXD nominal positions, together with an absolute flux confirmation with differnt hit-pattern widths.	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab at nominal positions		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100023020/	Quick Look
53	NGC 2110	88.0444	-7.458	87.440268	-7.468978	87.743148	-30.884192	212.92660512	-16.54877043	103.4188	53629.3796296296	2005-09-16 09:06:40	53631.8308333333	2005-09-18 19:56:24	100024010	101.7487	100	101.9265	103.7601	101.7487	102.1483	2	2	2	2	1	0	0	86.0433	86.0433	211.7558	4	PROCESSED	57527.4030324074	2016-05-19 09:40:22	54247	2007-05-27 00:00:00	54035.4624189815	2006-10-27 11:05:53	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000024	The Narrow Emission Line Galaxy NGC 2110 was the brightest AGN in the initial BAT survey release (BAT flux of 2.1E-10 erg/cm2/sec) visible to Suzaku during Sept./Oct., and is still currently bright in BAT. A 2003 RXTE observation yielded F_2-10 keV = 4E-11 erg/cm2/sec. The source is currently almost 3 times brighter than during the SAX observations. The main goals are to measure the high energy cutoff and to place a strong limit on the presence of reflection. The Compton reflection hump is weak in SAX data (suggesting that the Fe K line originates in Compton-thin material). Determining the strength of the reflection component is critical for constraining the geometry of the accreting material.	CALIBRATION	1	A	SWG		JAP	0	SWG	Narrow Emission Line Galaxy NGC 2110		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100024010/	Quick Look
54	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
55	SS 433	287.9527	4.99	287.334904	4.905608	290.182673	27.181461	39.69879316	-2.23786427	78.6446	53833.4611458333	2006-04-08 11:04:03	53834.4579166667	2006-04-09 10:59:24	401004010	40.1976	40	40.2216	40.1976	40.2296	40.2136	2	2	2	2	1	0	0	30.4749	30.4749	86.11	2	PROCESSED	57533.4357638889	2016-05-25 10:27:30	54400	2007-10-27 00:00:00	53906.5501736111	2006-06-20 13:12:15	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010031	SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber.	GALACTIC POINT SOURCES	4	A	NOBUYUKI KAWAI		JAP	1	AO1	SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401004010/	Quick Look
56	MRK 1073	48.7759	41.9723	47.948749	41.787366	57.835678	23.02641	149.56255257	-13.3516285	258.3737	54135.7651851852	2007-02-04 18:21:52	54136.6641087963	2007-02-05 15:56:19	701007020	39.5111	40	39.5191	39.5111	0	39.5191	2	2	0	2	1	0	0	37.1814	37.1814	77.6519	0	PROCESSED	57537.3263657407	2016-05-29 07:49:58	54735	2008-09-26 00:00:00	54151.4969444445	2007-02-20 11:55:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010037	We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	1	AO1	COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701007020/	Quick Look
57	1E1207.4-5209	182.4916	-52.442	181.83735	-52.163724	209.144209	-45.784625	296.53791481	9.91413144	148.6893	54146.2087384259	2007-02-15 05:00:35	54147.6390509259	2007-02-16 15:20:14	401030020	49.8266	50	50.0734	49.8266	0	50.0894	1	2	0	1	1	0	0	44.4468	44.4468	123.576	2	PROCESSED	57537.4372337963	2016-05-29 10:29:37	54750	2008-10-11 00:00:00	54153.9886458333	2007-02-22 23:43:39	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010152	1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object.	GALACTIC POINT SOURCES	4	B	ATSUMASA YOSHIDA		JAP	1	AO1	A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401030020/	Quick Look
58	V1223 SGR	283.7445	-31.105	282.940068	-31.169256	281.851865	-8.228404	5.0082738	-14.31987205	79.9528	54203.4803240741	2007-04-13 11:31:40	54204.9418055556	2007-04-14 22:36:12	402002010	60.706	60	60.706	60.706	0	60.706	2	2	0	2	1	0	0	46.2861	46.2861	126.2719	2	PROCESSED	57538.1822800926	2016-05-30 04:22:29	54744	2008-10-05 00:00:00	54210.6596875	2007-04-20 15:49:57	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020008	The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS.	GALACTIC POINT SOURCES	4	A	MANABU ISHIDA		JAP	2	AO2	MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402002010/	Quick Look
59	PSR B1259-63	195.6556	-63.8839	194.86632	-63.61523	227.712317	-50.941906	304.16255435	-1.03887935	293.4832	54304.2811226852	2007-07-23 06:44:49	54304.6877777778	2007-07-23 16:30:24	402014050	19.7023	20	19.7023	19.7023	0	19.7023	1	1	0	1	1	0	0	17.7549	17.7549	35.1279	0	PROCESSED	57539.3024768518	2016-05-31 07:15:34	54707	2008-08-29 00:00:00	54339.2175347222	2007-08-27 05:13:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014050/	Quick Look
60	LS 5039	276.5633	-14.9109	275.848755	-14.941003	276.400444	8.383997	16.82651822	-1.31880921	270.412	54352.6780555556	2007-09-09 16:16:24	54358.4725	2007-09-15 11:20:24	402015010	203.2399	200	203.2399	203.2399	0	203.2399	2	2	0	2	1	0	0	181.095	181.095	442.0879	4	PROCESSED	57540.0947685185	2016-06-01 02:16:28	54745	2008-10-06 00:00:00	54384.7259027778	2007-10-11 17:25:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020062	The periodicity of TeV gamma-rays from the Galactic microquasar LS 5039 has recently been detected by the HESS Cherenkov telescope. We propose to conduct a simultaneous X-ray/VHE gamma-ray observations for a total of 200 ks of the microquasar with Suzaku XIS and HXD in conjuction with the HESS telescope. A full orbital period of 3.9 days is planned to be covered with Suzaku and HESS. The goal of this program is to study a possible correlation of X-TeV fluxes and spectral changes as a function of orbital phase, thereby shedding a new light on the origin of high-energy radiation from the microquasar system.	GALACTIC POINT SOURCES	4	A	TADAYUKI TAKAHASHI		JAP	2	AO2	SIMULTANEOUS SUZAKU AND HESS OBSERVATIONS OF THE TEV GAMMA-RAY MICROQUASAR LS 5039	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402015010/	Quick Look
61	SN1006 SW-Rim	225.5051	-42.0698	224.686984	-41.873221	235.327536	-23.832864	327.36692545	14.52303039	297.2712	53623.5862962963	2005-09-10 14:04:16	53624.993287037	2005-09-11 23:50:20	100019030	28.5245	50	28.5325	28.5245	28.5409	28.5405	2	2	2	2	1	0	0	27.0082	27.0082	121.5519	5	PROCESSED	57527.3126967593	2016-05-19 07:30:17	54247	2007-05-27 00:00:00	54034.9697453704	2006-10-26 23:16:26	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000019		CALIBRATION	1	A	SWG		JAP	0	SWG	SN1006 observation with XIS and HXD		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019030/	Quick Look
62	4U 1700+24	256.6316	23.9071	256.110961	23.972677	252.098688	46.519124	45.07419011	32.98144858	280.149	54334.7787615741	2007-08-22 18:41:25	54335.875162037	2007-08-23 21:00:14	402023010	50.2445	50	50.2525	50.2605	0	50.2445	2	2	0	2	1	0	0	45.3268	45.3268	94.7158	2	PROCESSED	57539.6636226852	2016-05-31 15:55:37	54723	2008-09-14 00:00:00	54350.4606481482	2007-09-07 11:03:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020105	We propose the observation of Neutron Star Low Mass X-ray Binary (LMXB) system 4U 1700+24.This system would be Advection Dominant Accretion Flow (ADAF) and we research the hard-tail in hard X-ray region. Though the X-ray intensity in a Low Hard state is very faint, $sim$10$^{33}$ erg/s we can obtain the energy spectrum of 10-100keV for the first time using Suzaku 50ksec observation because it is the nearest LMXB. If we know the extension of hard-tail in low luminosity state, we can understand the physical state of electron in the accretion disk and/or compact object. Suzaku is the best satellite to research the faint emission around 100keV.	GALACTIC POINT SOURCES	4	B	OSAMU NAGAE		JAP	2	AO2	STUDY OF MASS ACCRETION FLOW IN ADAF FOR LOW LUMINOUS X-RAY BINARY 4U 1700+24	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402023010/	Quick Look
63	CYG OB2 ASSOCIATION	308.2175	41.2935	307.768848	41.122144	329.008943	57.17316	80.16491027	0.83267098	220.3949	54452.9185532407	2007-12-18 22:02:43	54453.843912037	2007-12-19 20:15:14	402030010	41.1147	40	41.1147	41.1147	0	41.1147	2	2	0	2	1	0	0	37.9181	37.9181	79.9439	0	PROCESSED	57540.9006597222	2016-06-01 21:36:57	54828	2008-12-28 00:00:00	54460.6521643518	2007-12-26 15:39:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020150	Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku.	GALACTIC POINT SOURCES	4	C	SHUNJI KITAMOTO		JAP	2	AO2	STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402030010/	Quick Look
64	EMS0071	16.6433	48.9425	15.913472	48.675321	36.903288	38.099489	125.49064727	-13.85403968	69.9406	55392.4123148148	2010-07-15 09:53:44	55392.8855092593	2010-07-15 21:15:08	705010010	23.0102	20	23.0102	23.0102	0	23.0102	2	2	0	2	1	0	0	19.568	19.568	40.8819	0	PROCESSED	57552.6419560185	2016-06-13 15:24:25	55779	2011-08-06 00:00:00	55411.2637384259	2010-08-03 06:19:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050050	We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators".	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5	SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705010010/	Quick Look
65	BD +30 3639	293.6993	30.5065	293.208675	30.395694	303.554886	51.223276	64.78119899	5.00649051	237.7342	53676.9934837963	2005-11-02 23:50:37	53677.8230324074	2005-11-03 19:45:10	100025020	31.1384	40	31.1384	31.1624	31.1464	31.1544	2	2	2	2	1	0	0	27.1258	27.1258	71.638	1	PROCESSED	57527.9315509259	2016-05-19 22:21:26	54247	2007-05-27 00:00:00	54037.1080902778	2006-10-29 02:35:39	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000025	The proposed target, BD +30 3639, is a prototypical planetary nebula which emit diffuse X-rays; planetary nebulae represent the final evolutionary stage of low mass stars, and contain very rich information on the stellar nucleosynthesis. The Chandra ACIS spectrum of BD +30 3639 bears an amazingly strong Ne-K line, most certainly because the X-ray emitting material directly reflect the "onion-like structure" of elements insied evolved stars. However, the ACIS was not able to resolve C, N, O lines, which are of vital importance. The XMM RGS and Chandra LETG could do, but we need very long exposure. Using the Suzaku XIS-BI with the excellent low-energy performance, we can for the first time measure the C/N/O/Mg abundance ratios of this important object in a short time.	CALIBRATION	1	A	SWG		JAP	0	SWG	Observation of planetary nebula BD +30 3639		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100025020/	Quick Look
66	KS1741-293(GC_BGD_2)	266.2069	-29.3515	265.410046	-29.331146	266.666918	-5.954235	359.55541243	-0.06909433	265.0174	53637.5288541667	2005-09-24 12:41:33	53637.5946296296	2005-09-24 14:16:16	100027040	1.937	5	1.937	1.937	1.937	1.937	1	1	1	1	1	0	0	1.7637	1.7637	5.68	0	PROCESSED	57527.404525463	2016-05-19 09:42:31	54247	2007-05-27 00:00:00	53907.393275463	2006-06-21 09:26:19	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000027	We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.	CALIBRATION	1	A	SWG		JAP	0	SWG	Suzaku Observation of Galactic Center Region		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027040/	Quick Look
67	HESS J1616-508_BGD2	244.4656	-50.6883	243.5199	-50.566183	251.824242	-28.844194	332.70353325	-0.14997577	283.1793	53633.8196412037	2005-09-20 19:40:17	53634.3120833333	2005-09-21 07:29:24	100028030	21.8735	25	21.8895	21.8895	21.8815	21.8735	1	1	1	1	1	0	0	18.2063	18.2063	42.5359	0	PROCESSED	57527.3722800926	2016-05-19 08:56:05	54247	2007-05-27 00:00:00	54035.4698842593	2006-10-27 11:16:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000028		CALIBRATION	1	A	SWG		JAP	0	SWG	New HESS sources and the Galactic ridge Background		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100028030/	Quick Look
68	GC_SOUTH_1	268.0988	-29.4771	267.30082	-29.465922	268.32614	-6.047082	0.29758282	-1.54591478	274.6002	56190.0385069444	2012-09-20 00:55:27	56191.3341435185	2012-09-21 08:01:10	507028010	51.7619	50	51.7619	51.7699	0	51.7699	3	3	0	3	1	0	0	41.1534	41.1534	111.9318	1	PROCESSED	57607.1304398148	2016-08-07 03:07:50	56584	2013-10-19 00:00:00	56218.5464930556	2012-10-18 13:06:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070042	We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation.	GALACTIC DIFFUSE EMISSION	5	A	SHINYA NAKASHIMA		JAP	7	AO7	OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507028010/	Quick Look
69	ULXs in NGC 1313	49.5245	-66.5352	49.373425	-66.716272	341.380796	-74.178462	283.41323765	-44.63106544	172.6337	53658.556400463	2005-10-15 13:21:13	53659.6252777778	2005-10-16 15:00:24	100032010	32.878	40	32.878	32.878	32.878	32.878	1	1	1	1	1	0	0	30.38	30.38	92.3439	1	PROCESSED	57527.587349537	2016-05-19 14:05:47	54247	2007-05-27 00:00:00	54036.1929398148	2006-10-28 04:37:50	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000032	We propose Suzaku observation of a nearby (4.5 Mpc) galaxy NGC 1313 hosting two prototypical ULXs. These ASCA specta of many ULXs were described with a "high temperature diskbb" model, spectra obtained with XMM (and Chandra) prefer a "power-law plus low-temperature disk" modeling. The superior 5-10 keV sensitivity of Suzaku allows us to examine whether the spectra of luminous ULXs indeed exhibit a turn-over around 5 keV or extend up to 10 keV.	CALIBRATION	1	A	SWG		JAP	0	SWG	ULXs in NGC 1313		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100032010/	Quick Look
70	JUPITER	104.4639	23.0622	103.708176	23.129949	103.287865	0.285992	192.81439153	11.62759441	264.6138	56767.1149421296	2014-04-20 02:45:31	56767.448125	2014-04-20 10:45:18	508023110	16.7417	160	16.7417	16.7737	0	16.7657	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57614.9630671296	2016-08-14 23:06:49	57212	2015-07-09 00:00:00	56789.801712963	2014-05-12 19:14:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023110/	Quick Look
71	CYGNUS LOOP BLOWOUT3	312.3799	29.0257	311.853293	28.839005	325.853846	44.599011	72.47923846	-9.33489782	78.1517	55688.6493981482	2011-05-07 15:35:08	55689.9654976852	2011-05-08 23:10:19	506013010	60.2669	60	60.2669	60.2749	0	60.2669	2	2	0	2	1	0	0	55.9803	55.9803	113.6288	1	PROCESSED	57601.9873611111	2016-08-01 23:41:48	56066	2012-05-19 00:00:00	55700.4602083333	2011-05-19 11:02:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060053	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	6	AO6	MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506013010/	Quick Look
72	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
73	A 3376	90.5561	-39.9584	90.148808	-39.956705	90.960808	-63.398292	246.50686261	-25.98989573	107.6124	53649.6153703704	2005-10-06 14:46:08	53653.4495833333	2005-10-10 10:47:24	100034010	118.7792	150	118.7792	121.7373	118.8498	119.3357	2	2	2	2	1	0	0	100.5401	100.5401	331.2537	3	PROCESSED	57527.6218171296	2016-05-19 14:55:25	54247	2007-05-27 00:00:00	54109.6396990741	2007-01-09 15:21:10	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000034	Abell 3376 (z=0.046) is a merging cluster with a T=4 keV (*3) hosting a pair of strong radio halos (see figure). It is one of the few clusters from which BeppoSAX positively detected excess hard X-rays (Nevalainen et al. ApJ 608, 166, 2004). Because of the relatively low temperature, the HXD-PIN energy band is expected to be relatively free from thermal emission, making this object ideal to the search for non-thermal signals. We expect the non-thermal flux to be 4-5% of the PIN background at 20 keV, and a 150 ksec on-source exposure would be needed to securely detect this. To know the current background over the full COR range, an off-source exposure for one day or a ~40 ksec exposure onto a very soft source, would be required immediately before or after the on-source data acquisition.	CALIBRATION	1	A	SWG		JAP	0	SWG	Diffuse Hard X-rays from Clusters		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100034010/	Quick Look
74	1E1743.1-2843 GCBGD3	266.5944	-28.6526	265.801896	-28.634135	266.98972	-5.247071	0.32852719	0.00581314	264.8798	53644.2657523148	2005-10-01 06:22:41	53644.3162268518	2005-10-01 07:35:22	100037050	2.4	5	2.4	2.4	2.4	2.4	2	2	2	2	1	0	0	2.2329	2.2329	4.3539	0	PROCESSED	57527.4530902778	2016-05-19 10:52:27	54247	2007-05-27 00:00:00	54056.1970833333	2006-11-17 04:43:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000037		CALIBRATION	1	A	SWG		JAP	0	SWG	Suzaku Obseration of Galactic Center region 2		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037050/	Quick Look
75	1E 1048.1-5937	162.5452	-59.8394	162.049535	-59.57411	203.219635	-58.558248	288.24102095	-0.47209541	101.4368	54800.9597337963	2008-11-30 23:02:01	54802.5927083333	2008-12-02 14:13:30	403005010	100.4231	100	100.443	100.4231	0	100.4231	2	2	0	2	1	0	0	68.1049	68.1049	141.0819	0	PROCESSED	57544.6078472222	2016-06-05 14:35:18	55178	2009-12-13 00:00:00	54812.0471875	2008-12-12 01:07:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030013	Observations in soft X-ray through hard X-ray bands are key to understand the emission processes in the magnetosphere of Anomalous X-ray Pulsars (AXPs). We propose to observe the two AXPs, 1E 2259+586 and 1E 1048.1-5937, with SUZAKU. Although no detections of the hard X-ray emissions have been reported, the results of the simulation using XSPEC for HXD indicate that SUZAKU detects the hard X-ray emissions above 20~keV from both AXPs for the first time with a quite high probability. The time resolution of HXD is able to provide the pulse profiles and the phase-resolved spectra in hard X-rays emissions. With these results of the observations, SUZAKU will provide a crucial information to study the emission processes in the magnetosphere of AXPs.	GALACTIC POINT SOURCES	4	C	JUMPEI TAKATA		JAP	3	AO3	X-RAY OBSERVATIONS OF ANOMALOUS X-RAY PULSARS WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403005010/	Quick Look
76	MARS-P3	102.9612	25.1565	102.192848	25.217116	101.724463	2.241555	190.28784034	11.26022306	298.032	54559.4933796296	2008-04-03 11:50:28	54559.5766087963	2008-04-03 13:50:19	403006030	3.886	100	3.886	3.91	0	3.894	1	1	0	1	1	0	0	3.1134	3.1134	7.1839	0	PROCESSED	57542.0373148148	2016-06-03 00:53:44	54953	2009-05-02 00:00:00	54577.0484259259	2008-04-21 01:09:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006030/	Quick Look
77	MARS-P11	103.2936	25.1207	102.525618	25.182892	102.027614	2.233108	190.44969799	11.5184009	298.1493	54560.1601041667	2008-04-04 03:50:33	54560.2433333333	2008-04-04 05:50:24	403006110	4.6198	100	4.6278	4.6198	0	4.6358	1	1	0	1	1	0	0	4.0749	4.0749	7.1839	0	PROCESSED	57542.0559490741	2016-06-03 01:20:34	54953	2009-05-02 00:00:00	54577.1745023148	2008-04-21 04:11:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006110/	Quick Look
78	MARS-P13	103.3779	25.1101	102.610021	25.172691	102.104653	2.229561	190.49210676	11.58330245	298.1799	54560.3267708333	2008-04-04 07:50:33	54560.41	2008-04-04 09:50:24	403006130	4.2518	100	4.2678	4.2518	0	4.2678	1	1	0	1	1	0	0	3.529	3.529	7.1839	0	PROCESSED	57542.0605671296	2016-06-03 01:27:13	54953	2009-05-02 00:00:00	54577.9292939815	2008-04-21 22:18:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006130/	Quick Look
79	MARS-P16	103.503	25.0968	102.735261	25.159983	102.218767	2.2268	190.55275085	11.68067717	298.2223	54560.5768171296	2008-04-04 13:50:37	54560.66	2008-04-04 15:50:24	403006160	2.3262	100	2.3262	2.3262	0	2.3262	2	2	0	2	1	0	0	2.134	2.134	7.1799	0	PROCESSED	57542.0664236111	2016-06-03 01:35:39	54953	2009-05-02 00:00:00	54577.9478935185	2008-04-21 22:44:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006160/	Quick Look
80	MARS-P21	103.7101	25.0688	102.942627	25.132964	102.408276	2.21649	190.65860601	11.8395058	298.2947	54560.9933217593	2008-04-04 23:50:23	54561.0765509259	2008-04-05 01:50:14	403006210	2.8808	100	2.8808	2.8808	0	2.8808	1	1	0	1	1	0	0	3.4516	3.4516	7.1839	0	PROCESSED	57542.0774884259	2016-06-03 01:51:35	54953	2009-05-02 00:00:00	54578.0612847222	2008-04-22 01:28:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006210/	Quick Look
81	MARS-P23	103.7955	25.0599	103.028122	25.124467	102.486187	2.214951	190.69976585	11.90614711	298.325	54561.1600347222	2008-04-05 03:50:27	54561.2432175926	2008-04-05 05:50:14	403006230	4.5188	100	4.5268	4.5188	0	4.5348	1	1	0	1	1	0	0	3.6868	3.6868	7.1839	0	PROCESSED	57542.0791898148	2016-06-03 01:54:02	54953	2009-05-02 00:00:00	54578.1176157407	2008-04-22 02:49:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006230/	Quick Look
82	MARS-P25	103.8803	25.0503	103.113021	25.115268	102.56363	2.212708	190.74132534	11.97202775	298.3546	54561.3266550926	2008-04-05 07:50:23	54561.4098842593	2008-04-05 09:50:14	403006250	4.2612	100	4.2692	4.2612	0	4.2692	1	1	0	1	1	0	0	3.2511	3.2511	7.1839	0	PROCESSED	57542.2336458333	2016-06-03 05:36:27	54953	2009-05-02 00:00:00	54578.1323032407	2008-04-22 03:10:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006250/	Quick Look
83	MARS-P26	103.921	25.0474	103.153759	25.112561	102.600638	2.213348	190.75967691	12.00436516	298.3671	54561.4100347222	2008-04-05 09:50:27	54561.4932175926	2008-04-05 11:50:14	403006260	4.7976	100	4.8136	4.7976	0	4.8216	1	1	0	1	1	0	0	3.7622	3.7622	7.1839	0	PROCESSED	57542.2337962963	2016-06-03 05:36:40	54953	2009-05-02 00:00:00	54578.1374074074	2008-04-22 03:17:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006260/	Quick Look
84	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
85	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
86	NORTH POLAR SPUR	260.5905	4.7489	259.972652	4.795886	259.371969	27.842624	26.83412197	21.95376599	264.1143	53646.4785763889	2005-10-03 11:29:09	53647.4515277778	2005-10-04 10:50:12	100038010	43.0689	50	43.1489	44.2129	43.0689	43.2929	2	2	2	2	1	0	0	40.7715	40.7715	84.0019	0	PROCESSED	57527.5342824074	2016-05-19 12:49:22	54247	2007-05-27 00:00:00	54035.8928009259	2006-10-27 21:25:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000038	We propose to observe the North Polar Spur for 100 ksec. The main objectives are below (1) Search for emission lines of N and C that originates from low kT emission (2) Precisely determine the abundance of the NPS The measurement of N and C lines will be the first for XIS. This is also the first for extended sources. The first trial to measure the emission from the C-band (below 0.3keV) by using BI. This will be a guide line how to use the C-band data. Since the C-band intensity is already known, this will be the first calibration of the BI at low energy. The scientific objectives are already given in the mail distributed in the swg.	CALIBRATION	1	A	SWG		JAP	0	SWG	North Polar Spur		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100038010/	Quick Look
87	ARCHES CLUSTER	266.4808	-28.778	265.687528	-28.758983	266.892731	-5.374834	0.16960578	0.02569084	109.9998	54911.0857407407	2009-03-21 02:03:28	54913.7681712963	2009-03-23 18:26:10	403009010	110.7933	100	110.7933	110.7933	0	110.7933	2	2	0	2	1	0	0	91.6578	91.6578	231.7417	3	PROCESSED	57545.9555787037	2016-06-06 22:56:02	55330	2010-05-14 00:00:00	54924.3822106482	2009-04-03 09:10:23	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030029	We propose to observe a hard X-ray ring which has an emission line around 6.4 keV, located at the north of the Arches cluster. The ring is probably produced by an energetic jet or a supernova explosion. We aim to determine the continuum shape, the center energy of the emission line, and the absorption column to figure out the origin of the ring.	GALACTIC POINT SOURCES	4	B	MASAHIRO TSUJIMOTO		JAP	3	AO3	A 6.4 KEV RING AT THE NORTH OF THE ARCHES CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403009010/	Quick Look
88	LS I+61 303_1	40.1455	61.188	39.183267	60.973753	59.828193	42.868734	135.69810374	1.0510579	270.0003	54853.9515856482	2009-01-22 22:50:17	54854.8648032407	2009-01-23 20:45:19	403015010	40.5514	40	40.5514	40.5514	0	40.5514	2	2	0	2	1	0	0	25.7312	25.7312	78.868	0	PROCESSED	57545.3022916667	2016-06-06 07:15:18	55329	2010-05-13 00:00:00	54880.5343865741	2009-02-18 12:49:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030077	We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST.	GALACTIC POINT SOURCES	4	A	YASUSHI FUKAZAWA		JAP	3	AO3	X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403015010/	Quick Look
89	LS I+61 303_2	40.1457	61.1877	39.18347	60.973453	59.828143	42.868421	135.69831419	1.05082335	270.0006	54856.6966087963	2009-01-25 16:43:07	54858.1766666667	2009-01-27 04:14:24	403016010	61.0667	60	61.0784	61.0667	0	61.0784	2	2	0	2	1	0	0	26.6591	26.6591	127.8398	1	PROCESSED	57545.3828819444	2016-06-06 09:11:21	55329	2010-05-13 00:00:00	54880.5522106482	2009-02-18 13:15:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030077	We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST.	GALACTIC POINT SOURCES	4	A	YASUSHI FUKAZAWA		JAP	3	AO3	X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403016010/	Quick Look
90	LS I+61 303_3	40.2018	61.1949	39.239095	60.980826	59.865781	42.86376	135.72005286	1.06843757	246.2753	54872.1842592593	2009-02-10 04:25:20	54873.7252199074	2009-02-11 17:24:19	403017010	68.6273	60	68.6273	68.6273	0	68.6273	2	2	0	2	1	0	0	65.0685	65.0685	133.1218	1	PROCESSED	57545.5290856482	2016-06-06 12:41:53	55330	2010-05-14 00:00:00	54893.4210300926	2009-03-03 10:06:17	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030077	We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST.	GALACTIC POINT SOURCES	4	A	YASUSHI FUKAZAWA		JAP	3	AO3	X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403017010/	Quick Look
91	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
92	IGR J16194-2810	244.8908	-28.0663	244.116394	-27.946439	247.849887	-6.534784	349.1669856	15.58223604	95.1879	54867.1762152778	2009-02-05 04:13:45	54868.4314236111	2009-02-06 10:21:15	403024010	45.5687	50	45.5687	45.5738	0	45.5687	2	2	0	2	1	0	0	38.7859	38.7859	108.4358	1	PROCESSED	57545.4895023148	2016-06-06 11:44:53	55329	2010-05-13 00:00:00	54880.5743518518	2009-02-18 13:47:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030121	We propose to observe the weakly magnetized neutron star X-ray binary, IGR J16194-2810. This target object has almost constant luminosity and is expected to be state of ADAF. Assuming that we observe the object using HXD and XIS of the Suzaku for 50ks, we can investigate the soft X-ray emission from the NS and/or the accretion disk and hard X-ray tail. Comparing Black Body and Disk Black Body parameters of this object with that of fainter source, 4U 1700+24, we obtain a picture of accretion disk and accretion flow. If we measure the photon index and cutoff energy of the hard tail, we can reveal the physical condition of corona surrounding the NS or the disk. Only Suzaku can carry out this observation which observe soft-thermal and hard-nonthermal X-ray emission from faint source.	GALACTIC POINT SOURCES	4	C	OSAMU NAGAE		JAP	3	AO3	ELUCIDATION OF THE ADAF OBSERVING LOW LUMINOUS NEUTRON STAR X-RAY BINARY IGR J16194-2810	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403024010/	Quick Look
93	V709 CAS	7.1951	59.3013	6.498819	59.024957	38.349683	49.774418	120.03837674	-3.44309479	84.0816	54637.4334837963	2008-06-20 10:24:13	54638.1542824074	2008-06-21 03:42:10	403025010	35.8982	30	35.8982	35.8982	0	35.8982	2	2	0	2	1	0	0	33.3823	33.3823	62.2679	0	PROCESSED	57542.8811921296	2016-06-03 21:08:55	55014	2009-07-02 00:00:00	54648.3358101852	2008-07-01 08:03:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030140	Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	3	AO3	IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403025010/	Quick Look
94	RX J1940.1-1025	295.0445	-10.4193	294.356962	-10.535652	295.074294	10.867465	28.98688715	-15.49869645	79.7405	54572.8979976852	2008-04-16 21:33:07	54573.743275463	2008-04-17 17:50:19	403027010	32.4536	30	32.4536	32.4536	0	32.4536	2	2	0	2	1	0	0	26.4657	26.4657	73.0219	2	PROCESSED	57542.3241087963	2016-06-03 07:46:43	54953	2009-05-02 00:00:00	54587.0481481482	2008-05-01 01:09:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030140	Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	3	AO3	IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403027010/	Quick Look
95	Crab Nebula	83.6372	22.097	82.884469	22.064333	84.106634	-1.213794	184.48946706	-5.73697	84.9994	53613.8323032407	2005-08-31 19:58:31	53613.975787037	2005-08-31 23:25:08	100015010	5.6587	5	5.6587	5.6587	5.6587	5.6587	1	1	1	1	1	0	0	5.7907	5.7907	12.3879	0	PROCESSED	57527.2296412037	2016-05-19 05:30:41	54247	2007-05-27 00:00:00	54109.1053240741	2007-01-09 02:31:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000015		CALIBRATION	1	A	SWG		JAP	0	SWG	HXD boresight check with Crab		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015010/	Quick Look
96	GS 1826-238	277.3735	-23.8572	276.610421	-23.891095	276.73109	-0.588705	9.22092987	-6.12003001	267.2862	55125.8488310185	2009-10-21 20:22:19	55127.9502777778	2009-10-23 22:48:24	404007010	102.5154	100	102.5154	102.5314	0	102.5372	2	2	0	2	1	0	0	87.9996	87.9996	181.5418	2	PROCESSED	57549.0104976852	2016-06-10 00:15:07	55534	2010-12-04 00:00:00	55166.4220833333	2009-12-01 10:07:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040035	We propose a 100 ksec Suzaku observation of the neutron star (NS) binary GS 1826-238. It is already known that there is a high energy cutoff at around 150 keV in the hard state of black hole candidates (BNCs). Additional non-thermal spectrum above 300 keV has sometimes been verified by gamma-ray observatories. Some NS binaries exhibit a 'hard state' which shows X-ray properties similar to those observed in hard state BHCs. Their cutoff energies (~50 keV) are systematically lower than those of BHCs, but firm detections of non-thermal emissions are not reported so far. This proposal is aimed at the first detection of the non-thermal hard tail from this source in the steady 'hard state', and verification of its possible jet origin via simultaneous radio, near-IR, and optical observations.	GALACTIC POINT SOURCES	4	B	KAZUTAKA YAMAOKA		JAP	4	AO4	SEARCH FOR A NON-THERMAL HARD TAIL FROM THE NEUTRON STAR BINARY GS 1826-238	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404007010/	Quick Look
97	EUVE J0317-85.5	48.9864	-85.5003	51.11405	-85.679196	278.533864	-69.749958	299.84736337	-30.72881529	65.46	55028.6017476852	2009-07-16 14:26:31	55030.1460185185	2009-07-18 03:30:16	404019010	63.0843	60	63.0843	63.0843	0	63.0843	2	2	0	2	1	0	0	56.8965	56.8965	133.4138	1	PROCESSED	57547.8712847222	2016-06-08 20:54:39	55406	2010-07-29 00:00:00	55040.2674305556	2009-07-28 06:25:06	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040083	Where is the particle acceleration site in the universe? The Cosmic-ray origin is the long standing mystery for near 100 years. The first discovery of "the white dwarf pulsar" in the AE Aquarii system with Suzaku is one of the most important step in this study, because Suzaku demonstrated the possibility of particle acceleration in white dwarfs. The next important step is to search for the sign of non-thermal emission from a NORMAL white dwarf. Here, we propose the Suzaku observation of an isolated white dwarf EUVE J0317-85.5, which has very high magnetic field strength of 450 MG and very fast rotation period 725 sec among this type of objects.	GALACTIC POINT SOURCES	4	B	ATSUSHI HARAYAMA		JAP	4	AO4	FIRST SEARCH FOR NON THERMAL EMISSION FROM AN ISOLATED MAGNETIZED WHITE DWARF	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404019010/	Quick Look
98	TT ARI	31.7181	15.2972	31.038138	15.059527	34.795947	2.311089	148.52228749	-43.79443	71.0668	55018.4424652778	2009-07-06 10:37:09	55019.3023611111	2009-07-07 07:15:24	404021010	35.7421	35	35.7421	35.7796	0	35.7876	2	2	0	2	1	0	0	31.794	31.794	74.2578	1	PROCESSED	57547.7822453704	2016-06-08 18:46:26	55399	2010-07-22 00:00:00	55029.236712963	2009-07-17 05:40:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040095	The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail.	GALACTIC POINT SOURCES	4	B	KEI SAITOU		JAP	4	AO4	IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404021010/	Quick Look
99	TX COL	85.7822	-41.0648	85.383592	-41.086265	82.635964	-64.399356	246.79781267	-29.77494364	322.4827	54963.6800578704	2009-05-12 16:19:17	54965.2502199074	2009-05-14 06:00:19	404031010	59.7818	40	59.7898	59.7898	0	59.7818	2	2	0	2	1	0	0	51.123	51.123	135.654	0	PROCESSED	57546.5734143518	2016-06-07 13:45:43	55345	2010-05-29 00:00:00	54978.2105439815	2009-05-27 05:03:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040113	We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.	GALACTIC POINT SOURCES	4	A	TAKAYUKI YUASA		JAP	4	AO4	SURVEY OBSERVATION OF INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404031010/	Quick Look
100	Crab nebula	83.6105	22.3483	82.856361	22.315501	84.093042	-0.96164	184.26290563	-5.62323625	86.8596	53607.2790509259	2005-08-25 06:41:50	53607.5139583333	2005-08-25 12:20:06	100010030	8.1129	5	8.1129	8.1129	8.1129	8.1129	2	2	2	2	1	0	0	7.8359	7.8359	20.264	1	PROCESSED	57526.8876388889	2016-05-18 21:18:12	54247	2007-05-27 00:00:00	54118.9698958333	2007-01-18 23:16:39	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010030/	Quick Look
101	DA 240 EAST LOBE	117.3573	55.877	116.349381	56.002734	108.151975	34.146502	161.8466677	30.16323196	293.7777	55274.9306134259	2010-03-19 22:20:05	55276.7238657407	2010-03-21 17:22:22	704020010	81.7834	80	81.7834	81.7914	0	81.7914	2	2	0	2	1	0	0	74.3033	74.3033	154.9218	1	PROCESSED	57550.9753587963	2016-06-11 23:24:31	55654	2011-04-03 00:00:00	55286.3268518518	2010-03-31 07:50:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040096	Suzaku observations of two giant radio galaxies, 3C 35 and DA 240, with a total size of about 1 Mpc are proposed, in order to detect diffuse inverse Compton X-ray emission from their radio lobes. The X-ray flux from the lobes, in comparison with the radio one, provides a precise determination of electron and magnetic field energies there. A comparison of them with those in smaller radio galaxies is used to probe into the history of jets and lobes.	EXTRAGALACTIC COMPACT SOURCES	7	B	NAOKI ISOBE		JAP	4	AO4	SUZAKU OBSERVATION OF GIANT RADIO GALAXIES AS A PROBE OF JET HISTORY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704020010/	Quick Look
102	N132D	81.2794	-69.6524	81.381964	-69.694399	312.375338	-85.522525	280.31514531	-32.77566051	53.3291	53595.4703125	2005-08-13 11:17:15	53597.5313541667	2005-08-15 12:45:09	100002010	7.4066	80	7.4066	7.4066	7.4066	7.4066	2	2	2	2	0	0	0	0	0	0	0	PROCESSED	57520.7109606482	2016-05-12 17:03:47	54247	2007-05-27 00:00:00	54038.5875925926	2006-10-30 14:06:08	3.0.22.43	6	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000002	HXD HV ON WITH N132D, and 5 pointings with XIS	CALIBRATION	1	A	SWG		JAP	0	SWG	HXD HV ON WITH N132D		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100002010/	Quick Look
103	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
104	V773TAU	63.5571	28.1952	62.783682	28.069565	66.716115	6.867305	168.22500409	-16.34364304	260.6557	55610.1581712963	2011-02-18 03:47:46	55611.9815277778	2011-02-19 23:33:24	405011010	82.2463	80	82.2543	82.2463	0	82.2543	2	2	0	2	1	0	0	72.8287	72.8287	157.5258	2	PROCESSED	57601.0256134259	2016-08-01 00:36:53	55990	2012-03-04 00:00:00	55621.2978703704	2011-03-01 07:08:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050033	We propose a Suzaku observation of the pre-main sequence binary system V773 Tau with the high sensitivity of HXD. The empirical Lx-Lr relation (Benz-G"udel relation) and radio flux variation predict that this source can have a flare with a peak luminosity Lx=10^34 ergs s-1, seven orders of magnitude larger than that of the Sun, when it is just before the periastron passage. We will observe this target simultaneously with radio band using VLBI network. Our goal is (1) to test whether the gigantic flare is still on the empirical relation (2) to detect inpulsive non-thermal emission at the most powerful stellar flare (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band.	GALACTIC POINT SOURCES	4	B	YOHKO TSUBOI		JAP	5	AO5	NON-THERMAL EMISSION AT THE MOST POWERFUL STELLAR FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405011010/	Quick Look
105	1E 1547.0-5408	237.7284	-54.3676	236.761869	-54.21692	248.127922	-33.347549	327.20000551	-0.18012949	271.1663	55415.1611921296	2010-08-07 03:52:07	55415.9633796296	2010-08-07 23:07:16	405024010	51.6728	50	51.6728	51.7928	0	52.1529	2	2	0	1	1	0	0	42.7812	42.7812	69.2999	0	PROCESSED	57552.8870949074	2016-06-13 21:17:25	55793	2011-08-20 00:00:00	55427.247025463	2010-08-19 05:55:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050099	Recently, hard X-ray tails have been detected by INTEGRAL at least up to 150 keV from ~5 magnetars. Suzaku has observed some magnetars during Key Project (AO-4) and ToO observations. As a result, soft X-ray emissions and hard X-ray tails have been detected from ~10 magnetars. This peculiar spectrum is seem to be common in all the magnetars, and we discovered the spectral evolution of magnetars. The remaining problem is to study the spectral difference between the active and quiescent states. Transient magnetar 1E 1547.0-540 was observed with Suzaku in 2009 January, and the extremely hard X-ray tail was detected up to 110 keV with photon index of 1.5, and it is appropriate to study the spectral change. Thus, we propose the observation of 1E 1547.0-5408 with 50 ks.	GALACTIC POINT SOURCES	4	B	HIROYUKI NISHIOKA		JAP	5	AO5	OBSERVATION OF THE HARD X-RAY TAIL AND SOFT X-RAY EMISSION OF AXP 1E 1547.0-5408 IN QUIESCENT STATE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405024010/	Quick Look
106	EMS1150	263.083	-32.7212	262.264926	-32.685689	264.095488	-9.421504	355.27740066	0.39306698	91.2452	55611.9964930556	2011-02-19 23:54:57	55612.6968055556	2011-02-20 16:43:24	405026010	20.9186	20	20.9186	20.9186	0	20.9186	1	1	0	1	1	0	0	17.2639	17.2639	60.5039	0	PROCESSED	57600.9777893518	2016-07-31 23:28:01	55988	2012-03-02 00:00:00	55621.1440740741	2011-03-01 03:27:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050104	Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV.	GALACTIC POINT SOURCES	4	A	YASUYUKI TANAKA		JAP	5	AO5	SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405026010/	Quick Look
107	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
108	4U1812-12	273.8053	-12.0935	273.104949	-12.110284	273.784611	11.297146	18.04900466	2.37362039	267.159	55838.1400347222	2011-10-04 03:21:39	55839.9168981482	2011-10-05 22:00:20	406008010	62.0143	60	62.0143	62.0143	0	62.0143	2	2	0	2	1	0	0	53.5441	53.5441	153.5099	1	PROCESSED	57603.3255902778	2016-08-03 07:48:51	56226	2012-10-26 00:00:00	55858.3124768518	2011-10-24 07:29:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060012	Low-Mass X-ray binaries (LMXBs) are known to have soft and hard states, like black hole binaries. Through an analysis of archival Suzaku data of the LMXB Aql X-1 in the hard state, we obtained a clear picture of its accretion geometry; a truncated accretion disk, and a hot corona that Comptonize blackbody photons from the neutron star surface. In order to investigate whether this picture also applies to other LMXBs in the low/hard state, and to better constrain the accretion geometry in comparison with those of black hole binaries, we propose a 60 ksec Suzaku observation of the LMXB 4U 1812-12. This is a valuable object,which is known to reside almost always in the low/hard state.	GALACTIC POINT SOURCES	4	A	SOKI SAKURAI		JAP	6	AO6	REVEALING THE ACCRETION GEOMETRY OF THE LOW/HARD STATE LMXB 4U 1812-12 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406008010/	Quick Look
109	VW HYI	62.3084	-71.2978	62.399199	-71.427045	322.000013	-79.107776	284.88912946	-38.12913625	338.7313	56049.8124305556	2012-05-02 19:29:54	56050.1668171296	2012-05-03 04:00:13	406009040	16.8177	20	16.8257	16.8257	0	16.8177	2	1	0	2	1	0	0	13.9478	13.9478	30.6159	0	PROCESSED	57605.3312847222	2016-08-05 07:57:03	56449	2013-06-06 00:00:00	56083.0857060185	2012-06-05 02:03:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060023	SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate.	GALACTIC POINT SOURCES	4	B	KEI SAITOU		JAP	6	AO6-TOO	TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009040/	Quick Look
110	CYG X-1	299.5916	35.1745	299.121401	35.038023	313.64901	54.223609	71.31236822	3.05181611	279.5001	55839.9245023148	2011-10-05 22:11:17	55840.9169328704	2011-10-06 22:00:23	406013010	3.7027	40	3.832	3.7027	0	40.2718	1	1	0	1	1	0	0	32.9625	32.9625	85.7339	1	PROCESSED	57603.3954166667	2016-08-03 09:29:24	56582	2013-10-17 00:00:00	56212.7247916667	2012-10-12 17:23:42	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060057	We achieved 0.1 s time resolution with enough statistics on accumulating profiles of source brightening and made clear that electron temperature decreases and optical depth increases at the peak of brightness by using the XIS data of Psum mode. Progress to understanding the nature of fast time variability, which has been a mystery for 40 years since its discovery, connected with spectral properties is being made now. However, this property is not confirmed yet in other observations having different time scales of variability and spectral shapes, lacking the XIS data in Psum mode. We propose here another observation of Cyg X-1 with XIS0 1/8 window no burst, XIS1 1/4 window 0.5 s burst,and XIS3 Psum mode for a exposure of 40 ks.	GALACTIC POINT SOURCES	4	A	SHIN'YA YAMADA		JAP	6	AO6	REVEALING THE NATURE OF FAST TIME VARIABILITY OF CYG X-1 WITH SHOT ANALYSIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406013010/	Quick Look
111	AXP 4U 0142+614	26.5682	61.7591	25.700455	61.509234	52.151654	46.394786	129.37061357	-0.42523158	40.384	55811.6552314815	2011-09-07 15:43:32	55812.5731134259	2011-09-08 13:45:17	406031010	38.6497	60	38.6497	38.6497	0	38.6825	2	2	0	2	1	0	0	42.1964	42.1964	79.292	0	PROCESSED	57603.1220138889	2016-08-03 02:55:42	56218	2012-10-18 00:00:00	55851.4406828704	2011-10-17 10:34:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060092	We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI.	GALACTIC POINT SOURCES	4	A	YUJIN NAKAGAWA		JAP	6	AO6-TOO	A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406031010/	Quick Look
112	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
113	H1743-322	266.5672	-32.235	265.751321	-32.216345	267.052375	-8.828926	357.25482673	-1.83530791	277.9713	56212.4049884259	2012-10-12 09:43:11	56213.3744560185	2012-10-13 08:59:13	407005030	21.361	40	21.3706	21.3722	0	21.361	3	3	0	3	1	0	0	40.615	40.615	83.736	1	PROCESSED	57607.7385416667	2016-08-07 17:43:30	56598	2013-11-02 00:00:00	56232.473275463	2012-11-01 11:21:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070002	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	7	AO7-TOO	MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407005030/	Quick Look
114	CYG X-1	299.5875	35.2031	299.117489	35.06664	313.660052	54.251673	71.33506579	3.06957776	88.7802	56390.0953472222	2013-04-08 02:17:18	56391.9585532407	2013-04-09 23:00:19	407015010	4.1499	85	8.503	4.1499	0	66.4751	2	1	0	1	1	0	0	71.7128	71.7128	160.9658	3	PROCESSED	57611.2046875	2016-08-11 04:54:45	56808	2014-05-31 00:00:00	56402.1391087963	2013-04-20 03:20:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070030	We propose to observe Cyg X-1 for 85 ks, utilizing P-sum mode for XIS3. Our aim is to perform shot analysis, which is originally invented by Negoro et al. 1995 with Ginga, and obtain high-quality wide-band spectra for several phases in less than 1 sec; for example, 0.1 sec before the peak, +/- 0.05 sec at the peak, and after the peak. With these spectra, we will quantify changes in five spectral components: hard Comptonization, soft Comptonization, disk emission, Fe-K lines, and reflection. This will be a clue to know long-standing mystery on rapid variability in black holes.	GALACTIC POINT SOURCES	4	A	SHINYA YAMADA		JAP	7	AO7	INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407015010/	Quick Look
115	Z CAM	126.3	73.123	124.909699	73.28505	106.108743	51.709102	141.36861973	32.62424745	91.2043	56239.0368981482	2012-11-08 00:53:08	56239.7800347222	2012-11-08 18:43:15	407016010	35.852	35	35.852	35.852	0	35.852	2	2	0	2	1	0	0	33.8968	33.8968	64.1939	1	PROCESSED	57607.9797337963	2016-08-07 23:30:49	56631	2013-12-05 00:00:00	56264.602349537	2012-12-03 14:27:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070038	Dwarf novae are a subclass of cataclysmic variables, which sometimes show outbursts. In the outbursts, they are considered to emanate disk winds, but observational evidence had been lacking. Recently, our Suzaku observation of Z Cam during a very transition from quiescence to an outburst revealed clear evidence of the disk wind for the first time, and we were able to study characteristics of the disk wind in detail. Z Cam in quiescence, however, has never been observed with high quality instruments. We, therefore, propose an observation of Z Cam in quiescence in order to study entire behavior of the disk wind throughout different phases, combining the existent Suzaku transition phase data and ASCA archival data taken in other phases.	GALACTIC POINT SOURCES	4	C	KEI SAITOU		JAP	7	AO7	COMPREHENSIVE STUDY FOR THE DISK WIND OF THE DWARF NOVA Z CAM THROUGH OUTBURST CYCLES WITH AN OBSERVATION IN QUIESCENCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407016010/	Quick Look
116	AX J1445.7-5931	221.4519	-59.5275	220.50216	-59.317243	239.705831	-41.083897	316.97780419	0.18867801	281.526	56143.2829513889	2012-08-04 06:47:27	56144.2918865741	2012-08-05 07:00:19	407021010	40.0525	40	41.0682	41.0602	0	40.0525	2	1	0	2	1	0	0	36.8089	36.8089	87.1579	1	PROCESSED	57606.7459722222	2016-08-06 17:54:12	56533	2013-08-29 00:00:00	56167.2116319444	2012-08-28 05:04:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070043	Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution.	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	7	AO7	ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407021010/	Quick Look
117	IGR J17091-3624	257.2866	-36.4073	256.446112	-36.344023	259.498562	-13.427876	349.52701092	2.20940495	283.8915	56202.8636689815	2012-10-02 20:43:41	56203.7202662037	2012-10-03 17:17:11	407037010	42.0759	120	42.0759	42.0837	0	42.0797	3	3	0	3	1	0	0	40.392	40.392	74.0079	0	PROCESSED	57607.2660069444	2016-08-07 06:23:03	56728	2014-03-12 00:00:00	56226.6701388889	2012-10-26 16:05:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070097	We propose a Suzaku observation of "the second GRS 1915+105" IGR J17091-3624 with a high energy resolution and broadband capability. GRS 1915+105 has been considered to be the unique black hole binary that stays at a high mass accretion rate and shows limit-cycle oscillations, but it was recently discovered that the BHC IGR J17091-3624 has exactly the same X-ray variability patterns as GRS 1915+105. This fact suggests an evidence for common physical mechanism in both system. The Suzaku observation will reveal both similarity and difference with GRS 1915+105 from a point of view of broad-band spectral properties and disk wind, and help us understanding of the accretion flow onto a black hole under a high mass accretion rate.	GALACTIC POINT SOURCES	4	B	KAZUTAKA YAMAOKA		JAP	7	AO7	SUZAKU BROADBAND OBSERVATION OF "THE SECOND GRS 1915+105" IGR J17091-3624	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407037010/	Quick Look
118	PG 1658 +440	254.9348	44.0094	254.55381	44.082621	242.595421	66.02047	69.11167171	38.06633743	330.9998	56115.6740972222	2012-07-07 16:10:42	56116.8301041667	2012-07-08 19:55:21	407040010	51.0329	50	51.0329	51.0329	0	51.0329	1	1	0	1	1	0	0	46.6746	46.6746	99.8718	1	PROCESSED	57606.5897222222	2016-08-06 14:09:12	56508	2013-08-04 00:00:00	56142.1447337963	2012-08-03 03:28:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070112	The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects.	GALACTIC POINT SOURCES	4	B	ATSUSHI HARAYAMA		JAP	7	AO7	SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407040010/	Quick Look
119	GC20	265.6604	-28.73	264.867608	-28.707008	266.169302	-5.346539	359.83402449	0.66365416	262.9349	54385.4117939815	2007-10-12 09:52:59	54385.9099421296	2007-10-12 21:50:19	502008010	23.7786	20	23.7906	23.7866	0	23.7786	2	2	0	2	1	0	0	22.9234	22.9234	43.032	0	PROCESSED	57540.2572337963	2016-06-01 06:10:25	54771	2008-11-01 00:00:00	54403.0227314815	2007-10-30 00:32:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502008010/	Quick Look
120	4U 0142+61	26.5838	61.7628	25.715895	61.512967	52.16359	46.394147	129.37704782	-0.4200572	82.997	56504.4205902778	2013-07-31 10:05:39	56506.6252430556	2013-08-02 15:00:21	408011010	101.1678	100	101.1678	101.1828	0	101.1828	2	2	0	2	1	0	0	102.4739	102.4739	190.4637	1	PROCESSED	57612.1558680556	2016-08-12 03:44:27	56953	2014-10-23 00:00:00	56587.5059606482	2013-10-22 12:08:35	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080035	A toroidal magnetic field is thought to be formed in neutron star interior after core-collapse supernovae and become an energy source with recently observed X-ray outbursts from magnetars. Since the toroidal field is hidden in the stellar interior, it was thought to be undetectable via the well-known p-pdot method and the cyclotron resonance scattering features. However, a magnetic stress of the magnetar toroidal field is strong enough to distort the stellar shape and produce a free precession in its X-ray pulse timing if the emission pattern deviates from its axis of symmetry. From our analyses of magnetar 4U 0142+61, we found an evidence on the free precession in the hard X-ray component. To confirm and establish this evidence, we propose an additional 100 ks observation of 4U 0142+61.	GALACTIC POINT SOURCES	4	A	TERUAKI ENOTO		JAP	8	AO8	TOROIDAL FIELD INSIDE MAGNETARS OBSERVED WITH SUZAKU TIMING ANALYSES OF ITS FREE PRECESSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408011010/	Quick Look
121	SGR 0501+4516	75.2774	45.2864	74.365802	45.213531	78.849797	22.414701	161.53821228	1.95483036	87.7054	56535.9761574074	2013-08-31 23:25:40	56536.8752662037	2013-09-01 21:00:23	408013010	36.1244	40	36.1244	41.2611	0	41.2452	2	2	0	1	1	0	0	35.7177	35.7177	77.6719	1	PROCESSED	57612.459375	2016-08-12 11:01:30	56974	2014-11-13 00:00:00	56608.6586342593	2013-11-12 15:48:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080040	Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources.	GALACTIC POINT SOURCES	4	B	TERUAKI ENOTO		JAP	8	AO8	ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408013010/	Quick Look
122	SAGITTARIUS A*	266.4146	-29.0065	265.619896	-28.987158	266.840205	-5.604694	359.94434823	-0.0438121	107.0001	56728.6474537037	2014-03-12 15:32:20	56729.1147569445	2014-03-13 02:45:15	408017060	21.1387	20	21.1427	21.1387	0	21.1595	2	2	0	3	1	0	0	20.4844	20.4844	40.368	0	PROCESSED	57614.0078240741	2016-08-14 00:11:16	57113	2015-04-01 00:00:00	56747.6540972222	2014-03-31 15:41:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017060/	Quick Look
123	X 1630-472	248.5012	-47.3939	247.580186	-47.289758	254.085797	-25.132076	336.90807869	0.25236055	88.6321	57077.0625578704	2015-02-24 01:30:05	57078.1140277778	2015-02-25 02:44:12	409007020	5.5296	40	5.547	5.5659	0	5.5296	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6879282407	2016-08-17 16:30:37	57454	2016-03-07 00:00:00	57087.4605208333	2015-03-06 11:03:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090015	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	9	AO9-TOO	MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409007020/	Quick Look
124	ASO0376	263.1417	-31.5448	262.331507	-31.509592	264.088273	-8.244108	356.29011362	0.99386623	267.5095	55082.1506365741	2009-09-08 03:36:55	55083.1084606482	2009-09-09 02:36:11	504049010	37.2278	20	38.9878	39.2598	0	37.2278	5	4	0	4	1	0	0	31.8134	31.8134	82.7299	1	PROCESSED	57548.4976041667	2016-06-09 11:56:33	55479	2010-10-10 00:00:00	55113.2260069444	2009-10-09 05:25:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.	GALACTIC DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504049010/	Quick Look
125	H1743-322	266.2607	-32.2285	265.444935	-32.208359	266.789922	-8.828952	357.12541364	-1.6105206	285.4288	56932.6365625	2014-10-02 15:16:39	56933.284837963	2014-10-03 06:50:10	409008010	15.0094	40	15.6012	15.6169	0	15.0094	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6096527778	2016-08-16 14:37:54	57345	2015-11-19 00:00:00	56979.4022569444	2014-11-18 09:39:15	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090015	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	9	AO9-TOO	MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409008010/	Quick Look
126	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
127	H1743-322	266.5672	-32.2343	265.751326	-32.215645	267.052358	-8.828226	357.25542532	-1.83494451	273.3773	56939.7339236111	2014-10-09 17:36:51	56940.5245138889	2014-10-10 12:35:18	409008020	19.0006	40	19.0006	19.0145	0	19.0115	3	3	0	3	0	0	0	0	0	0	0	PROCESSED	57616.6317824074	2016-08-16 15:09:46	57345	2015-11-19 00:00:00	56979.407974537	2014-11-18 09:47:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090015	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	9	AO9-TOO	MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409008020/	Quick Look
128	SAGITTARIUS A*	266.4193	-29.0102	265.624572	-28.990881	266.844426	-5.60829	359.94333122	-0.04924818	267.3027	56929.1441550926	2014-09-29 03:27:35	56929.6668402778	2014-09-29 16:00:15	409011010	20.2183	20	20.2183	20.3303	0	20.3543	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5861226852	2016-08-16 14:04:01	56748	2014-04-01 00:00:00	56979.4039814815	2014-11-18 09:41:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090048	With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	9	AO9	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011010/	Quick Look
129	SAGITTARIUS A*	266.4217	-29.0078	265.626986	-28.988492	266.846474	-5.605838	359.94647323	-0.04978962	278.8011	56938.0879861111	2014-10-08 02:06:42	56938.4619097222	2014-10-08 11:05:09	409011020	17.2605	20	17.2605	17.2605	0	17.2605	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6209606482	2016-08-16 14:54:11	56748	2014-04-01 00:00:00	56979.4091087963	2014-11-18 09:49:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090048	With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	9	AO9	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011020/	Quick Look
130	1RXSJ182853.8-241746	277.2212	-24.2932	276.455559	-24.326354	276.570172	-1.017121	8.76671438	-6.19414371	87.3419	57120.5005092593	2015-04-08 12:00:44	57120.8217476852	2015-04-08 19:43:19	409013010	9.7072	12	9.7072	11.8422	0	11.8502	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.9447453704	2016-08-17 22:40:26	57496	2016-04-18 00:00:00	57129.4074189815	2015-04-17 09:46:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090051	We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	B	HIDEYUKI MORI		JAP	9	AO9	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409013010/	Quick Look
131	GK PER	52.8052	43.8974	51.953057	43.727495	61.505862	24.068527	150.96310366	-10.10758836	250.0842	57086.777037037	2015-03-05 18:38:56	57090.7709606482	2015-03-09 18:30:11	409018020	182.886	140	0	0	0	182.886	0	0	0	2	1	0	0	134.9166	134.9166	344.9376	0	PROCESSED	57617.786712963	2016-08-17 18:52:52	57468	2016-03-21 00:00:00	57101.0913657407	2015-03-20 02:11:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090055	A 140-ks observation of the magnetic cataclysmic variable GK Per is proposed. By fitting Suzaku broadband spectra using our multitemperature spectral model of the accretion column, we estimate a white dwarf mass with statistical fitting errors smaller than 5%. The estimated mass will be compared with one obtained from the optical lightcurve fitting method developed and applied by Hachisu and Kato in a series of papers. GK Per is the only known magnetic cataclysmic variable which underwent classical nova explosion (in 1901), and both the mass estimation methods can be applied. Cross-validated WD mass estimation methods will be of importance in studying massive white dwarfs in accretion systems, in relation with the progenitor of type Ia supernovae.	GALACTIC POINT SOURCES	4	A	TAKAYUKI YUASA		JAP	9	AO9	CROSS VALIDATION OF WHITE DWARF MASS ESTIMATION METHODS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409018020/	Quick Look
132	Crab nebula	83.6222	22.1365	82.869251	22.10376	84.094492	-1.173718	184.44846107	-5.72755512	86.8666	53608.2089236111	2005-08-26 05:00:51	53608.316087963	2005-08-26 07:35:10	100010080	3.382	5	3.382	3.382	3.382	3.382	1	1	1	1	1	0	0	3.7003	3.7003	9.2539	0	PROCESSED	57526.9140856482	2016-05-18 21:56:17	54247	2007-05-27 00:00:00	54119.0056134259	2007-01-19 00:08:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010080/	Quick Look
133	VELA JR P26	132.8787	-46.6693	132.45444	-46.480585	159.781455	-60.154541	266.46476457	-1.49839932	347.0019	54653.4341203704	2008-07-06 10:25:08	54653.837025463	2008-07-06 20:05:19	503038010	14.553	10	14.553	14.553	0	14.553	1	1	0	1	1	0	0	10.9536	10.9536	34.7839	0	PROCESSED	57542.9869675926	2016-06-03 23:41:14	55048	2009-08-05 00:00:00	54679.3709606482	2008-08-01 08:54:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503038010/	Quick Look
134	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
135	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
136	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
137	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
138	CYGNUS_LOOP_P8	313.9965	31.4722	313.478406	31.279742	329.042886	46.311836	75.29540263	-8.88432445	62.5181	53868.0059837963	2006-05-13 00:08:37	53868.1717476852	2006-05-13 04:07:19	501028010	4.8706	6	4.8706	4.8706	4.8706	4.8706	2	2	2	2	1	0	0	2.328	2.328	14.316	0	PROCESSED	57534.2851736111	2016-05-26 06:50:39	54394	2007-10-21 00:00:00	53914.3326157407	2006-06-28 07:58:58	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501028010/	Quick Look
139	M82 X-1	149.1432	69.7042	148.108278	69.941832	119.044016	52.159559	141.33659361	40.60182861	163.0524	54367.135775463	2007-09-24 03:15:31	54367.8716898148	2007-09-24 20:55:14	702026010	35.5999	40	36.0319	35.5999	0	36.0239	2	2	0	2	1	0	0	30.4749	30.4749	63.5699	1	PROCESSED	57540.0638194444	2016-06-01 01:31:54	54770	2008-10-31 00:00:00	54402.2563657407	2007-10-29 06:09:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020092	We propose Suzaku observations of the intermediate-mass black hole candidate M82 X-1 for spectral study with a wide-band energy range including over 10 keV. In particular, the purpose is to determine a spectral cut-off energy in details in order to improve unified understanding of different mass black holes in comparison with those of stellar-mass black holes and ULXs in nearby galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	C	RYOHEI MIYAWAKI		JAP	2	AO2	HARD X-RAY SPECTRAL STUDY OF M82 X-1 WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702026010/	Quick Look
140	1H0323+342	51.1746	34.1741	50.388045	33.998103	57.519907	15.008853	155.73224486	-18.75935356	251.4848	56352.6173611111	2013-03-01 14:49:00	56354.8078819444	2013-03-03 19:23:21	707015010	101.272	100	101.288	101.272	0	101.288	2	2	0	2	1	0	0	97.1283	97.1283	189.2516	0	PROCESSED	57610.7547916667	2016-08-10 18:06:54	56739	2014-03-23 00:00:00	56372.5724189815	2013-03-21 13:44:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070088	We propose to observe a narrow-line radio-loud gamma-ray emitting Seyfert 1 galaxy 1H0323+342, which is the X-ray brightest among a new class of GeV gamma-ray emitting AGNs, first detected by Fermi/LAT. Based on accurate and high-sensitive measurement of X-ray spectra with Suzaku, we study the presence of Fe-K lines and energy-dependence of time variability, in order to constrain the origin of X-ray emission of this object. This leads to understanding the SED of this object and constraining the jet power.	EXTRAGALACTIC COMPACT SOURCES	7	C	YASUSHI FUKAZAWA		JAP	7	AO7	STUDY OF X-RAY SPECTRAL VARIABILITY OF A NARROW-LINE RADIO-LOUD GAMAM-RAY EMITTING SEYFERT 1 GALAXY 1H0323+342	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707015010/	Quick Look
141	PSR J1957+5036	299.4354	50.5474	299.08901	50.41133	327.273287	68.217535	84.58480161	10.99652902	216.5649	55543.4586689815	2010-12-13 11:00:29	55544.0842939815	2010-12-14 02:01:23	405016010	32.469	30	32.485	32.469	0	32.485	2	2	0	2	1	0	0	25.3139	25.3139	54.0339	2	PROCESSED	57554.3965393518	2016-06-15 09:31:01	55959	2012-02-02 00:00:00	55592.9341782407	2011-01-31 22:25:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050047	Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.	GALACTIC POINT SOURCES	4	C	NOBUYUKI KAWAI		JAP	5	AO5	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405016010/	Quick Look
142	VELA PWN N4	128.8415	-44.0453	128.410682	-43.871484	152.26227	-59.375821	262.64764922	-2.10667439	326.4998	56110.0169097222	2012-07-02 00:24:21	56110.3459953704	2012-07-02 08:18:14	507051010	17.289	15	17.289	17.289	0	17.289	2	2	0	2	1	0	0	17.6558	17.6558	28.4019	0	PROCESSED	57606.5331018518	2016-08-06 12:47:40	56646	2013-12-20 00:00:00	56280.6029050926	2012-12-19 14:28:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070103	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	7	AO7	HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507051010/	Quick Look
143	VELA PWN W1	128.3503	-45.1912	127.929525	-45.019236	152.791152	-60.544208	263.35940671	-3.07091685	303.5014	56438.6169444444	2013-05-26 14:48:24	56439.0342476852	2013-05-27 00:49:19	508042010	14.1172	15	14.1172	14.1252	0	14.1252	1	1	0	1	1	0	0	13.2844	13.2844	36.0239	0	PROCESSED	57611.3765046296	2016-08-11 09:02:10	56864	2014-07-26 00:00:00	56498.6138888889	2013-07-25 14:44:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080090	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered.	GALACTIC DIFFUSE EMISSION	5	B	KOJI MORI		JAP	8	AO8	SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508042010/	Quick Look
144	G359.0-0.9 NW	266.56	-30.3287	265.756777	-30.310042	266.999862	-6.92337	358.88098313	-0.83974756	102	56723.5510648148	2014-03-07 13:13:32	56724.8162268518	2014-03-08 19:35:22	508058010	52.0885	50	52.0885	52.0965	0	52.1045	2	2	0	2	1	0	0	45.5738	45.5738	109.2758	2	PROCESSED	57613.9935416667	2016-08-13 23:50:42	57100	2015-03-19 00:00:00	56734.6649189815	2014-03-18 15:57:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080113	We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	8	AO8	FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508058010/	Quick Look
145	SS433_JET_KNOT	288.5694	4.9037	287.951117	4.816458	290.852472	27.010013	39.90628699	-2.82264549	256.6998	56597.9130555556	2013-11-01 21:54:48	56600.2502314815	2013-11-04 06:00:20	508024010	106.8942	100	106.8942	106.8942	0	106.8942	2	2	0	2	1	0	0	102.4583	102.4583	201.8897	3	PROCESSED	57613.2427777778	2016-08-13 05:49:36	56980	2014-11-19 00:00:00	56611.6875578704	2013-11-15 16:30:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080065	We propose an observation of the jet of SS 433. Our purpose is to detect high-temperature diffuse plasma component made by the black hole jet.	GALACTIC DIFFUSE EMISSION	5	C	HIDEKI UCHIYAMA		JAP	8	AO8	SEARCHING DIFFUSE HOT-PLASMA COMPONENT MADE BY A BLACK HOLE JET OF SS 433	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508024010/	Quick Look
146	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
147	GC_SGR_B_EAST	267.0203	-28.3518	266.229607	-28.335406	267.358668	-4.938031	0.77973231	-0.1584432	71.8708	54162.5141203704	2007-03-03 12:20:20	54164.5273726852	2007-03-05 12:39:25	501039010	96.4018	100	96.4018	96.4018	0	96.4018	2	2	0	2	1	0	0	91.0829	91.0829	173.9318	3	PROCESSED	57537.6522800926	2016-05-29 15:39:17	54736	2008-09-27 00:00:00	54171.4429050926	2007-03-12 10:37:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010060	We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	1	AO1	OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501039010/	Quick Look
148	CXO J172641.7-354052	261.6769	-35.6761	260.838718	-35.633773	263.074511	-12.434469	352.17176486	-0.26901827	279.4529	56540.003275463	2013-09-05 00:04:43	56540.8015509259	2013-09-05 19:14:14	408021010	37.3165	40	37.3317	37.3349	0	37.3165	2	3	0	2	1	0	0	35.3693	35.3693	68.9659	0	PROCESSED	57612.5112037037	2016-08-12 12:16:08	56956	2014-10-26 00:00:00	56587.7063541667	2013-10-22 16:57:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080100	We propose an additional Suzaku observation of an unclassified gamma-ray source detected with the Fermi LAT telescope. In previous cycles, we found an enigmatic source XSS J12270-4859 to be the first gamma-ray binary among the low-mass X-ray binaries. This proposal aims to find a second source of the same nature for the most prospective target extracted from our catalogue search.	GALACTIC POINT SOURCES	4	C	MASAHIRO TSUJIMOTO		JAP	8	AO8	X-RAY SEARCH OF ANOTHER ENIGMATIC SOURCE IN OUR GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408021010/	Quick Look
149	CYGNUS X-3	308.2593	40.981	307.808438	40.809488	328.80084	56.880196	79.93230299	0.62160244	252.424	54052.0902893518	2006-11-13 02:10:01	54054.3676388889	2006-11-15 08:49:24	401011010	99.7445	100	99.7462	99.7462	0	99.7445	2	2	0	2	1	0	0	95.3893	95.3893	196.745	1	PROCESSED	57536.1520717593	2016-05-28 03:38:59	54456	2007-12-22 00:00:00	54088.9545023148	2006-12-19 22:54:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010058	We propose an observation of the unusual X-ray binary Cygnus X-3. Cyg X-3 is a final stage of the massive binary stars consisting of a WR(N) star and a compact star. However the nature of the compact star is not well understood. We have fore scientific objective. (A)Determine the Doppler modulation of iron K lines and discuss the binary nature. (2) Determine the iron abundance in the WR wind. (3) Search for the high energy cut off about 100keV of the power law component. (4) Search for the X-ray emission from radio knots. For these four sciences, we propose 100ksec observation of Cyg X-3.	GALACTIC POINT SOURCES	4	C	SHUNJI KITAMOTO		JAP	1	AO1	WIDE BAND OBSERVATION OF CYGNUS X-3 WITH SUZAKU	SPE	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401011010/	Quick Look
150	1RXS J070407.9+26250	106.0341	26.4126	105.260164	26.487679	104.355942	3.767203	190.27497025	14.29877104	282.0717	54548.4868865741	2008-03-23 11:41:07	54549.9862384259	2008-03-24 23:40:11	402008010	58.3157	50	58.3237	58.3157	0	58.3237	1	1	0	1	1	0	0	49.4766	49.4766	129.5278	0	PROCESSED	57541.9808912037	2016-06-02 23:32:29	54933	2009-04-12 00:00:00	54566.326712963	2008-04-10 07:50:28	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020029	Soft Intermediate Polar (IP) is a small group of IPs whose X-ray spectrum is extremely soft compared with general IPs. Recent observations reveal that some soft IPs harbor a soft blackbody component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand possible evolutionary link from IPs to polars, the origin of the soft excess in polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure their temperature and flux systematically.	GALACTIC POINT SOURCES	4	C	MANABU ISHIDA		JAP	2	AO2	OBSERVATIONS OF SOFT INTERMEDIATE POLARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402008010/	Quick Look
151	U SCO	245.6288	-17.8156	244.907071	-17.699112	246.808077	3.684973	357.72079613	21.90901194	93.2747	55233.0102430556	2010-02-06 00:14:45	55234.2918865741	2010-02-07 07:00:19	404018010	46.0764	20	46.0764	46.0764	0	46.0764	2	2	0	2	1	0	0	37.6117	37.6117	110.7199	1	PROCESSED	57550.518599537	2016-06-11 12:26:47	55617	2011-02-25 00:00:00	55250.1559375	2010-02-23 03:44:33	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040057	We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each.	GALACTIC POINT SOURCES	4	A	DAI TAKEI		JAP	4	AO4-TOO	TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404018010/	Quick Look
152	HESSJ1741-A	265.3548	-30.1316	264.55314	-30.107106	265.945938	-6.755753	358.50289854	0.15030933	73.8229	54886.7117013889	2009-02-24 17:04:51	54888.0419328704	2009-02-26 01:00:23	503076010	52.9323	50	52.9323	52.9323	0	52.9323	2	2	0	2	1	0	0	43.7708	43.7708	114.9158	1	PROCESSED	57545.6752546296	2016-06-06 16:12:22	55330	2010-05-14 00:00:00	54902.4869791667	2009-03-12 11:41:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030113	HESSJ1741-302 is one of the most darkest TeV unidentified objects which was discovered with the H.E.S.S. telescope recently. The location strongly suggests that the object is physically connected to the diffuse TeV gamma-ray emission along the Galactic plane. On the other hand, there is a pulsar near the object, and it may be an off-set pulsar wind nebula. To clarify the origin of the object, we propose to the observation of HESSJ1741.	GALACTIC DIFFUSE EMISSION	5	C	HIRONORI MATSUMOTO		JAP	3	AO3	DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503076010/	Quick Look
153	II PEG	358.7744	28.6284	358.137778	28.350132	11.171995	26.557383	108.23861581	-32.63076231	231.1411	56301.1877314815	2013-01-09 04:30:20	56303.6487962963	2013-01-11 15:34:16	407038010	17.0176	100	111.5065	111.5145	0	17.0176	3	3	0	3	1	0	0	107.9058	107.9058	212.6198	2	PROCESSED	57608.5074305556	2016-08-08 12:10:42	56724	2014-03-08 00:00:00	56363.602037037	2013-03-12 14:26:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070102	We propose a Suzaku observation of the powerful flare star II Peg with the high sensitivity of HXD. MAXI/GSC results from 2009 to 2011 show that this source exhibits the highest flaring activity with the largest luminosities and the largest fluxes. Then detection of the non-thermal emission is the most expected from this source at the on-set of a flare. We are to observe this target simultaneously with radio, infrared, optical, and X-ray bands for the first time. Our goal is (1) to detect impulsive non-thermal emission at the powerful II Peg flare (2) to obtain wide-band SED variability from radio to hard X-ray band, and (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band.	GALACTIC POINT SOURCES	4	C	YOHKO TSUBOI		JAP	7	AO7	NON-THERMAL EMISSION ON THE POWERFUL STELLAR FLARE FROM II PEG	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407038010/	Quick Look
154	SWIFT J1922.7-1716	290.6403	-17.2233	289.918336	-17.319807	289.738469	4.813727	20.73500926	-14.48356253	80.064	54198.231099537	2007-04-08 05:32:47	54200.4321643518	2007-04-10 10:22:19	702028010	78.6386	80	78.6386	78.6386	0	78.6386	2	2	0	2	1	0	0	61.3533	61.3533	190.1298	0	PROCESSED	57538.1728356482	2016-05-30 04:08:53	54744	2008-10-05 00:00:00	54206.3754166667	2007-04-16 09:00:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020097	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	2	AO2	BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702028010/	Quick Look
155	2MASX J15115979-2119	227.9997	-21.3083	227.279118	-21.120692	231.351076	-3.323732	341.57056512	30.81939061	105.6253	55979.0551388889	2012-02-22 01:19:24	55980.937650463	2012-02-23 22:30:13	706010010	83.8162	80	83.8162	83.8162	0	83.8162	2	2	0	2	1	0	0	82.2568	82.2568	162.6359	1	PROCESSED	57604.7185763889	2016-08-04 17:14:45	56361	2013-03-10 00:00:00	55995.1640393518	2012-03-09 03:56:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060032	We propose to observe two hard X-ray bright narrow-line Seyfert 1 galaxies, which are an important class of objects in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be a fundamental piece of information to better understand accretion physics and ``feedback'' processes in galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	6	AO6	ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED NARROW-LINE SEYFERT 1S	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706010010/	Quick Look
156	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
157	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
158	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
159	DRACO HVC REGION B	243.9603	59.1738	243.739297	59.296448	199.753416	76.165002	90.07720195	42.68363475	80.282	53816.0059953704	2006-03-22 00:08:38	53817.4148611111	2006-03-23 09:57:24	501005010	61.632	60	61.6447	61.644	61.632	61.636	2	2	2	2	1	0	0	60.6865	60.6865	121.7099	2	PROCESSED	57533.3166319444	2016-05-25 07:35:57	54400	2007-10-27 00:00:00	53906.4964583333	2006-06-20 11:54:54	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010069	High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	1	AO1	SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE -	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501005010/	Quick Look
160	CYGNUS_LOOP_P9	311.8173	30.594	311.299257	30.409327	326.059392	46.235255	73.41991066	-7.98099126	239.9998	54416.7228935185	2007-11-12 17:20:58	54417.2502199074	2007-11-13 06:00:19	501019010	19.5656	15	19.5656	19.5656	0	19.5656	2	2	0	2	1	0	0	17.3446	17.3446	45.5379	0	PROCESSED	57540.4965393518	2016-06-01 11:55:01	54798	2008-11-28 00:00:00	54430.2327546296	2007-11-26 05:35:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501019010/	Quick Look
161	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
162	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
163	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
164	1RXSJ173905.2-392615	264.7748	-39.4365	263.906258	-39.409033	265.79264	-16.071333	350.35081336	-4.37467046	271.2006	56188.8237384259	2012-09-18 19:46:11	56189.3446990741	2012-09-19 08:16:22	407029010	22.0638	15	22.0718	22.0638	0	22.0718	1	1	0	1	1	0	0	18.2515	18.2515	44.9999	0	PROCESSED	57607.0891898148	2016-08-07 02:08:26	56584	2013-10-19 00:00:00	56218.4994212963	2012-10-18 11:59:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070052	We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	C	HIDEYUKI MORI		JAP	7	AO7	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407029010/	Quick Look
165	U GEM IN QUIECSECNCE	118.777	21.9977	118.037172	22.130129	116.517698	1.166962	199.22882002	23.39765052	280.879	56041.5636921296	2012-04-24 13:31:43	56044.5765856482	2012-04-27 13:50:17	407034010	119.1136	120	119.1136	119.1136	0	119.1136	3	2	0	2	1	0	0	102.8354	102.8354	260.306	1	PROCESSED	57605.3496064815	2016-08-05 08:23:26	56434	2013-05-22 00:00:00	56068.6228356482	2012-05-21 14:56:53	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070065	It has been believed that the optically thin boundary layer in dwarf novae (DNe) turns into optically thick state in outburst, and, as a result, hard optically thin X-ray emission becomes weaker than in quiescence. This theory was verified in multi-waveband observations of SS Cyg. The DN U Gem, however, does not follow this scenario, and the hard X-ray intensity increases in outburst as well as soft X-ray emission. We propose ToO observations of U Gem both in quiescence and in outburst in order to understand behavior of DNe in X-rays in general, by means of detailed spectroscopy of the soft disk blackbody component, the hard component reflected off the white dwarf, and a 6.4 keV iron line. This study eventually enables us to understand the origin of the Galactic Ridge X-ray Emission.	GALACTIC POINT SOURCES	4	B	TAKAYUKI HAYASHI		JAP	7	AO7-TOO	OBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407034010/	Quick Look
166	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
167	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
168	NGC 4593	189.915	-5.3482	189.270103	-5.073686	191.205514	-0.992169	297.48487911	57.39893055	292.7762	56824.1040972222	2014-06-16 02:29:54	56824.8563888889	2014-06-16 20:33:12	709014010	29.7616	30	29.7696	29.7616	0	29.7696	2	2	0	2	1	0	0	24.185	24.185	64.9919	1	PROCESSED	57615.2408449074	2016-08-15 05:46:49	57204	2015-07-01 00:00:00	56835.7291435185	2014-06-27 17:29:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090097	In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	9	AO9	X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014010/	Quick Look
169	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
170	1RXS J180340.0+40121	270.932	40.2098	270.526529	40.206239	271.586717	63.644696	66.8583442	25.77561005	157.538	54478.0290972222	2008-01-13 00:41:54	54479.1877777778	2008-01-14 04:30:24	402009010	53.0907	50	53.0907	53.0907	0	53.0907	1	1	0	1	1	0	0	44.3489	44.3489	100.0959	3	PROCESSED	57541.2965625	2016-06-02 07:07:03	54864	2009-02-02 00:00:00	54490.0707291667	2008-01-25 01:41:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020029	Soft Intermediate Polar (IP) is a small group of IPs whose X-ray spectrum is extremely soft compared with general IPs. Recent observations reveal that some soft IPs harbor a soft blackbody component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand possible evolutionary link from IPs to polars, the origin of the soft excess in polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure their temperature and flux systematically.	GALACTIC POINT SOURCES	4	C	MANABU ISHIDA		JAP	2	AO2	OBSERVATIONS OF SOFT INTERMEDIATE POLARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402009010/	Quick Look
171	SAGITTARIUS A*	266.4179	-29.0156	265.623138	-28.996274	266.843332	-5.613719	359.938084	-0.05101613	284.9967	56561.9008101852	2013-09-26 21:37:10	56562.4828587963	2013-09-27 11:35:19	408017040	18.3285	20	18.3422	18.3285	0	18.3422	3	2	0	3	1	0	0	18.9519	18.9519	50.282	0	PROCESSED	57612.7244560185	2016-08-12 17:23:13	56956	2014-10-26 00:00:00	56588.4972222222	2013-10-23 11:56:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017040/	Quick Look
172	SAGITTARIUS A*	266.4147	-29.0052	265.620004	-28.985859	266.84026	-5.603392	359.94550345	-0.04320951	106.9995	56723.0565277778	2014-03-07 01:21:24	56723.5487384259	2014-03-07 13:10:11	408017050	21.9949	20	21.9949	22.0029	0	22.0144	1	1	0	1	1	0	0	15.862	15.862	42.5199	1	PROCESSED	57613.9706828704	2016-08-13 23:17:47	57100	2015-03-19 00:00:00	56734.6444328704	2014-03-18 15:27:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017050/	Quick Look
173	GALACTIC CENTER	265.3803	-29.7558	264.581055	-29.731436	265.955939	-6.379444	358.83357751	0.33021849	269	54016.4324074074	2006-10-08 10:22:40	54017.0968055556	2006-10-09 02:19:24	501049010	19.5627	20	19.5627	19.5627	19.5627	19.5627	2	2	2	2	1	0	0	17.6336	17.6336	57.3959	1	PROCESSED	57535.7944675926	2016-05-27 19:04:02	54735	2008-09-26 00:00:00	54053.4403356482	2006-11-14 10:34:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501049010/	Quick Look
174	V2301 OPH	270.1519	8.1612	269.551065	8.161911	270.165981	31.601449	34.53664844	14.98247082	262.0703	56573.9878356482	2013-10-08 23:42:29	56576.0002893518	2013-10-11 00:00:25	408024010	40.1356	150	40.1356	40.1356	0	40.1356	2	2	0	2	1	0	0	65.6843	65.6843	173.8587	1	PROCESSED	57612.9068981482	2016-08-12 21:45:56	57184	2015-06-11 00:00:00	56596.5744907407	2013-10-31 13:47:16	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080107	It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion.	GALACTIC POINT SOURCES	4	A	TAKAYUKI HAYASHI		JAP	8	AO8	MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408024010/	Quick Look
175	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
176	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
177	RCW86_WEST	220.2753	-62.427	219.29491	-62.212988	240.606158	-43.963376	315.24703456	-2.20673417	96.1553	54864.7563194444	2009-02-02 18:09:06	54866.0134259259	2009-02-04 00:19:20	503001010	53.5519	50	53.5519	53.5519	0	53.5519	2	2	0	2	1	0	0	48.9081	48.9081	108.602	1	PROCESSED	57545.4580324074	2016-06-06 10:59:34	55329	2010-05-13 00:00:00	54880.570462963	2009-02-18 13:41:28	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030011	Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		JAP	3	AO3	RCW86 MAPPING OBSERVATION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503001010/	Quick Look
178	CYGNUS LOOP (P20)	311.9894	31.1824	311.473917	30.997098	326.586885	46.721175	73.97872298	-7.73281487	50.0002	54596.7397685185	2008-05-10 17:45:16	54597.51	2008-05-11 12:14:24	503056010	30.1129	25	30.1129	30.1343	0	30.1209	2	2	0	2	1	0	0	27.2057	27.2057	66.5339	0	PROCESSED	57545.8695023148	2016-06-06 20:52:05	54972	2009-05-21 00:00:00	54606.1121759259	2008-05-20 02:41:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503056010/	Quick Look
179	RCW 86	221.2555	-62.3618	220.269135	-62.150858	241.140538	-43.714444	315.68741681	-2.33681001	278.3377	53959.4574652778	2006-08-12 10:58:45	53961.1294907407	2006-08-14 03:06:28	501037010	59.8054	60	59.8294	59.8054	59.8294	59.8214	2	2	2	2	1	0	0	54.405	54.405	144.42	1	PROCESSED	57535.2984259259	2016-05-27 07:09:44	54394	2007-10-21 00:00:00	54021.0740972222	2006-10-13 01:46:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010054	We propose an observation of the Northwest region of RCW 86, one of Galactic supernova remnants (SNRs). Hard X-ray continuum of RCW 86 is accompanied by Fe K line emission at 6.4keV. There is strong possibility that the origin of this line is electrons and protons accelerated in the shell of the SNR. In PV phase, the Southeast region of RCW 86 will be observed, and the density of this region is much larger than that of the Northwest region. Therefore we must compare the fluxes of Fe line and hard continuum of both regions, and discuss the correlation between the flux and the density of emitting region. Such comparative study is very useful for understanding the particle acceleration in the shell-like SNRs.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		JAP	1	AO1	RCW 86:PECULIAR SNR WITH NEUTRAL FE K LINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501037010/	Quick Look
180	NGC 5347	208.2716	33.4399	207.717601	33.685673	191.037943	41.510938	62.06849004	75.29189994	312.225	54627.6603703704	2008-06-10 15:50:56	54628.6064699074	2008-06-11 14:33:19	703011010	42.1611	40	42.1611	42.1611	0	42.1611	2	2	0	2	1	0	0	37.1302	37.1302	81.734	1	PROCESSED	57542.8072569444	2016-06-03 19:22:27	55008	2009-06-26 00:00:00	54637.3250810185	2008-06-20 07:48:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030040	We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	3	AO3	COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703011010/	Quick Look
181	VELA JR P30	134.1665	-46.7036	133.737948	-46.510338	161.294913	-59.700207	267.059354	-0.84402772	347.0006	54654.7208449074	2008-07-07 17:18:01	54655.0844328704	2008-07-08 02:01:35	503042010	10.1159	10	10.1159	10.1159	0	10.1159	2	2	0	2	1	0	0	10.0536	10.0536	31.3839	0	PROCESSED	57542.9967592593	2016-06-03 23:55:20	55048	2009-08-05 00:00:00	54679.397962963	2008-08-01 09:33:04	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503042010/	Quick Look
182	1E1207.4-5209	182.5062	-52.436	181.851861	-52.157726	209.149793	-45.774623	296.5458403	9.92149786	302.4939	53946.5682060185	2006-07-30 13:38:13	53948.2603587963	2006-08-01 06:14:55	401030010	96.3519	120	96.3519	102.2784	96.3679	96.3519	3	2	3	3	1	0	0	94.0498	94.0498	135.3799	1	PROCESSED	57535.1230787037	2016-05-27 02:57:14	54750	2008-10-11 00:00:00	54132.8187268518	2007-02-01 19:38:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010152	1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object.	GALACTIC POINT SOURCES	4	B	ATSUMASA YOSHIDA		JAP	1	AO1	A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401030010/	Quick Look
183	A2218_offset	244.4769	65.4468	244.387309	65.566901	174.329918	79.629039	97.72059475	40.11912915	237.1965	53645.3474537037	2005-10-02 08:20:20	53646.32375	2005-10-03 07:46:12	100030020	44.8592	50	44.8592	46.1907	44.9141	45.3747	2	2	2	2	1	0	0	42.5366	42.5366	84.3439	0	PROCESSED	57527.5203125	2016-05-19 12:29:15	54247	2007-05-27 00:00:00	54036.969224537	2006-10-28 23:15:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000030	Search of redshifted (z=0.171) OVII emission line from warm-hot intergalactic matter around a cluster which shows a merger feature in the line of sight, with no central cool component. The depth of the structure can be ~20 Mpc, and the redshift allows a clear separation of the lines from the Galactic hot gas. The low background and the superior resolution of XIS in the soft X-ray energy range will allow the best measurement of the WHIM emission so far.	CALIBRATION	1	A	SWG		JAP	0	SWG	A2218 and its offset observation		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100030020/	Quick Look
184	RXJ1713-3946	258.1672	-39.4231	257.303004	-39.36394	260.487659	-16.371231	347.50735004	-0.13585591	267.9988	53989.9221643518	2006-09-11 22:07:55	53990.3106712963	2006-09-12 07:27:22	501065010	22.011	20	22.011	22.011	22.011	22.011	2	2	2	2	1	0	0	20.7973	20.7973	33.5579	0	PROCESSED	57535.5534606482	2016-05-27 13:16:59	54526	2008-03-01 00:00:00	54020.8390162037	2006-10-12 20:08:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501065010/	Quick Look
185	GC SGR D	267.0913	-27.9356	266.303192	-27.919557	267.412914	-4.520645	1.16847417	0.00287016	108.7996	54174.7887847222	2007-03-15 18:55:51	54176.2127199074	2007-03-17 05:06:19	501059010	62.2372	63	62.2372	62.2452	0	62.2452	2	2	0	2	1	0	0	54.3697	54.3697	123.028	0	PROCESSED	57537.7233912037	2016-05-29 17:21:41	54736	2008-09-27 00:00:00	54185.4865740741	2007-03-26 11:40:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501059010/	Quick Look
186	SAGITTARIUS A*	266.4197	-29.0062	265.624997	-28.986883	266.844677	-5.604282	359.94692786	-0.04746309	282.0043	56539.5310416667	2013-09-04 12:44:42	56540.000162037	2013-09-05 00:00:14	408017010	19.4579	20	19.4789	19.4579	0	19.4709	2	2	0	2	1	0	0	20.6423	20.6423	40.5219	0	PROCESSED	57612.4854976852	2016-08-12 11:39:07	56974	2014-11-13 00:00:00	56608.6493981482	2013-11-12 15:35:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017010/	Quick Look
187	ASO0078	59.472	32.09	58.682067	31.946958	63.963224	11.368156	162.76236061	-16.0043339	83.0007	55045.8202777778	2009-08-02 19:41:12	55046.3273032407	2009-08-03 07:51:19	504041010	21.312	20	21.32	21.32	0	21.312	1	1	0	1	1	0	0	21.2959	21.2959	43.7999	0	PROCESSED	57548.0349074074	2016-06-09 00:50:16	55430	2010-08-22 00:00:00	55064.0383912037	2009-08-21 00:55:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.	GALACTIC DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504041010/	Quick Look
188	E1821+643	275.5207	64.3306	275.456094	64.303959	318.282096	86.807262	93.98984501	27.40177083	228.4067	56239.7868981482	2012-11-08 18:53:08	56241.8217708333	2012-11-10 19:43:21	707016010	100.4132	100	100.4132	100.4132	0	100.4132	2	2	0	2	1	0	0	95.5411	95.5411	175.7799	2	PROCESSED	57608.0299421296	2016-08-08 00:43:07	56631	2013-12-05 00:00:00	56265.6966319444	2012-12-04 16:43:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070089	Central engines of AGN are considered to be generally in Multi-Zone Comptonization (MZC) condition (e.g., Noda et al. 2011a,b). To verify this thing on a high-luminosiy AGN, we suggest to observe Radio-Quiet Quasar E1821+643 By Suzaku. Utilizing a time variability of each Comptonization component, we will resolve spectral variable components, and study whether the central engine of E1821+643 is in MZC condition or not.	EXTRAGALACTIC COMPACT SOURCES	7	C	HIROUMI NODA		JAP	7	AO7	SUZAKU STUDY OF MULTI-ZONE COMPTONIZATION PICTURE ON THE CENTRAL ENGINE OF RADIO-QUIET QUASAR E1821+643	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707016010/	Quick Look
189	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
190	CYGNUS_LOOP_P17	312.199	30.014	311.677424	29.82795	326.178147	45.573278	73.16561663	-8.59879153	61.9999	53877.7613657407	2006-05-22 18:16:22	53878.0446064815	2006-05-23 01:04:14	501034010	14.1953	14	14.1993	14.2033	14.1993	14.1953	2	2	2	2	1	0	0	14.8231	14.8231	24.464	0	PROCESSED	57534.3944328704	2016-05-26 09:27:59	54394	2007-10-21 00:00:00	53926.1395833333	2006-07-10 03:21:00	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501034010/	Quick Look
191	JUPITER	103.8837	23.1078	103.127442	23.17281	102.752218	0.279385	192.54363279	11.16228902	264.4065	56762.7225115741	2014-04-15 17:20:25	56763.066099537	2014-04-16 01:35:11	508023030	8.9125	160	8.9125	8.9125	0	8.9125	2	2	0	2	1	0	0	6.9063	6.9063	22.6469	0	PROCESSED	57614.254212963	2016-08-14 06:06:04	57212	2015-07-09 00:00:00	56833.5559722222	2014-06-25 13:20:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023030/	Quick Look
192	HESSJ1741-B	265.2407	-30.3098	264.437915	-30.284751	265.852586	-6.937089	358.29952005	0.1396669	74.0024	54888.0423611111	2009-02-26 01:01:00	54889.4828587963	2009-02-27 11:35:19	503077010	51.2616	50	51.2696	51.2616	0	51.2696	2	2	0	2	1	0	0	43.7072	43.7072	124.4239	1	PROCESSED	57545.6763773148	2016-06-06 16:13:59	55330	2010-05-14 00:00:00	54908.5791550926	2009-03-18 13:53:59	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030113	HESSJ1741-302 is one of the most darkest TeV unidentified objects which was discovered with the H.E.S.S. telescope recently. The location strongly suggests that the object is physically connected to the diffuse TeV gamma-ray emission along the Galactic plane. On the other hand, there is a pulsar near the object, and it may be an off-set pulsar wind nebula. To clarify the origin of the object, we propose to the observation of HESSJ1741.	GALACTIC DIFFUSE EMISSION	5	C	HIRONORI MATSUMOTO		JAP	3	AO3	DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503077010/	Quick Look
193	1FGL J2339.7-0531	354.9077	-5.5469	354.264388	-5.824081	353.120926	-3.069352	81.34836456	-62.4702773	67.4026	55741.5915625	2011-06-29 14:11:51	55743.8092361111	2011-07-01 19:25:18	406007010	104.0914	100	104.0914	104.0914	0	104.0994	2	2	0	2	1	0	0	92.9022	92.9022	191.5837	2	PROCESSED	57602.4861805556	2016-08-02 11:40:06	56144	2012-08-05 00:00:00	55775.4025925926	2011-08-02 09:39:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060007	We propose to observe an unidentified Fermi source (1FGL J2339.7-0531) in the first-year Fermi catalog to search for the first ``radio-quiet'' Gamma-ray emitting millisecond pulsar. The Fermi source has a candidate X-ray counterpart from Chandra data and its X-ray and Gamma-ray properties are consistent with known Gamma-ray pulsars. This system is likely in a low-mass X-ray binary system based on optical observations. Both X-ray and optical observations show clear variability. We propose to observe the Chandra source with Suzaku to search for the possible orbital period and to study its X-ray spectrum in detail. The results will provide a better insight into the high-energy emission processes in the magnetosphere of millisecond pulsars.	GALACTIC POINT SOURCES	4	A	ALBERT KONG	JUN KATAOKA	JAP	6	AO6	REVEALING THE NATURE OF AN UNIDENTIFIED FERMI SOURCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406007010/	Quick Look
194	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
195	JUPITER	104.3715	23.0706	103.615684	23.137913	103.202438	0.28593	192.77027841	11.55390373	264.582	56766.448287037	2014-04-19 10:45:32	56766.781400463	2014-04-19 18:45:13	508023090	11.9454	160	11.9534	11.9454	0	11.9614	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57614.9588773148	2016-08-14 23:00:47	57212	2015-07-09 00:00:00	56782.506099537	2014-05-05 12:08:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023090/	Quick Look
196	SWIFT J1200.8+0650	180.2185	6.7488	179.57779	7.027186	177.502279	6.275772	270.13481807	66.34579154	293.0035	54617.9027662037	2008-05-31 21:39:59	54619.9280555556	2008-06-02 22:16:24	703009010	84.4866	80	84.5106	84.4866	0	84.5106	2	2	0	2	1	0	0	71.1109	71.1109	174.9638	3	PROCESSED	57542.752037037	2016-06-03 18:02:56	55003	2009-06-21 00:00:00	54634.1479282407	2008-06-17 03:33:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030034	The hard X-ray survey with Swift BAT have been finding various types of AGNs. Many buried AGNs with very low scattered X-rays have been discovered, for example. We propose to obtain broad band spectra of Compton-thin buried AGNs in the Swift sample. The data will be used to measure the amount of absoption in the direct and reflected emission and to constrain the structure of the obscuring matter around the AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	3	AO3	THE STRUCTURE OF BURIED COMPTON-THIN AGNS DISCOVERED BY SWIFT	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703009010/	Quick Look
197	VELA JR P27	133.2844	-46.6061	132.858246	-46.415943	160.180564	-59.949881	266.59417196	-1.24373956	347.0008	54653.8375925926	2008-07-06 20:06:08	54654.1668865741	2008-07-07 04:00:19	503039010	11.0337	10	11.0417	11.0417	0	11.0337	1	1	0	1	1	0	0	11.3372	11.3372	28.4479	0	PROCESSED	57542.9844560185	2016-06-03 23:37:37	55048	2009-08-05 00:00:00	54679.3497222222	2008-08-01 08:23:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503039010/	Quick Look
198	SGR D SNR	267.1922	-28.1274	266.402882	-28.111843	267.506075	-4.710631	1.05009547	-0.17236121	267.8977	54349.018599537	2007-09-06 00:26:47	54352.6738310185	2007-09-09 16:10:19	502020010	139.0808	133	139.0808	139.0808	0	139.0808	2	2	0	2	1	0	0	124.5025	124.5025	315.7798	1	PROCESSED	57540.026087963	2016-06-01 00:37:34	54776	2008-11-06 00:00:00	54371.5203472222	2007-09-28 12:29:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020031	We propose a 100 ksec observation of the Sgr D region. This region contains a supernova remnant (SNR), a massive molecular cloud, an HII region and diffuse TeV gamma-ray emission. The objectives are to detect Sgr D SNR and diffuse X-rays from the TeV source, to discover new SNRs and X-ray Reflection Nebulae (XRNe), and to investigate the spatial distribution of high temperature plasma connecting the Galactic center and the Galactic ridge regions.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	2	AO2	OBSERVATIONS OF SGR D SNR, A TEV SOURCE AND DIFFUSE X-RAYS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502020010/	Quick Look
199	SN 1006 SW-Rim	225.4961	-42.0706	224.678007	-41.87399	235.320846	-23.835662	327.36052248	14.52564865	117.2713	53761.0914930556	2006-01-26 02:11:45	53761.7155555556	2006-01-26 17:10:24	100019050	28.4186	50	28.4186	28.4186	28.4186	28.4186	2	2	2	2	1	0	0	24.7444	24.7444	53.91	0	PROCESSED	57532.7834375	2016-05-24 18:48:09	54247	2007-05-27 00:00:00	54040.4586689815	2006-11-01 11:00:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000019		CALIBRATION	1	A	SWG		JAP	0	SWG	SN1006 observation with XIS and HXD	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019050/	Quick Look
200	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
201	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
202	HESSJ1857-A	284.2126	2.7519	283.584668	2.685017	285.744612	25.418977	35.99783049	0.0515802	269.8116	55822.9197800926	2011-09-18 22:04:29	55823.984212963	2011-09-19 23:37:16	506019010	40.9249	40	40.9249	40.9249	0	40.9249	2	2	0	2	1	0	0	35.8469	35.8469	91.9279	1	PROCESSED	57603.2046180556	2016-08-03 04:54:39	56233	2012-11-02 00:00:00	55865.2326157407	2011-10-31 05:34:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060061	Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	6	AO6	ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506019010/	Quick Look
203	IC 443	94.2974	22.7535	93.540286	22.772525	93.964523	-0.628288	188.8890151	3.10517693	91.6993	56197.2290277778	2012-09-27 05:29:48	56199.7780324074	2012-09-29 18:40:22	507015010	101.8023	400	101.8103	101.8023	0	101.8103	2	2	0	2	1	0	0	91.994	91.994	220.1877	0	PROCESSED	57607.2728472222	2016-08-07 06:32:54	56018	2012-04-01 00:00:00	56225.5965162037	2012-10-25 14:18:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070015	The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	7	AO7	DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA --	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015010/	Quick Look
204	FERMI_BUBBLE_N4	233.8333	7.0797	233.2207	7.24518	229.504794	25.578453	13.3126084	46.30488493	287.5	56146.4387268518	2012-08-07 10:31:46	56146.9862615741	2012-08-07 23:40:13	507004010	20.9469	20	20.9509	20.9469	0	20.9549	2	2	0	2	1	0	0	20.7048	20.7048	47.306	2	PROCESSED	57606.7955787037	2016-08-06 19:05:38	56535	2013-08-31 00:00:00	56169.0484375	2012-08-30 01:09:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507004010/	Quick Look
205	GC15	266.9617	-29.4257	266.164223	-29.409004	267.329759	-6.012747	359.83382525	-0.66952641	260.7835	54383.1536226852	2007-10-10 03:41:13	54383.6391666667	2007-10-10 15:20:24	502003010	21.4671	20	21.4751	21.4671	0	21.4751	2	2	0	2	1	0	0	18.9225	18.9225	41.9439	0	PROCESSED	57540.2312731482	2016-06-01 05:33:02	54771	2008-11-01 00:00:00	54402.7485532407	2007-10-29 17:57:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502003010/	Quick Look
206	VELA JR P2	132.1691	-45.7748	131.740578	-45.588644	157.998003	-59.663034	265.4613949	-1.31133586	347.0033	54285.6908217593	2007-07-04 16:34:47	54285.9036342593	2007-07-04 21:41:14	502024010	10.8502	10	10.8742	10.8662	0	10.8502	1	1	0	1	1	0	0	9.6037	9.6037	18.3759	0	PROCESSED	57539.0914467593	2016-05-31 02:11:41	54696	2008-08-18 00:00:00	54328.4167361111	2007-08-16 10:00:06	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502024010/	Quick Look
207	1FGL J1715.2-3319	258.713	-33.4282	257.892464	-33.371742	260.432113	-10.360749	352.62684601	3.01774525	99.0737	56002.5629166667	2012-03-16 13:30:36	56003.3750810185	2012-03-17 09:00:07	406024010	32.165	30	32.165	32.165	0	32.165	2	2	0	2	1	0	0	27.9848	27.9848	70.166	0	PROCESSED	57604.9296064815	2016-08-04 22:18:38	56386	2013-04-04 00:00:00	56019.2516435185	2012-04-02 06:02:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060087	We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object.	GALACTIC POINT SOURCES	4	C	MASANORI OHNO		JAP	6	AO6	SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406024010/	Quick Look
208	VELA JR P33	133.4681	-47.1616	133.045488	-46.970785	161.00407	-60.345222	267.10091899	-1.50393046	347.0007	54655.5652777778	2008-07-08 13:34:00	54656.0084837963	2008-07-09 00:12:13	503045010	12.0155	10	12.0155	12.0155	0	12.0155	2	2	0	2	1	0	0	11.0116	11.0116	38.2899	0	PROCESSED	57543.0047106482	2016-06-04 00:06:47	55048	2009-08-05 00:00:00	54679.4195601852	2008-08-01 10:04:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503045010/	Quick Look
209	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
210	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
211	1RXSJ135341.1-664002	208.4233	-66.67	207.481758	-66.423993	237.082372	-50.124321	309.05087215	-4.54070575	288.5314	55774.1593055556	2011-08-01 03:49:24	55774.6939236111	2011-08-01 16:39:15	406036010	23.2679	20	23.2759	23.2679	0	23.2759	1	1	0	1	1	0	0	22.4241	22.4241	46.1839	0	PROCESSED	57602.7124189815	2016-08-02 17:05:53	56166	2012-08-27 00:00:00	55802.4628472222	2011-08-29 11:06:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060097	We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray.	GALACTIC POINT SOURCES	4	B	HIROMITSU TAKAHASHI		JAP	6	AO6	SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406036010/	Quick Look
212	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
213	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
214	EMS0857	198.1882	0.8497	197.548985	1.114667	196.443673	7.917565	314.828891	63.22804034	111.0249	55578.1935532407	2011-01-17 04:38:43	55578.746087963	2011-01-17 17:54:22	705011010	22.07	20	22.078	22.07	0	22.085	1	1	0	1	1	0	0	15.3267	15.3267	47.7279	0	PROCESSED	57600.6315046296	2016-07-31 15:09:22	55962	2012-02-05 00:00:00	55595.4732986111	2011-02-03 11:21:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050050	We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators".	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5	SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705011010/	Quick Look
215	3C454.3	343.4951	16.1379	342.877484	15.871411	351.362437	21.321746	86.10833014	-38.194784	252.9263	55525.0494675926	2010-11-25 01:11:14	55526.0141087963	2010-11-26 00:20:19	705021010	41.0252	40	41.0332	41.0332	0	41.0252	2	2	0	2	1	0	0	37.1412	37.1412	83.3278	0	PROCESSED	57554.2391319445	2016-06-15 05:44:21	55916	2011-12-21 00:00:00	55550.1355439815	2010-12-20 03:15:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050052	We propose 40 ksec x 2 (at most) Suzaku ToO observations - from a list of five -of GeV-bright flat spectrum radio quasars (FSRQs) that would be triggered by significant flaring (with E>100 MeV flux of 2x10^(-6) photons/cm^2/s or greater) in the Fermi all-sky monitoring. Those observations will be coordinated with optical and Swift XRT observations, with the goal of obtaining broadband spectra and light-curves during a flare gamma-ray activity. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the content and by extension, the accelertation process of the jet and energization of the radiating particles.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5-TOO	SUZAKU TOO OBSERVATION OF GIANT FLARE IN FRSQS TRIGGERED BY FERMI-LAT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705021010/	Quick Look
216	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
217	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
218	LMC X-2	80.025	-71.9941	80.229686	-72.041872	298.35324	-83.539153	283.14092563	-32.7117801	313.3022	53849.381712963	2006-04-24 09:09:40	53850.7731365741	2006-04-25 18:33:19	401012010	56.152	60	56.1657	56.1657	56.152	56.16	2	2	2	2	1	0	0	73.408	73.408	120.1938	1	PROCESSED	57533.5735300926	2016-05-25 13:45:53	54394	2007-10-21 00:00:00	53907.6288078704	2006-06-21 15:05:29	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010090	We propose the Suzaku observation of LMC X-2, to detect the slim disk structure in its flaring branch. The luminosity of LMC X-2 is always as luminous as the Eddington limit, and the absorption is so low that the energy spectrum can be observed over the 0.2-30 keV energy range. Then, LMC X-2 is the best target to study whether the disk structure becomes the slim disk or not.	GALACTIC POINT SOURCES	4	B	HIROMITSU TAKAHASHI		JAP	1	AO1	DETECTION OF SLIM-DISK STRUCTURE FROM LOW-MASS X-RAY BINARY LMC X-2	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401012010/	Quick Look
219	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
220	NGC 7130	327.065	-34.8962	326.317147	-35.128916	317.224283	-20.334869	10.02903365	-50.33744977	78.4767	54597.5198726852	2008-05-11 12:28:37	54598.56625	2008-05-12 13:35:24	703012010	44.4931	40	44.4931	44.4931	0	44.4931	1	1	0	1	1	0	0	36.7677	36.7677	90.3759	1	PROCESSED	57542.510474537	2016-06-03 12:15:05	54975	2009-05-24 00:00:00	54609.0170949074	2008-05-23 00:24:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030040	We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	3	AO3	COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703012010/	Quick Look
221	CYGNUS_LOOP_P10	311.5744	30.3992	311.055864	30.215413	325.67249	46.135207	73.13474548	-7.93635975	240.0007	54417.2506944444	2007-11-13 06:01:00	54417.6043402778	2007-11-13 14:30:15	501020010	16.7958	10	16.7958	16.8198	0	16.8038	2	2	0	2	1	0	0	12.6729	12.6729	30.5499	0	PROCESSED	57540.5008333333	2016-06-01 12:01:12	54798	2008-11-28 00:00:00	54430.1578472222	2007-11-26 03:47:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501020010/	Quick Look
222	SWIFT J2052.0-5704	312.9788	-57.0176	312.02055	-57.205734	297.951069	-37.67562	340.05945565	-38.72742848	73.9304	54945.6280671296	2009-04-24 15:04:25	54946.6863310185	2009-04-25 16:28:19	704010010	45.16	40	45.16	45.168	0	45.168	2	2	0	2	1	0	0	57.6242	57.6242	91.4098	1	PROCESSED	57546.2560416667	2016-06-07 06:08:42	55339	2010-05-23 00:00:00	54973.4487152778	2009-05-22 10:46:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040059	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	4	AO4	SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704010010/	Quick Look
223	SWIFT J1952.4+0237	298.0556	2.5705	297.425623	2.440903	300.700434	23.070542	42.31566647	-12.27488447	82.9116	54929.8284722222	2009-04-08 19:53:00	54931.1079166667	2009-04-10 02:35:24	704011010	47.9211	40	47.9259	47.9211	0	47.9259	2	2	0	2	1	0	0	39.3044	39.3044	110.5258	2	PROCESSED	57546.1208680556	2016-06-07 02:54:03	55324	2010-05-08 00:00:00	54949.4878356482	2009-04-28 11:42:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040059	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	4	AO4	SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704011010/	Quick Look
224	CTB109 NOTHWEST	345.2638	59.0349	344.742477	58.766045	23.94959	57.015916	109.14185824	-0.84931137	252.0017	55908.2838078704	2011-12-13 06:48:41	55909.1988078704	2011-12-14 04:46:17	506037010	40.7488	40	40.7488	40.7568	0	40.7648	2	2	0	2	1	0	0	39.201	39.201	79.044	0	PROCESSED	57604.1345601852	2016-08-04 03:13:46	56288	2012-12-27 00:00:00	55921.0397685185	2011-12-26 00:57:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060100	Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations.	GALACTIC DIFFUSE EMISSION	5	C	TOSHIO NAKANO		JAP	6	AO6	SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506037010/	Quick Look
225	NGC1365	53.4052	-36.1452	52.927869	-36.31215	36.804669	-53.045157	237.96410536	-54.59489483	47.2005	56107.1526041667	2012-06-29 03:39:45	56107.9972916667	2012-06-29 23:56:06	707017010	30.6949	30	30.6949	30.6949	0	30.6949	2	2	0	2	1	0	0	27.8321	27.8321	72.9738	0	PROCESSED	57606.5279050926	2016-08-06 12:40:11	56491	2013-07-18 00:00:00	56125.2372453704	2012-07-17 05:41:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070095	NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. }	EXTRAGALACTIC COMPACT SOURCES	7	B	YASUSHI FUKAZAWA		JAP	7	AO7	MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017010/	Quick Look
226	NGC 3516	166.6957	72.5543	165.843141	72.824666	123.386475	57.973853	133.24670004	42.41457084	283.0856	56435.1473148148	2013-05-23 03:32:08	56436.2952199074	2013-05-24 07:05:07	708006070	51.4752	50	51.4772	51.4752	0	51.4792	2	2	0	2	1	0	0	53.7203	53.7203	99.1658	1	PROCESSED	57611.3639351852	2016-08-11 08:44:04	56383	2013-04-01 00:00:00	56449.6609027778	2013-06-06 15:51:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080066	We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	8	AO8	THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006070/	Quick Look
227	CTB109 SOUTHEAST	345.764	58.7015	345.237296	58.43203	23.8569	56.597018	109.24155205	-1.25930647	252.0022	55910.7526851852	2011-12-15 18:03:52	55911.4007638889	2011-12-16 09:37:06	506040010	30.4455	30	30.4455	30.4455	0	30.4455	2	2	0	2	1	0	0	28.7511	28.7511	55.9879	1	PROCESSED	57604.1444212963	2016-08-04 03:27:58	56289	2012-12-28 00:00:00	55922.0080555556	2011-12-27 00:11:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060100	Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations.	GALACTIC DIFFUSE EMISSION	5	C	TOSHIO NAKANO		JAP	6	AO6	SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506040010/	Quick Look
228	NGC 4968	196.7464	-23.7282	196.071371	-23.461103	204.633939	-15.321329	307.51234678	39.00523278	298.8345	53954.7307523148	2006-08-07 17:32:17	53955.6822222222	2006-08-08 16:22:24	701005010	39.0508	40	39.0508	39.0508	39.0508	39.0508	2	2	2	2	1	0	0	35.617	35.617	82.1979	1	PROCESSED	57535.2527546296	2016-05-27 06:03:58	54408	2007-11-04 00:00:00	54020.7898148148	2006-10-12 18:57:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010037	We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	1	AO1	COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701005010/	Quick Look
229	AM HERCULES	274.126	49.8084	273.81383	49.78911	279.176537	73.11739	77.81082077	25.81903319	234.8814	54768.8590162037	2008-10-29 20:36:59	54771.3043287037	2008-11-01 07:18:14	403007010	108.4965	100	108.5045	108.5045	0	108.4965	2	2	0	2	1	0	0	94.4671	94.4671	211.2577	3	PROCESSED	57544.3392476852	2016-06-05 08:08:31	55156	2009-11-21 00:00:00	54788.4722222222	2008-11-18 11:20:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030021	We propose the observation of the proto-type magnetic catacrysmic variables, AM Hercules, to search for possible hard X-ray tail on the thermal emission with Suzaku. To reduce the systematics of the estimation of the GSO background in the analyses, we propose the additional observation of blank sky near the object.	GALACTIC POINT SOURCES	4	C	YUKIKATSU TERADA		JAP	3	AO3	NON THERMAL EMISSION FROM THE POLAR AM HERCULES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403007010/	Quick Look
230	HESS J1356-645 1	209.4297	-64.5068	208.507718	-64.263148	235.862386	-48.071536	309.98959301	-2.54712319	106.5083	56318.4192939815	2013-01-26 10:03:47	56320.0002083333	2013-01-28 00:00:18	507019010	55.7489	50	55.762	55.7569	0	55.7489	2	2	0	2	1	0	0	65.1023	65.1023	136.5678	2	PROCESSED	57608.6328587963	2016-08-08 15:11:19	56708	2014-02-20 00:00:00	56342.6666319444	2013-02-19 15:59:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070017	Recently, pulsar wind nebulae is focused on one of the electron accelerators in our Galaxy. Especially TeV pulsar wind nebulae are supposed to have a largely extended X-ray emission. Since the X-ray emission is much larger than the size considering the typical electron lifetime, high energy electrons strangely seem to be transferred too fast or without cooling. To study the electron diffusion of young pulsar wind nebula, we propose observations of HESS J1356-645, which is off the Galactic plane and is free from the Galactic ridge X-ray emission.	GALACTIC DIFFUSE EMISSION	5	C	TAKAHISA FUJINAGA		JAP	7	AO7	OFF-PLANE TEV GAMMA-RAY SOURCE HESS J1356-645	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507019010/	Quick Look
231	A 2052	229.0471	6.9211	228.432118	7.104686	224.516271	24.128025	9.16646689	50.17566284	281.2031	53603.6121875	2005-08-21 14:41:33	53603.9938425926	2005-08-21 23:51:08	100006040	16.7443	20	16.7443	16.7443	16.7443	16.7443	1	1	1	1	1	0	0	12.8395	12.8395	32.9519	0	PROCESSED	57520.7325810185	2016-05-12 17:34:55	53705	2005-12-01 00:00:00	53905.4634143518	2006-06-19 11:07:19	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000006		CALIBRATION	1	A	SWG		JAP	0	SWG	Outer region of A 2052		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006040/	Quick Look
232	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
233	Crab Nebula	83.5484	22.0881	82.795741	22.055005	84.024019	-1.219032	184.45272098	-5.81121698	85.0004	53614.9103009259	2005-09-01 21:50:50	53615.0418518518	2005-09-02 01:00:16	100015050	5.3447	5	5.3447	5.3447	5.3447	5.3447	1	1	1	1	1	0	0	5.4859	5.4859	11.356	0	PROCESSED	57527.2511342593	2016-05-19 06:01:38	54247	2007-05-27 00:00:00	54109.1357986111	2007-01-09 03:15:33	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000015		CALIBRATION	1	A	SWG		JAP	0	SWG	HXD boresight check with Crab		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015050/	Quick Look
234	EP DRA	286.7359	69.1573	286.793684	69.076999	30.014466	83.210835	100.08892772	23.87463538	44.5637	57164.4409953704	2015-05-22 10:35:02	57166.2856365741	2015-05-24 06:51:19	410006010	80.2346	80	80.2346	80.2426	0	80.2426	2	2	0	2	1	0	0	67.9585	67.9585	155.5819	1	PROCESSED	57618.7517939815	2016-08-18 18:02:35	57558	2016-06-19 00:00:00	57176.3159027778	2015-06-03 07:34:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	100018	It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar mass (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar mass and approach 3.3 solar mass. We will get observational relations between WD mass and radius for proposed targets with Suzaku. With WD masses dynamically measured, we can estimate the WD radii without any theoretical mass-radius relation. We will be able to, for the first time, observationally investigate the influence of magnetic field on EOS in WDs and the WD mass-radius relation by the estimating WD radii and masses.	GALACTIC POINT SOURCES	4	A	TAKAYUKI HAYASHI		JAP	10	AO10	CONSTRAINT ON MASS-RADIUS RELATION OF HIGHLY MAGNETIZED WHITE DWARFS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410006010/	Quick Look
235	Cas A	350.8254	58.8156	350.259841	58.54105	27.364711	54.864063	111.72292809	-2.12474901	12.9937	53614.2486458333	2005-09-01 05:58:03	53614.7640509259	2005-09-01 18:20:14	100016010	27.965	20	27.973	27.973	27.973	27.965	2	2	2	2	1	0	0	24.13	24.13	44.4959	2	PROCESSED	57527.2832175926	2016-05-19 06:47:50	53705	2005-12-01 00:00:00	53905.4659606482	2006-06-19 11:10:59	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000016		CALIBRATION	1	A	SWG		JAP	0	SWG	Cas A		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100016010/	Quick Look
236	VW HYI	62.2833	-71.2901	62.373607	-71.419454	322.048735	-79.101508	284.88594452	-38.13999051	181.9815	55894.1004513889	2011-11-29 02:24:39	55895.1821759259	2011-11-30 04:22:20	406009010	70.0834	60	70.0914	70.0834	0	70.0914	2	2	0	2	1	0	0	64.9701	64.9701	93.4468	1	PROCESSED	57604.0242939815	2016-08-04 00:34:59	56274	2012-12-13 00:00:00	55907.1562615741	2011-12-12 03:45:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060023	SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate.	GALACTIC POINT SOURCES	4	B	KEI SAITOU		JAP	6	AO6-TOO	TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009010/	Quick Look
237	H2356_VICINITY_A	359.8969	-30.2089	359.255002	-30.487352	346.863445	-27.454803	14.71906615	-78.22459894	68.0006	55696.8464583333	2011-05-15 20:18:54	55698.0938773148	2011-05-17 02:15:11	506028010	52.1657	50	52.1657	52.1657	0	52.1657	2	2	0	2	1	0	0	46.5791	46.5791	107.7539	1	PROCESSED	57602.0723148148	2016-08-02 01:44:08	56075	2012-05-28 00:00:00	55708.0697106482	2011-05-27 01:40:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060075	We propose to observe the two vicinities of H2356-309 for 50 ks each. Absorption lines from ions at z=0 and z=0.03 has been observed with grating spectrometers in the spectrum of H2356-309. Emission analysis with Suzaku will provide independent information on the medium responsible for the absorption lines. By combining the emission surface brightness and aborption equivalent width, we will constrain the temperature and physical length of the interstellar and intergalactic medium.	GALACTIC DIFFUSE EMISSION	5	A	YOH TAKEI		JAP	6	AO6	EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC AND INTERGALACTIC WARM-HOT GAS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506028010/	Quick Look
238	H2356_VICINITY_B	359.9868	-29.9493	359.345168	-30.227755	347.07269	-27.257526	15.89682365	-78.35224854	69.5008	55698.0951388889	2011-05-17 02:17:00	55699.3474305556	2011-05-18 08:20:18	506029010	51.4072	50	51.4312	51.4232	0	51.4072	2	2	0	2	1	0	0	42.546	42.546	108.1559	1	PROCESSED	57602.0868402778	2016-08-02 02:05:03	56075	2012-05-28 00:00:00	55708.1035069444	2011-05-27 02:29:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060075	We propose to observe the two vicinities of H2356-309 for 50 ks each. Absorption lines from ions at z=0 and z=0.03 has been observed with grating spectrometers in the spectrum of H2356-309. Emission analysis with Suzaku will provide independent information on the medium responsible for the absorption lines. By combining the emission surface brightness and aborption equivalent width, we will constrain the temperature and physical length of the interstellar and intergalactic medium.	GALACTIC DIFFUSE EMISSION	5	A	YOH TAKEI		JAP	6	AO6	EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC AND INTERGALACTIC WARM-HOT GAS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506029010/	Quick Look
239	HESS_J1809-193_S	272.3365	-19.5311	271.597005	-19.540657	272.197453	3.891828	10.84429394	0.04252392	106.4999	54557.6901851852	2008-04-01 16:33:52	54558.6161805556	2008-04-02 14:47:18	503079010	44.2481	40	44.2481	44.2481	0	44.2481	2	2	0	2	1	0	0	32.2142	32.2142	79.9698	1	PROCESSED	57542.0277546296	2016-06-03 00:39:58	54950	2009-04-29 00:00:00	54570.1866666667	2008-04-14 04:28:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030126	A survey of the Galactic plane with H.E.S.S. has revealed the existance of several new very-high-energy (VHE) gamma-ray sources. As gamma rays are produced by interactions of relativistic particles, observing VHE emission reveals the acceleration sites of particles. Although it had been thought that such acceleration occur in the shock of SNR, it became clear that several VHE sources are pulsar wind nebulae (PWNe). This indicates that PWNe are also the acceleration sites of particles. HESS J1809-193 is a diffuse and a pulsar wind nebula candidate source, but details of the VHE emission mechanisms have been unclear yet. With the high sensitivity of XIS, we investigate spatial distribution of the spectrum around HESS J1809-193 and reveal its nature and the VHE emission mechanism.	GALACTIC DIFFUSE EMISSION	5	A	TAKAYASU ANADA		JAP	3	AO3	INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503079010/	Quick Look
240	CYG_BGD1	306.6527	39.4856	306.195949	39.320312	325.617981	56.073001	78.0015669	0.73572902	218.9004	56280.1666666667	2012-12-19 04:00:00	56280.6286458333	2012-12-19 15:05:15	507041010	26.9324	25	26.9404	26.9324	0	26.9404	1	1	0	1	1	0	0	20.4527	20.4527	39.9119	0	PROCESSED	57608.3151273148	2016-08-08 07:33:47	56683	2014-01-26 00:00:00	56316.5312268518	2013-01-24 12:44:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070060	The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object.	GALACTIC DIFFUSE EMISSION	5	C	TSUNEFUMI MIZUNO		JAP	7	AO7	SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507041010/	Quick Look
241	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
242	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
243	3C 236 BACKGROUND	151.1488	34.7362	150.413548	34.979134	140.636655	21.408004	190.35215815	53.68789407	299.9977	56055.786712963	2012-05-08 18:52:52	56056.7919444444	2012-05-09 19:00:24	707006010	46.2113	40	46.2113	46.2113	0	46.2113	2	2	0	2	1	0	0	44.1095	44.1095	86.8399	0	PROCESSED	57605.3836574074	2016-08-05 09:12:28	56436	2013-05-24 00:00:00	56070.1639930556	2012-05-23 03:56:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070014	Through the Suzaku observations of giant radio galaxies, of which the size is larger than about 1 Mpc, we are going to reveal a picture that the jets in radio galaxies become inactive as they evolve from 500 kpc to 1 Mpc. However, the current Suzaku sample of the giant radio galaxies is far from being satisfactory to make a definite conclusion. Therefore, we propose a Suzaku observation of 3C 236, one of the most giant radio galaxy in the Universe.	EXTRAGALACTIC COMPACT SOURCES	7	A	NAOKI ISOBE		JAP	7	AO7	INVESTIGATION INTO EVOLUTION OF THE JET ENERGETICS, THROUGH THE SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 236	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707006010/	Quick Look
244	NEP	272.7884	65.9814	272.771336	65.967881	333.879188	88.742697	95.75202722	28.67554678	290.9299	53615.6136921296	2005-09-02 14:43:43	53617.625162037	2005-09-04 15:00:14	100018010	106.2015	100	106.2015	106.2175	106.2495	106.2255	2	2	2	2	1	0	0	106.125	106.125	173.5718	3	PROCESSED	57527.2880092593	2016-05-19 06:54:44	53705	2005-12-01 00:00:00	53905.4636921296	2006-06-19 11:07:43	3.0.22.43	6	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000018		CALIBRATION	1	A	SWG		JAP	0	SWG	HXD background at North Ecliptic Pole		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100018010/	Quick Look
245	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
246	JUPITER	103.8407	23.1129	103.084394	23.177707	102.712362	0.280692	192.5219391	11.12856775	264.3937	56762.3891782407	2014-04-15 09:20:25	56762.7223611111	2014-04-15 17:20:12	508023020	15.4083	160	15.4083	15.4083	0	15.4083	1	1	0	1	1	0	0	12.2744	12.2744	28.7839	1	PROCESSED	57614.2553819445	2016-08-14 06:07:45	57212	2015-07-09 00:00:00	56778.6154166667	2014-05-01 14:46:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023020/	Quick Look
247	Crab Nebula	83.6274	22.0192	82.875108	21.986487	84.094124	-1.29112	184.55062413	-5.78629385	86.8663	53604.1571412037	2005-08-22 03:46:17	53604.2501273148	2005-08-22 06:00:11	100007010	1.7229	5	1.7229	1.7229	1.7229	1.7229	1	1	1	1	1	0	0	1.808	1.808	8.034	0	PROCESSED	57520.7330324074	2016-05-12 17:35:34	54247	2007-05-27 00:00:00	54105.2758912037	2007-01-05 06:37:17	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000007	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Nebula		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100007010/	Quick Look
248	Crab nebula	83.6201	22.1854	82.866876	22.152649	84.094711	-1.124779	184.40591259	-5.70300776	86.8631	53604.2507175926	2005-08-22 06:01:02	53604.3889351852	2005-08-22 09:20:04	100007020	3.0531	5	3.0571	3.0531	3.0531	3.0531	1	1	1	1	1	0	0	3.1343	3.1343	11.94	1	PROCESSED	57520.7416782407	2016-05-12 17:48:01	54247	2007-05-27 00:00:00	54105.2987268518	2007-01-05 07:10:10	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000007	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Nebula		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100007020/	Quick Look
249	Crab nebula	83.4512	22.0082	82.699013	21.974637	83.930395	-1.294795	184.47195778	-5.93010486	86.7989	53604.489849537	2005-08-22 11:45:23	53604.5835416667	2005-08-22 14:00:18	100007040	4.2682	5	4.2682	4.2682	4.2682	4.2682	1	1	1	1	1	0	0	4.1392	4.1392	8.056	0	PROCESSED	57520.7454513889	2016-05-12 17:53:27	54247	2007-05-27 00:00:00	54105.3073726852	2007-01-05 07:22:37	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000007	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Nebula		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100007040/	Quick Look
250	NGC 4945	196.3733	-49.4666	195.643253	-49.198924	217.025297	-38.636782	305.27803835	13.34111135	313.9078	53605.101087963	2005-08-23 02:25:34	53605.1034490741	2005-08-23 02:28:58	100008020	0.1776	10	0.1815	0.1815	0.1796	0.1776	1	1	1	1	1	0	0	0.2001	0.2001	0.202	0	PROCESSED	57526.8486574074	2016-05-18 20:22:04	54247	2007-05-27 00:00:00	54034.6891435185	2006-10-26 16:32:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000008		CALIBRATION	1	A	SWG		JAP	0	SWG	NGC 4945		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100008020/	Quick Look
251	CYG X-1	299.5907	35.1892	299.120596	35.052727	313.656273	54.237702	71.32454904	3.06010347	276.9898	53648.2025347222	2005-10-05 04:51:39	53648.6335532407	2005-10-05 15:12:19	100036010	18.213	20	18.213	18.213	18.213	18.213	1	1	1	1	1	0	0	18.1457	18.1457	37.2299	0	PROCESSED	57527.5598726852	2016-05-19 13:26:13	54247	2007-05-27 00:00:00	54037.7278819444	2006-10-29 17:28:09	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000036	We propose to probe the geometry of optically-thick accretion disks which should exist around a BH even in the hard state and to verify the HXD performance to thermal cut-off in hard X-rays expected from AGN. The 1st may be done by measuring the cool disk emission with the XIS-BI, resolving the fluorescent Fe-K line with the XIS-FI and detecting the reflection continuum with the HXD. Since these features are thought to come from the optically-thick disk a simultaneous measurement will for the 1st time allow for self-consistent constraining of the disk geometry in the hard state. Cyg X-1 is the best & most secure object for this stufy and is now in the low/hard state. A 20 ks Suzaku obs. is sufficient to get a fine spectrum up to 300 keV & to determine the cutoff with a high significance.	CALIBRATION	1	A	SWG		JAP	0	SWG	Cyg X-1 in the low state		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100036010/	Quick Look
252	Sgr_B2	266.8775	-28.4435	266.086257	-28.426412	267.234561	-5.032377	0.63628385	-0.09835114	265.3727	53653.5194560185	2005-10-10 12:28:01	53655.2954050926	2005-10-12 07:05:23	100037060	76.5966	100	76.6286	76.6446	76.5966	76.6286	2	2	2	2	1	0	0	70.8192	70.8192	153.4319	0	PROCESSED	57527.5776041667	2016-05-19 13:51:45	54247	2007-05-27 00:00:00	54036.2262731482	2006-10-28 05:25:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000037		CALIBRATION	1	A	SWG		JAP	0	SWG	Suzaku Obseration of Galactic Center region 2		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037060/	Quick Look
253	Sgr_B2_BGD	267.0943	-28.1356	266.304946	-28.119568	267.419629	-4.720546	0.99854005	-0.10262599	269.0208	53655.2988888889	2005-10-12 07:10:24	53655.4620833333	2005-10-12 11:05:24	100037070	9.1612	10	9.1612	9.1643	9.1643	9.1632	2	2	2	2	1	0	0	9.5364	9.5364	14.092	0	PROCESSED	57527.5688078704	2016-05-19 13:39:05	54247	2007-05-27 00:00:00	54036.0749884259	2006-10-28 01:47:59	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000037		CALIBRATION	1	A	SWG		JAP	0	SWG	Suzaku Obseration of Galactic Center region 2		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037070/	Quick Look
254	MKN 3	93.8839	71.0477	92.433649	71.063052	91.875357	47.63268	143.2836301	22.71631463	71.8326	53665.0848263889	2005-10-22 02:02:09	53667.2682175926	2005-10-24 06:26:14	100040010	95.0265	100	95.0265	95.0772	95.0452	95.0345	2	2	2	2	1	0	0	91.3441	91.3441	188.6299	0	PROCESSED	57527.6643055556	2016-05-19 15:56:36	54247	2007-05-27 00:00:00	53906.4896759259	2006-06-20 11:45:08	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000040	Mkn 3 is the second brightest Compton-thick Sy 2 currently visible with Suzaku. The broadband spectrum of Mkn 3, as probed by previous SAX and Chandra observations, is dominated by a reflection component (Compton hump strength R is near 1), but there is also evidence for a strongly absorbed hard X-ray power law that may be direct emission from the obscured nucleus, filtering through Compton-thick material (such as the molecular torus).	CALIBRATION	1	A	SWG		JAP	0	SWG	MKN 3	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100040010/	Quick Look
255	RXJ1856.5-3754	284.1498	-37.9103	283.298136	-37.976359	281.509901	-15.033652	358.59888263	-17.21635309	269.4259	53667.2829976852	2005-10-24 06:47:31	53669.4793287037	2005-10-26 11:30:14	100041010	76.2548	80	0	76.2548	0	0	0	2	0	0	1	0	0	62.6217	62.6217	189.72	3	PROCESSED	57527.6811111111	2016-05-19 16:20:48	54247	2007-05-27 00:00:00	54037.2294791667	2006-10-29 05:30:27	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000041	We propose Suzaku observation of a nearby isolated neuron star RXJ1856.5-3754 for the low energy QE calibration of the XIS. Our main purpose is, however, using this source as a soft X-ray QE calibrator on the sky. We hope this source will be observed again in future to check possible contamination on the filter surface etc. Note that the calibration is not only for the BI-CCD(XIS1), but also for FI-CCDs or relative QE among them.	CALIBRATION	1	A	SWG		JAP	0	SWG	LOW ENERGY QE CALIBRATION OF XIS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100041010/	Quick Look
256	RXJ1713-3946_ID3	258.1658	-40.0306	257.296734	-39.971421	260.540524	-16.976597	347.01547145	-0.49239611	87.0009	55244.1262847222	2010-02-17 03:01:51	55244.4779398148	2010-02-17 11:28:14	504029010	20.8716	20	20.9036	20.9036	0	20.8716	1	1	0	1	1	0	0	20.8868	20.8868	30.3759	0	PROCESSED	57550.6116087963	2016-06-11 14:40:43	55622	2011-03-02 00:00:00	55256.0720601852	2010-03-01 01:43:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040021	We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009.	GALACTIC DIFFUSE EMISSION	5	B	TADAYUKI TAKAHASHI		JAP	4	AO4	STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504029010/	Quick Look
257	G11.2-0.3	272.8676	19.433	272.324919	19.420376	273.677117	42.836704	46.34586116	17.29738119	77.6432	53834.4626041667	2006-04-09 11:06:09	53835.6634143518	2006-04-10 15:55:19	401010010	43.9846	50	43.9926	43.9846	43.9926	43.9926	2	2	2	2	1	0	0	37.3879	37.3879	83.6799	1	PROCESSED	57533.4279166667	2016-05-25 10:16:12	54397	2007-10-24 00:00:00	53905.4671875	2006-06-19 11:12:45	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010049	The PSR 1811-1925 in a historical supernova remnant G11.2-0.3 has its characteristic age as 10 times longer than the age of the remnant. The pulsar has its period 64 ms and the hard spectrum. We suggest that the pulsar shows the signs of having the small magnetic field. The SUZAKU observation must give the answer for this hypothesis. First, HXD allows us to observe the spectrum in the high energy range, and if the cut-off would be observed, the magnetic fields of pulsar will be estimate. Seconds, XIS has the great energy resolution to determine the abundance of the shell. This would let us estimate the mass of the progenitor. Third, HXD provides the new spin down rate observation. Then, we can make sure the constancy of the spin down rate. The pulsar age mystery must be solved by SUZAKU.	GALACTIC POINT SOURCES	4	C	ASAMI HAYATO		JAP	1	AO1	CLEARING UP THE MECHANISM OF THE PSR J1811-1925 IN SNR G11.2-0.3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401010010/	Quick Look
258	PSR B1259-63	195.6732	-63.8823	194.883764	-63.613652	227.720536	-50.935927	304.17036556	-1.03761834	285.8945	54294.6568865741	2007-07-13 15:45:55	54295.3459953704	2007-07-14 08:18:14	402014040	22.9149	20	22.9149	22.9149	0	22.9149	2	2	0	2	1	0	0	21.0706	21.0706	59.4959	1	PROCESSED	57539.2651273148	2016-05-31 06:21:47	54709	2008-08-31 00:00:00	54339.4142592593	2007-08-27 09:56:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014040/	Quick Look
259	HOT BLOB 2	131.2547	53.3234	130.330211	53.505247	118.317658	33.861433	164.89716269	38.20704104	284.8982	57137.3573842593	2015-04-25 08:34:38	57139.1293055556	2015-04-27 03:06:12	509008010	46.0224	80	46.0224	77.9795	0	78.0115	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.041412037	2016-08-18 00:59:38	57520	2016-05-12 00:00:00	57154.4516087963	2015-05-12 10:50:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090044	Hot blobs including plasma of temperature kT = 0.6 - 1.0 keV in the Milky-Way Halo were found in 1/10 of the sky by systematical analysis of the soft X-ray diffuse background in Suzaku/XIS observations. They can play a role in matter and energy transportation among the Galactic plane, the Milky-Way Halo and intergalactic space. In order to reveal origin and physical condition of them, we focus on the part of a hot blob in (ell, b) = (161.505, 40.696) and propose to observe neighboring this area to constrain its size.	GALACTIC DIFFUSE EMISSION	5	C	NORIO SEKIYA		JAP	9	AO9	ORIGIN AND PHYSICAL CONDITION OF HOT BLOBS IN THE MILKY-WAY HALO	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509008010/	Quick Look
260	IC 443	94.3028	22.7465	93.545727	22.765551	93.96971	-0.635136	188.89754986	3.10625906	259.0005	56378.1771527778	2013-03-27 04:15:06	56379.6668865741	2013-03-28 16:00:19	507015020	59.2712	300	59.2712	59.2712	0	59.2712	2	2	0	2	1	0	0	51.2705	51.2705	128.6878	3	PROCESSED	57610.9601388889	2016-08-10 23:02:36	56018	2012-04-01 00:00:00	56391.749224537	2013-04-09 17:58:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070015	The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	7	AO7	DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA --	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015020/	Quick Look
261	MARS-P1	102.8773	25.1625	102.108873	25.222717	101.648232	2.240772	190.24974394	11.19384085	298.0037	54559.3414814815	2008-04-03 08:11:44	54559.4099421296	2008-04-03 09:50:19	403006010	2.9048	100	2.9048	2.9128	0	2.9128	1	1	0	1	1	0	0	2.9096	2.9096	5.9119	0	PROCESSED	57542.0343981482	2016-06-03 00:49:32	54953	2009-05-02 00:00:00	54577.0446875	2008-04-21 01:04:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006010/	Quick Look
262	MARS-P4	103.0016	25.1536	102.233284	25.214407	101.761173	2.241936	190.30618657	11.29219101	298.0476	54559.5767592593	2008-04-03 13:50:32	54559.6599421296	2008-04-03 15:50:19	403006040	2.2882	100	2.2882	2.2882	0	2.2882	1	1	0	1	1	0	0	2.01	2.01	7.1839	0	PROCESSED	57542.0411226852	2016-06-03 00:59:13	54953	2009-05-02 00:00:00	54577.0528935185	2008-04-21 01:16:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006040/	Quick Look
263	MARS-P15	103.4611	25.1019	102.69331	25.164885	102.180485	2.228357	190.53184536	11.64832678	298.2083	54560.4934375	2008-04-04 11:50:33	54560.5766666667	2008-04-04 13:50:24	403006150	3.831	100	3.839	3.831	0	3.847	1	1	0	1	1	0	0	3.1928	3.1928	7.1839	1	PROCESSED	57542.0622222222	2016-06-03 01:29:36	54953	2009-05-02 00:00:00	54580.5809837963	2008-04-24 13:56:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006150/	Quick Look
264	AM HERCULES BGD	282.0964	47.9785	281.757583	47.920958	294.678535	70.385314	77.40285415	20.2844947	234.9986	54771.3072106482	2008-11-01 07:22:23	54772.3438310185	2008-11-02 08:15:07	403008010	44.3601	40	44.3681	44.3601	0	44.3921	2	2	0	2	1	0	0	40.4115	40.4115	89.5519	1	PROCESSED	57544.3170833333	2016-06-05 07:36:36	55154	2009-11-19 00:00:00	54788.4288541667	2008-11-18 10:17:33	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030021	We propose the observation of the proto-type magnetic catacrysmic variables, AM Hercules, to search for possible hard X-ray tail on the thermal emission with Suzaku. To reduce the systematics of the estimation of the GSO background in the analyses, we propose the additional observation of blank sky near the object.	GALACTIC POINT SOURCES	4	C	YUKIKATSU TERADA		JAP	3	AO3	NON THERMAL EMISSION FROM THE POLAR AM HERCULES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403008010/	Quick Look
265	RXJ0007.0+7302	1.8916	72.9843	1.226338	72.706084	53.083805	60.867639	119.68700382	10.38954096	241.7328	55204.6112847222	2010-01-08 14:40:15	55207.0675231482	2010-01-11 01:37:14	404011010	105.3739	100	105.3739	105.3739	0	106.9714	2	2	0	1	1	0	0	58.5644	58.5644	212.2059	2	PROCESSED	57550.1958564815	2016-06-11 04:42:02	55587	2011-01-26 00:00:00	55768.9633333333	2011-07-26 23:07:12	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040054	We propose to observe the gamma-ray pulsar and itswind nebula (PWN) in the supernova remnant CTA1 with SUZAKU. Observations in X-ray wavebands are crucial to study non-thermal processes of PWNe. Its flux and spectral shape provide us important information about the energy distribution of the accelerated particles and the strength of the magnetic field. Observations made by Suzaku-HXD will constrain the X-ray spectrum above 20keV from the PWN for the first time. The high spectral resolution of XIS will allow us to search for metal lines, which tell us circumstance of the emission region. In addition, we will probably able to detect X-ray pulsation, which has notbeen detected yet, using XIS timing mode.	GALACTIC POINT SOURCES	4	C	JUMPEI TAKATA		JAP	4	AO4	X-RAY OBSERVATIONS OF GAMMA-RAY PULSAR AND ITS WIND NEBULA IN CTA1	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404011010/	Quick Look
266	FO AQR	334.4646	-8.2931	333.805898	-8.543636	333.309968	2.14088	53.06192299	-49.11309098	76.4186	54987.3437152778	2009-06-05 08:14:57	54988.5536921296	2009-06-06 13:17:19	404032010	46.0846	40	46.0846	46.0846	0	46.0846	2	2	0	2	1	0	0	33.4993	33.4993	104.5299	0	PROCESSED	57547.5153356482	2016-06-08 12:22:05	55366	2010-06-19 00:00:00	54998.3271064815	2009-06-16 07:51:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040113	We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.	GALACTIC POINT SOURCES	4	A	TAKAYUKI YUASA		JAP	4	AO4	SURVEY OBSERVATION OF INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404032010/	Quick Look
267	LOW_LATITUDE_97-10	311.8076	60.1112	311.52726	59.92615	0.701483	70.601802	96.61384914	10.40907029	101.0346	54571.1324652778	2008-04-15 03:10:45	54572.8890509259	2008-04-16 21:20:14	503075010	79.8119	80	79.8199	79.8279	0	79.8119	2	2	0	2	1	0	0	80.8105	80.8105	151.7498	2	PROCESSED	57542.342962963	2016-06-03 08:13:52	54953	2009-05-02 00:00:00	54581.3271643518	2008-04-25 07:51:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030105	Suzaku observations of diffuse background emission indicate galactic-latitude dependence of OVII intensity. The result of our AO-2 observation strongly supports this dependence. This suggests that the major part of the emission is originating from the halo or the extended disk of our galaxy. In order to confirm the galactic-latitude dependency and to constrain the spatial distribution of the OVII emitting gas, we propose to observe diffuse radiation at a low galactic latitude of ~ 10 deg.	GALACTIC DIFFUSE EMISSION	5	B	TOMOTAKA YOSHINO		JAP	3	AO3	RESOLVING LARGE-SCALE SPATIAL DEPENDENCE OF SOFT X-RAY DIFFUSE EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503075010/	Quick Look
268	IGR J15094-6649	227.3484	-66.8278	226.235673	-66.63712	247.091848	-46.74399	315.91945149	-7.50109233	90.4626	55588.7031365741	2011-01-27 16:52:31	55589.5557638889	2011-01-28 13:20:18	405007010	49.4612	50	49.4832	49.4752	0	49.4612	2	2	0	2	1	0	0	48.0185	48.0185	73.6599	0	PROCESSED	57600.7830092593	2016-07-31 18:47:32	55990	2012-03-04 00:00:00	55621.2282291667	2011-03-01 05:28:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050025	The all-sky survey in hard X-rays with INTEGRAL has been finding new magnetic Cataclysmic Variables. Among them, we propose Suzaku observations of five Intermediate Polars (IPs) which have no detailed follow-up spectroscopy in the hard X-ray band up to now. The wide-band energy coverage of Suzaku, therefore, is definitely useful to extract physical information from their spectra since, generally, the vFv spectrum of an IP peaks at E=20-50 keV and strong intrinsic absorption (nH=1E22-23 cm-2). By fitting the spectrum with our numerical model, we estimate a plasma temperature and an Fe abundance, and furthermore, a white dwarf mass which is one of the most basic and important parameter of a binary system.	GALACTIC POINT SOURCES	4	C	TAKAYUKI YUASA		JAP	5	AO5	ESTIMATE MASSES OF NEWLY-FOUND MAGNETIC WHITE DWARFS BASED ON HARD X-RAY CONTINUUM AND FE EMISSION LINES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405007010/	Quick Look
269	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
270	XSS J16537-1905	253.8855	-18.1447	253.157456	-18.065723	254.650655	4.44189	2.56699105	15.52634316	96.7569	55602.7046412037	2011-02-10 16:54:41	55603.1488657407	2011-02-11 03:34:22	405032010	20.0243	20	20.0323	20.0403	0	20.0243	2	2	0	2	1	0	0	18.1528	18.1528	38.3439	0	PROCESSED	57600.887337963	2016-07-31 21:17:46	55983	2012-02-26 00:00:00	55617.4104282407	2011-02-25 09:51:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050116	Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	5	AO5	QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405032010/	Quick Look
271	VW HYI	62.3086	-71.2914	62.399129	-71.420645	322.033067	-79.109175	284.88209314	-38.1323503	276.4367	55986.5687962963	2012-02-29 13:39:04	55987.2501273148	2012-03-01 06:00:11	406009030	20.1097	20	20.1097	20.1097	0	20.1097	2	2	0	2	1	0	0	20.5712	20.5712	58.8579	1	PROCESSED	57604.7590972222	2016-08-04 18:13:06	56385	2013-04-03 00:00:00	56018.9417824074	2012-04-01 22:36:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060023	SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate.	GALACTIC POINT SOURCES	4	B	KEI SAITOU		JAP	6	AO6-TOO	TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009030/	Quick Look
272	AQL X-1	287.8264	0.5741	287.188103	0.49034	289.387425	22.822835	35.71314195	-4.15661165	244.5268	55855.5357986111	2011-10-21 12:51:33	55856.4599884259	2011-10-22 11:02:23	406010020	9.9406	40	10.041	9.9406	0	10.041	1	1	0	1	1	0	0	37.8451	37.8451	79.846	1	PROCESSED	57603.5073958333	2016-08-03 12:10:39	56241	2012-11-10 00:00:00	55873.3025578704	2011-11-08 07:15:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060036	We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object.	GALACTIC POINT SOURCES	4	A	KAZUTAKA YAMAOKA		JAP	6	AO6-TOO	SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406010020/	Quick Look
273	4U0114+65	19.4873	65.3067	18.650038	65.043652	51.171478	51.093575	125.69846298	2.57745686	71.642	55763.4307291667	2011-07-21 10:20:15	55764.9453472222	2011-07-22 22:41:18	406017010	106.4925	100	106.5508	106.5588	0	106.4925	2	2	0	2	1	0	0	88.5061	88.5061	130.8219	1	PROCESSED	57602.6518402778	2016-08-02 15:38:39	56152	2012-08-13 00:00:00	55785.0443981482	2011-08-12 01:03:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060071	We propose to observe an X-ray pulsar, 4U 0114+65 for 100 ks. This object is known to be a neutron star binary with an orbital period of 12 days and a long pulse priod of 10 ks. Our goals are to obtain time-averaged spectra of the XIS and HXD, and to quantify spectral changes between flare and quiescense phases, and to search for a cyclotron absorption line around ~ 60 keV. We also study pulse-phase resolved spectra. With these pieces of information, we aim at clarifying whether this source is a magnetar descendent or a neutron star with ordinary magnetic fields.	GALACTIC POINT SOURCES	4	A	MAKOTO SASANO		JAP	6	AO6	SEARCH FOR HIGH MAGNETIC NEUTRON STARS IN HIGH-MASS X-RAY BINARIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406017010/	Quick Look
274	EUVE J1439 +75.0	219.9459	75.0823	219.98134	75.295606	130.308915	72.229429	114.11249059	40.13551871	340.4897	56067.2884722222	2012-05-20 06:55:24	56067.8599421296	2012-05-20 20:38:19	407039010	29.9613	40	29.9693	29.9693	0	29.9613	1	1	0	1	1	0	0	32.3932	32.3932	49.3439	0	PROCESSED	57605.4757523148	2016-08-05 11:25:05	56442	2013-05-30 00:00:00	56076.028912037	2012-05-29 00:41:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070112	The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects.	GALACTIC POINT SOURCES	4	B	ATSUSHI HARAYAMA		JAP	7	AO7	SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407039010/	Quick Look
275	CRAB PULSAR	83.6302	22.0185	82.877911	21.9858	84.096687	-1.291934	184.55261516	-5.78447613	87.4628	56551.703599537	2013-09-16 16:53:11	56552.187650463	2013-09-17 04:30:13	408008010	0.2483	20	0.2483	0.2483	0	0.2483	2	2	0	2	1	0	0	16.312	16.312	41.8179	1	PROCESSED	57612.6349421296	2016-08-12 15:14:19	56956	2014-10-26 00:00:00	56588.603599537	2013-10-23 14:29:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080026	We hereby submit a proposal for Suzaku/HXD observations of the Crab pulsar' hard X-ray pulses, which will be coordinated with simultaneous detection of giant radio pulses at ground radio telescopes. With these observations, we will get a statistically significant confirmation (or denial) of the existence of correlation between X-ray intensity and giant radio pulses, which has been found, with a marginal significance, during our trial observations of the Crab pulsar in which we utilized the calibration data of the HXD. If this correlation is confirmed, a new insight into the physics of pulsars' magnetospheres can be obtained.	GALACTIC POINT SOURCES	4	C	TOSHIO TERASAWA		JAP	8	AO8	CORRELATION STUDY OF X-RAY PULSES AND GIANT RADIO PULSES FROM CRAB PULSAR WITH SUZAKU/HXD	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408008010/	Quick Look
276	ETA CARINAE	161.2758	-59.6779	160.789133	-59.414544	202.149273	-58.913486	287.59865979	-0.62113788	295.3343	56479.0480439815	2013-07-06 01:09:11	56481.2890509259	2013-07-08 06:56:14	408018020	83.9685	180	83.9685	83.9685	0	83.9685	2	2	0	2	1	0	0	75.7786	75.7786	193.6058	3	PROCESSED	57611.7548263889	2016-08-11 18:06:57	56861	2014-07-23 00:00:00	56492.6867361111	2013-07-19 16:28:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080081	Eta Carinae is a binary system containing two very massive main sequence stars orbiting with a period of 5.5 years. As reported by Sekiguchi et al. 2009 and Reitberger et al. 2012 based on Suzaku and Fermi data respectively, the system shows intense non-thermal emission extending from 20 keV to 200 GeV. Although detailed mechanism of this non-thermal emission has been clarified yet, it is now obvious that electrons and highly probably protons are accelerated to high energies by the collision of stellar winds. The aim of the present observation is to measure the spectral shape and flux of the non-thermal hard X-ray tail with the HXD, and compare with previous Suzaku observations. Based on a time variability (or non-variability), we examine proposed acceleration and emission mechanisms.	GALACTIC POINT SOURCES	4	B	TAKAYUKI YUASA		JAP	8	AO8	DETAILED SPECTROSCOPY OF NON-THERMAL HARD X-RAY EMISSION OF ETA CARINAE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408018020/	Quick Look
277	1RXSJ174559.6-370055	266.4961	-37.0139	265.645982	-36.994815	267.112271	-13.607714	353.13065719	-4.26083799	95.2535	57115.2722106482	2015-04-03 06:31:59	57115.6653240741	2015-04-03 15:58:04	409017010	14.2473	15	14.2473	14.2473	0	14.2633	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.9002777778	2016-08-17 21:36:24	57493	2016-04-15 00:00:00	57126.4170949074	2015-04-14 10:00:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090051	We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	B	HIDEYUKI MORI		JAP	9	AO9	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409017010/	Quick Look
278	GK PER	52.7957	43.9123	51.943474	43.742358	61.502929	24.084705	150.94865814	-10.09942696	88.9617	56876.7092708333	2014-08-07 17:01:21	56879.871712963	2014-08-10 20:55:16	409018010	109.7612	140	109.7612	114.4242	0	114.4722	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.4851157407	2016-08-16 11:38:34	57468	2016-03-21 00:00:00	56902.7320023148	2014-09-02 17:34:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090055	A 140-ks observation of the magnetic cataclysmic variable GK Per is proposed. By fitting Suzaku broadband spectra using our multitemperature spectral model of the accretion column, we estimate a white dwarf mass with statistical fitting errors smaller than 5%. The estimated mass will be compared with one obtained from the optical lightcurve fitting method developed and applied by Hachisu and Kato in a series of papers. GK Per is the only known magnetic cataclysmic variable which underwent classical nova explosion (in 1901), and both the mass estimation methods can be applied. Cross-validated WD mass estimation methods will be of importance in studying massive white dwarfs in accretion systems, in relation with the progenitor of type Ia supernovae.	GALACTIC POINT SOURCES	4	A	TAKAYUKI YUASA		JAP	9	AO9	CROSS VALIDATION OF WHITE DWARF MASS ESTIMATION METHODS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409018010/	Quick Look
279	IC 443	94.2972	22.4797	93.541644	22.498727	93.972502	-0.901975	189.13057055	2.97563306	274.0001	54166.5158680556	2007-03-07 12:22:51	54167.612025463	2007-03-08 14:41:19	501006020	44.0135	40	44.0135	44.0375	0	44.0215	2	2	0	2	1	0	0	36.3209	36.3209	94.6999	1	PROCESSED	57537.6255324074	2016-05-29 15:00:46	54736	2008-09-27 00:00:00	54172.2247800926	2007-03-13 05:23:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010040	IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution.	GALACTIC DIFFUSE EMISSION	5	B	MASANOBU OZAKI		JAP	1	AO1	UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501006020/	Quick Look
280	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
281	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
282	SN1006 NE BG	226.7036	-41.3998	225.886024	-41.207391	236.037501	-22.925171	328.51405135	14.65073262	293.6503	53617.7018865741	2005-09-04 16:50:43	53622.1668287037	2005-09-09 04:00:14	100019010	44.7503	50	44.7543	44.7543	44.7543	44.7503	2	2	2	2	1	0	0	37.3883	37.3883	385.6018	5	PROCESSED	57527.2923148148	2016-05-19 07:00:56	54247	2007-05-27 00:00:00	54035.4224768518	2006-10-27 10:08:22	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000019		CALIBRATION	1	A	SWG		JAP	0	SWG	SN1006 observation with XIS and HXD		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019010/	Quick Look
283	VICINITY OF LMC X-3	83.4844	-63.8863	83.408578	-63.918105	41.435206	-86.187449	273.3865557	-32.64248934	284.6189	53811.6008333333	2006-03-17 14:25:12	53813.9168055556	2006-03-19 22:00:12	500031010	82.0185	80	82.0265	82.0185	82.0265	82.0265	2	2	2	2	1	0	0	74.6148	74.6148	200.0639	2	PROCESSED	57533.2849537037	2016-05-25 06:50:20	54247	2007-05-27 00:00:00	54056.4806828704	2006-11-17 11:32:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000043	We propose to observe the vicnity of LMC X-3 for 80 ks. We expectt to determine the OVII and OVIII emission line intensities within 20% errors. Combining these results with the OVII and OVIII absorption lines observed in the energy spectra of LMC X-3 with Chandra LETG-HRC, we can determine the geometrocal extent od the hot gas along the line-of-sight direction. This will answer the long-unanswered question; from where the high lattitude OVII/OVIII emissions come ?	GALACTIC DIFFUSE EMISSION	5	A	SWG		JAP	0	SWG	VICINITY OF LMC X-3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500031010/	Quick Look
284	IC 443	94.2975	22.7757	93.54026	22.794725	93.963954	-0.606095	188.8694635	3.11574616	274.0004	54165.4446643518	2007-03-06 10:40:19	54166.5154398148	2007-03-07 12:22:14	501006010	42.0113	40	42.0113	42.0129	0	42.0209	2	2	0	2	1	0	0	34.6934	34.6934	92.5099	2	PROCESSED	57537.6197337963	2016-05-29 14:52:25	54736	2008-09-27 00:00:00	54174.6613541667	2007-03-15 15:52:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010040	IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution.	GALACTIC DIFFUSE EMISSION	5	B	MASANOBU OZAKI		JAP	1	AO1	UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501006010/	Quick Look
285	CYGNUS_LOOP_P1	313.519	31.9657	313.004288	31.774919	328.788742	46.92673	75.41990185	-8.25713566	240	54417.6059259259	2007-11-13 14:32:32	54418.0904976852	2007-11-14 02:10:19	501012010	16.7385	10	16.7385	16.7489	0	16.7425	2	2	0	2	1	0	0	15.7758	15.7758	41.86	1	PROCESSED	57540.5110648148	2016-06-01 12:15:56	54798	2008-11-28 00:00:00	54430.2159375	2007-11-26 05:10:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501012010/	Quick Look
286	CYGNUS_LOOP_P4	312.8083	31.361	312.292075	31.17275	327.627486	46.612051	74.56035476	-8.16867105	239.9997	54418.9382291667	2007-11-14 22:31:03	54419.3196643518	2007-11-15 07:40:19	501015010	18.279	15	18.287	18.279	0	18.287	1	1	0	1	1	0	0	14.286	14.286	32.9439	0	PROCESSED	57540.5253935185	2016-06-01 12:36:34	54798	2008-11-28 00:00:00	54430.2398726852	2007-11-26 05:45:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501015010/	Quick Look
287	CYGNUS_LOOP_P5	312.5567	31.1701	312.040041	30.982753	327.230821	46.520779	74.2739834	-8.12038976	239.9995	54419.3201388889	2007-11-15 07:41:00	54420.0627777778	2007-11-16 01:30:24	501016010	28.4062	22	28.4062	28.4062	0	28.4062	2	2	0	2	1	0	0	25.37	25.37	64.1559	1	PROCESSED	57540.538900463	2016-06-01 12:56:01	54798	2008-11-28 00:00:00	54430.4318865741	2007-11-26 10:21:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501016010/	Quick Look
288	CYGNUS_LOOP_P6	312.3057	30.9823	311.788615	30.795857	326.837045	46.431585	73.99029438	-8.06939848	240.0003	54415.3923032407	2007-11-11 09:24:55	54416.1668287037	2007-11-12 04:00:14	501017010	28.7049	22	28.7049	28.7049	0	28.7049	1	1	0	1	1	0	0	26.8878	26.8878	66.9119	0	PROCESSED	57540.490474537	2016-06-01 11:46:17	54798	2008-11-28 00:00:00	54430.18875	2007-11-26 04:31:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501017010/	Quick Look
289	CYGNUS_LOOP_P16	312.737	30.4592	312.216541	30.271212	327.037451	45.805605	73.81069789	-8.68546284	61.9998	53877.1905439815	2006-05-22 04:34:23	53877.7605671296	2006-05-22 18:15:13	501033010	23.3375	22	23.3695	23.3375	23.3695	23.3695	2	2	2	2	1	0	0	20.1184	20.1184	49.2439	2	PROCESSED	57534.3873611111	2016-05-26 09:17:48	54398	2007-10-25 00:00:00	53926.8416319445	2006-07-10 20:11:57	3.0.22.43	6	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501033010/	Quick Look
290	GC_SGR_B_NORTH	266.6955	-28.3829	265.90467	-28.36493	267.072555	-4.975375	0.60514127	0.06995468	271.4417	54002.2105555556	2006-09-24 05:03:12	54003.2919444444	2006-09-25 07:00:24	501040020	44.8295	38	44.8455	44.8295	44.8375	44.8535	2	2	2	2	1	0	0	39.9705	39.9705	93.4319	1	PROCESSED	57535.678125	2016-05-27 16:16:30	54744	2008-10-05 00:00:00	54021.2868055556	2006-10-13 06:53:00	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010060	We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	1	AO1	OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501040020/	Quick Look
291	HESS J1614-518	243.5851	-51.743	242.630135	-51.617031	251.446035	-29.987821	331.574855	-0.5276897	283.402	53993.6672222222	2006-09-15 16:00:48	53994.4571064815	2006-09-16 10:58:14	501042010	40.1777	50	40.1857	40.1777	40.1857	40.1857	2	2	2	2	1	0	0	43.5607	43.5607	68.2279	0	PROCESSED	57535.5776967593	2016-05-27 13:51:53	54526	2008-03-01 00:00:00	54020.8545833333	2006-10-12 20:30:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010073	We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	1	AO1	SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501042010/	Quick Look
292	HESS J1614-518 BG	242.0174	-52.4329	241.059171	-52.300176	250.522759	-30.865237	330.3996927	-0.37656553	291.2192	53994.4597569444	2006-09-16 11:02:03	53995.3015509259	2006-09-17 07:14:14	501043010	43.5554	50	43.5634	43.5634	43.5554	43.5634	1	1	1	1	1	0	0	50.5922	50.5922	72.7039	1	PROCESSED	57535.5823726852	2016-05-27 13:58:37	54526	2008-03-01 00:00:00	54020.8662268518	2006-10-12 20:47:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010073	We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	1	AO1	SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501043010/	Quick Look
293	GALACTIC CENTER GC3	265.5781	-29.4684	264.780645	-29.444998	266.119721	-6.086772	359.1684549	0.33584661	108.8001	54170.7951273148	2007-03-11 19:04:59	54171.3397453704	2007-03-12 08:09:14	501048010	27.4546	25	27.4786	27.4546	0	27.4786	1	1	0	1	1	0	0	24.0548	24.0548	47.0479	1	PROCESSED	57537.6483333333	2016-05-29 15:33:36	54736	2008-09-27 00:00:00	54182.2788425926	2007-03-23 06:41:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501048010/	Quick Look
294	GALACTIC CENTER	265.9089	-29.649	265.11021	-29.627197	266.414403	-6.258746	359.16615355	-0.00387238	269	54017.0975115741	2006-10-09 02:20:25	54017.5690277778	2006-10-09 13:39:24	501050010	22.0477	20	22.0477	22.0477	22.0477	22.0477	1	1	1	1	1	0	0	18.6256	18.6256	40.7359	0	PROCESSED	57535.8013194445	2016-05-27 19:13:54	54735	2008-09-26 00:00:00	54053.4127777778	2006-11-14 09:54:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501050010/	Quick Look
295	GALACTIC CENTER	265.2994	-30.4982	264.495374	-30.473432	265.90984	-7.123709	358.16648703	-0.00302139	269.0003	54018.8881828704	2006-10-10 21:18:59	54019.4209953704	2006-10-11 10:06:14	501053010	21.9086	20	21.9086	21.9321	21.9166	21.9166	1	1	1	1	1	0	0	19.948	19.948	46.0319	0	PROCESSED	57535.8190393518	2016-05-27 19:39:25	54735	2008-09-26 00:00:00	54053.5019675926	2006-11-14 12:02:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501053010/	Quick Look
296	GC SGR D EAST	267.2856	-27.6502	266.49923	-27.635104	267.579665	-4.231943	1.50163715	0.00269695	108.7997	54176.2132407407	2007-03-17 05:07:04	54177.8737731482	2007-03-18 20:58:14	501060010	64.7953	63	64.7953	64.8267	0	64.8113	2	2	0	2	1	0	0	54.6297	54.6297	143.4659	1	PROCESSED	57537.7151851852	2016-05-29 17:09:52	54736	2008-09-27 00:00:00	54185.4429050926	2007-03-26 10:37:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501060010/	Quick Look
297	RXJ1713-3946	258.5524	-39.4291	257.687827	-39.37177	260.79719	-16.352329	347.6770378	-0.38034705	267.9999	53997.5713773148	2006-09-19 13:42:47	53997.9140509259	2006-09-19 21:56:14	501069010	18.375	20	18.375	18.375	18.375	18.375	1	1	1	1	1	0	0	14.2767	14.2767	29.5999	0	PROCESSED	57535.6332060185	2016-05-27 15:11:49	54526	2008-03-01 00:00:00	54021.1502546296	2006-10-13 03:36:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501069010/	Quick Look
298	RXJ1713-3946	258.9408	-39.7267	258.073523	-39.671212	261.133474	-16.624716	347.60984156	-0.7970823	268.0009	54013.3138541667	2006-10-05 07:31:57	54013.877974537	2006-10-05 21:04:17	501072010	19.9817	20	19.9817	19.9817	19.9817	19.9817	2	2	2	2	1	0	0	16.2997	16.2997	48.718	1	PROCESSED	57535.7676736111	2016-05-27 18:25:27	54526	2008-03-01 00:00:00	54021.6599652778	2006-10-13 15:50:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501072010/	Quick Look
299	U SCO	245.6292	-17.8133	244.907482	-17.696814	246.808074	3.687304	357.72295453	21.91020567	93.2753	55239.299224537	2010-02-12 07:10:53	55239.8259027778	2010-02-12 19:49:18	404018030	26.826	20	26.826	26.826	0	26.826	1	1	0	1	1	0	0	24.9037	24.9037	45.472	1	PROCESSED	57550.5610763889	2016-06-11 13:27:57	55619	2011-02-27 00:00:00	55253.1155671296	2010-02-26 02:46:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040057	We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each.	GALACTIC POINT SOURCES	4	A	DAI TAKEI		JAP	4	AO4-TOO	TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404018030/	Quick Look
300	GC18	266.183	-28.6222	265.39077	-28.601742	266.626489	-5.225763	0.16630142	0.32982124	260.5302	54384.4819560185	2007-10-11 11:34:01	54384.9633564815	2007-10-11 23:07:14	502006010	22.6311	20	22.6311	22.6413	0	22.6351	2	2	0	2	1	0	0	21.6702	21.6702	41.5841	1	PROCESSED	57540.2503356482	2016-06-01 06:00:29	54771	2008-11-01 00:00:00	54402.6632291667	2007-10-29 15:55:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502006010/	Quick Look
301	GC21	267.484	-27.3686	266.699338	-27.354471	267.750913	-3.947195	1.83363899	-0.00346152	261.5433	54385.9113888889	2007-10-12 21:52:24	54386.3127199074	2007-10-13 07:30:19	502009010	20.8615	20	20.8615	20.8615	0	20.8615	2	2	0	2	1	0	0	19.6483	19.6483	34.6639	1	PROCESSED	57540.2599189815	2016-06-01 06:14:17	54771	2008-11-01 00:00:00	54402.5769444444	2007-10-29 13:50:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502009010/	Quick Look
302	GC22	266.3806	-28.337	265.590118	-28.317504	266.793387	-4.936169	0.50023196	0.3305092	262.5049	54386.3138888889	2007-10-13 07:32:00	54386.785	2007-10-13 18:50:24	502010010	21.6214	20	21.6214	21.6214	0	21.6214	2	2	0	2	1	0	0	21.1944	21.1944	40.662	1	PROCESSED	57540.2655439815	2016-06-01 06:22:23	54771	2008-11-01 00:00:00	54402.6900231482	2007-10-29 16:33:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502010010/	Quick Look
303	HESS J1745-303 3	266.0567	-30.2413	265.254155	-30.220204	266.559978	-6.847208	358.72882707	-0.42335991	69.0003	54533.6682523148	2008-03-08 16:02:17	54535.8752199074	2008-03-10 21:00:19	502018010	79.0162	67	79.0162	79.0402	0	79.0242	2	2	0	2	1	0	0	70.201	70.201	190.658	2	PROCESSED	57541.8566898148	2016-06-02 20:33:38	54919	2009-03-29 00:00:00	54550.3420601852	2008-03-25 08:12:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020023	A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku.	GALACTIC DIFFUSE EMISSION	5	B	RYO YAMAZAKI		JAP	2	AO2	SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502018010/	Quick Look
304	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
305	VELA JR P7	133.7759	-45.5828	133.340558	-45.390922	159.660843	-58.904253	266.02998701	-0.32446592	347.0033	54286.9870023148	2007-07-05 23:41:17	54287.3023032407	2007-07-06 07:15:19	502029010	14.5838	10	14.5838	14.5838	0	14.5838	2	2	0	2	1	0	0	12.605	12.605	27.2399	0	PROCESSED	57539.1100810185	2016-05-31 02:38:31	54696	2008-08-18 00:00:00	54328.4686111111	2007-08-16 11:14:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502029010/	Quick Look
306	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
307	XB1323-619	201.6454	-62.1418	200.814994	-61.88221	229.562797	-47.947963	307.02498182	0.45033402	99.5731	54109.4794907407	2007-01-09 11:30:28	54110.9168402778	2007-01-10 22:00:15	401002010	55.9368	50	55.9368	55.9368	0	55.9368	2	2	0	2	1	0	0	81.8173	81.8173	124.1769	1	PROCESSED	57536.8666087963	2016-05-28 20:47:55	54735	2008-09-26 00:00:00	54133.0271759259	2007-02-02 00:39:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010002	XB 1323-619 is a non-transient dipping LMXB and one of the few LMXB with spectrum extending to high energies. Our XMM-Newton observation revealed many lines including Fe XXV and XXVI absorption. Uniquely, the rate of bursting has increased systematically over 18 years by 15 times to every 20 min in 2006/07 making it the best source for study of absorption in bursts. Suzaku allows measurement of ADC temperature via the high energy cut-off and can give the first detection of cooling by soft photons from the neutron star from the change of cut-off energy during bursts. Curve-of-growth analysis gives the absorber temperature and tests our suggestion that absorption lines are formed in the ADC. Detailed comparison with burst theory is possible because of the regular bursting.	GALACTIC POINT SOURCES	4	C	TADAYASU DOTANI		JAP	1	AO1	BORADBAND INVESTIGATIONS OF THE DIPPING, BURSTGING LOW MASS X-RAY BINARY XB1323-619	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401002010/	Quick Look
308	VELA JR P10	132.9993	-45.7656	132.567919	-45.576468	158.955645	-59.347984	265.8217159	-0.85784968	347.0018	54287.9522337963	2007-07-06 22:51:13	54288.2308564815	2007-07-07 05:32:26	502032010	13.04	10	13.048	13.04	0	13.056	2	2	0	2	1	0	0	10.6988	10.6988	24.0679	0	PROCESSED	57539.1146527778	2016-05-31 02:45:06	54703	2008-08-25 00:00:00	54333.4328240741	2007-08-21 10:23:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502032010/	Quick Look
309	VELA JR P14	131.9312	-46.3861	131.508056	-46.200795	158.369308	-60.268301	265.83284327	-1.824218	347.0017	54290.4416087963	2007-07-09 10:35:55	54290.675150463	2007-07-09 16:12:13	502036010	11.034	10	11.034	11.042	0	11.042	1	1	0	1	1	0	0	11.1391	11.1391	20.1679	0	PROCESSED	57539.1311226852	2016-05-31 03:08:49	54696	2008-08-18 00:00:00	54328.4740277778	2007-08-16 11:22:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502036010/	Quick Look
310	VELA JR P15	132.3334	-46.3288	131.908455	-46.142044	158.77835	-60.071	265.96324441	-1.57253381	347.0016	54291.1946064815	2007-07-10 04:40:14	54291.46	2007-07-10 11:02:24	502037010	8.876	10	8.876	8.876	0	8.876	2	2	0	2	1	0	0	7.3411	7.3411	22.9121	1	PROCESSED	57539.1396990741	2016-05-31 03:21:10	54696	2008-08-18 00:00:00	54328.472962963	2007-08-16 11:21:04	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502037010/	Quick Look
311	47 TUCANAE	6.2112	-71.9961	5.659821	-72.273106	311.457534	-62.358991	305.8317488	-44.9821189	65.5967	54261.1765162037	2007-06-10 04:14:11	54263.5404976852	2007-06-12 12:58:19	502048010	132.1052	133	132.1452	132.1052	0	132.1372	2	2	0	2	1	0	0	132.9042	132.9042	204.2319	1	PROCESSED	57538.9491666667	2016-05-30 22:46:48	54745	2008-10-06 00:00:00	54271.5258796296	2007-06-20 12:37:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020066	We propose a 100 ks observation of the globular cluster 47 Tuc. An extended (~2') hard x-ray emission, presumably of non-thermal origin, was detected with Chandra from a position ~6' toward north east of its center. However, the Chandra ACIS spectrum does not allow us to determine with confidence whether it is a non-thermal emission or a high temperature thermal source. Utilizing the high sensitivity of the XIS, we try to distinguish between these two cases. If confirmed, the result may provide valuable information on particle acceleration in non-relativistic shocks, with potential relations the galactic-ridge x-ray emission. We perform a single pointing observation placing the center of the diffuse emission onto XIS nominal position.	GALACTIC DIFFUSE EMISSION	5	B	TAKAYUKI YUASA		JAP	2	AO2	OBSERVATIONAL INVESTIGATION OF PARTICLE ACCELERATION IN A GLOBULAR CLUSTER SHOCK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502048010/	Quick Look
312	M17 EAST BKG	275.6441	-15.5803	274.925967	-15.60595	275.476675	7.75309	15.81995827	-0.84785909	271.9998	54380.0947800926	2007-10-07 02:16:29	54381.7571064815	2007-10-08 18:10:14	502053010	71.494	67	71.494	71.5085	0	71.502	2	2	0	2	1	0	0	62.5549	62.5549	143.61	1	PROCESSED	57540.2032175926	2016-06-01 04:52:38	54771	2008-11-01 00:00:00	54403.2344791667	2007-10-30 05:37:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020085	We continue our XIS study of the soft extended X-ray emission in M17. The first study conducted in a region close to the OB association brought a detailed surface brightness distribution and the highest S/N ratio spectrum of the diffuse emission. In this proposed study, we move our eyes to the west to observe another bright emission outside of the previously studied regions. DSS and ROSAT all-sky survey images suggest that this is a shocked region, in which OB stellar winds impinge upon ISM. We aim to obtain the surface brightness map of this region and measure the plasma temperature difference in and out of the possible shocked region.	GALACTIC DIFFUSE EMISSION	5	A	MASAHIRO TSUJIMOTO		JAP	2	AO2	FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS -	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502053010/	Quick Look
313	GALACTIC BULGE	268.3774	-29.9651	267.576244	-29.955267	268.575567	-6.53206	359.99980668	-2.0020922	279.4328	54372.0700347222	2007-09-29 01:40:51	54375.590462963	2007-10-02 14:10:16	502059010	136.824	133	136.824	136.824	0	136.824	2	2	0	2	1	0	0	110.5156	110.5156	304.1306	2	PROCESSED	57540.2260185185	2016-06-01 05:25:28	54770	2008-10-31 00:00:00	54402.653275463	2007-10-29 15:40:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020118	We propose a 100 ks observation on the Galactic Bulge (b=-2.0) with Suzaku. The origin of thermal diffuse X-ray emission will be for the first time clarified with a fine spectroscopy with Suzaku XIS, especially from the Fe-K line analysis. The non-thermal emission from the Galactic Bulge will be also investigated with HXD-PIN.	GALACTIC DIFFUSE EMISSION	5	A	MOTOHIDE KOKUBUN		JAP	2	AO2	INVESTIGATION ON THE GALACTIC BULGE DIFFUSE X-RAY EMISSION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502059010/	Quick Look
314	HD45314	96.8131	14.89	96.098891	14.921299	96.656857	-8.393671	196.95740391	1.52274638	93.5296	56935.6339814815	2014-10-05 15:12:56	56937.7981134259	2014-10-07 19:09:17	409019010	82.0799	80	82.0879	82.0879	0	82.0799	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6300115741	2016-08-16 15:07:13	57355	2015-11-29 00:00:00	56989.5080208333	2014-11-28 12:11:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090079	We propose a Suzaku observation of a newly-found Gamma Cas analogue HD45314. The Gamma Cas analogues constitute a small but distinctive group showing anomalously hard X-ray spectra. We propose a Suzaku observation of HD45314 and compare it with the XMM data taken previously (Rauw et al. 2013) to reveal an expected change in the X-ray spectra. This will give us a clue to understand the X-ray production mechanism of this source and the gamma Cas analogues.	GALACTIC POINT SOURCES	4	B	MASAHIRO TSUJIMOTO		JAP	9	AO9	INVESTIGATION OF A GAMMA CAS ANALOGUES USING SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409019010/	Quick Look
315	Crab Nebula	83.6622	21.1838	82.914561	21.151265	84.089646	-2.127158	185.27784655	-6.20565133	88.1125	53628.0468055556	2005-09-15 01:07:24	53628.2988194444	2005-09-15 07:10:18	100022010	12.881	10	12.881	12.881	12.881	12.881	1	1	1	1	1	0	0	12.241	12.241	21.7679	0	PROCESSED	57527.323275463	2016-05-19 07:45:31	54247	2007-05-27 00:00:00	54109.2599768518	2007-01-09 06:14:22	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000022	Crab at 50arcmin off from the XIS aimpoint to study stray light.	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab at 50 arcmin off		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100022010/	Quick Look
316	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
317	ANTICENTER2	12.9862	62.9112	12.227424	62.639587	45.279185	50.910305	122.98962226	0.03950805	69.9598	54679.0120717593	2008-08-01 00:17:23	54680.8411921296	2008-08-02 20:11:19	503006010	86.1101	80	86.123	86.123	0	86.1101	2	2	0	2	1	0	0	106.785	106.785	158.0198	1	PROCESSED	57543.2173726852	2016-06-04 05:13:01	55070	2009-08-27 00:00:00	54693.3237847222	2008-08-15 07:46:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030020	We propose to observe diffuse radiation from the Galactic plane in the general direction of the anticenter. The ROSAT 3/4 keV band all sky map does not show significant dip in intensity at galactic plane, where the CXB component is totally absorbed by galactic absorption. Thus unknown emission must be compensating the CXB component in this energy band. Our AO-2 observation of a general direction of the anticenter direction gives a clear clue to understand the origin of the mysterious emission. We propose to make additional observation in order to confirm the emission component detected in the AO-2 observation generally exist in the galactic plane.	GALACTIC DIFFUSE EMISSION	5	B	KENSUKE MASUI		JAP	3	AO3	SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503006010/	Quick Look
318	GC_LARGEPROJECT2	266.7785	-29.1292	265.982946	-29.111621	267.162656	-5.719811	0.00479668	-0.37932142	260.8763	54712.9538078704	2008-09-03 22:53:29	54714.2891087963	2008-09-05 06:56:19	503008010	53.6388	50	53.6548	53.6388	0	53.6548	2	2	0	2	1	0	0	42.8111	42.8111	115.3338	0	PROCESSED	57543.7762615741	2016-06-04 18:37:49	54557	2008-04-01 00:00:00	54780.4880092593	2008-11-10 11:42:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503008010/	Quick Look
319	GC_LARGEPROJECT3	266.4525	-29.3384	265.655678	-29.319237	266.881748	-5.935661	359.67825031	-0.24492188	260.8779	54714.2896759259	2008-09-05 06:57:08	54715.6634722222	2008-09-06 15:55:24	503009010	52.3975	50	52.4055	52.3975	0	52.4114	2	2	0	2	1	0	0	40.2691	40.2691	118.6778	2	PROCESSED	57543.769375	2016-06-04 18:27:54	54557	2008-04-01 00:00:00	54780.6767476852	2008-11-10 16:14:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503009010/	Quick Look
320	GC_LARGEPROJECT5	265.9469	-29.8331	265.147019	-29.811478	266.45285	-6.44183	359.02671432	-0.12852462	265.43	54717.3806597222	2008-09-08 09:08:09	54718.8981365741	2008-09-09 21:33:19	503011010	57.6334	50	57.6334	57.6334	0	57.6334	2	2	0	2	1	0	0	40.1555	40.1555	131.0998	1	PROCESSED	57543.8408449074	2016-06-04 20:10:49	54557	2008-04-01 00:00:00	54780.6683912037	2008-11-10 16:02:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503011010/	Quick Look
321	GC_LARGEPROJECT9	265.0297	-30.9626	264.222709	-30.936519	265.692051	-7.595667	357.64981902	-0.05267713	269.1132	54728.3146412037	2008-09-19 07:33:05	54729.4140393518	2008-09-20 09:56:13	503015010	56.7716	50	56.7796	56.7716	0	56.7876	2	2	0	2	1	0	0	52.8454	52.8454	94.9759	0	PROCESSED	57543.8851041667	2016-06-04 21:14:33	54557	2008-04-01 00:00:00	54780.4933564815	2008-11-10 11:50:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503015010/	Quick Look
322	GC_LARGEPROJECT12	264.5606	-31.5967	263.749555	-31.56834	265.310874	-8.24393	356.89961278	-0.05143068	268.4538	54742.7536226852	2008-10-03 18:05:13	54743.154375	2008-10-04 03:42:18	503018020	12.2466	10	12.2466	12.2466	0	12.2466	2	2	0	2	1	0	0	10.232	10.232	34.6179	1	PROCESSED	57544.0096527778	2016-06-05 00:13:54	54557	2008-04-01 00:00:00	54780.5624652778	2008-11-10 13:29:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503018020/	Quick Look
323	HESS J1825-137	276.5024	-13.9965	275.79256	-14.02632	276.383198	9.300131	17.60816681	-0.84042551	271.0002	54754.9096064815	2008-10-15 21:49:50	54756.458599537	2008-10-17 11:00:23	503028010	57.2104	50	57.2104	57.2104	0	57.2104	2	2	0	2	1	0	0	51.5485	51.5485	133.7938	1	PROCESSED	57544.1955324074	2016-06-05 04:41:34	55148	2009-11-13 00:00:00	54780.7053703704	2008-11-10 16:55:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030044	The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons.	GALACTIC DIFFUSE EMISSION	5	B	TAKAAKI TANAKA		JAP	3	AO3	MAPPING OBSERVATIONS OF HESS J1825-137	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503028010/	Quick Look
324	VELA JR P24	132.0303	-46.6729	131.609003	-46.487232	158.79782	-60.473277	266.0989339	-1.95139979	347.001	54652.7719328704	2008-07-05 18:31:35	54653.1668865741	2008-07-06 04:00:19	503036010	12.3735	10	12.3735	12.3735	0	12.3735	2	2	0	2	1	0	0	12.2548	12.2548	34.12	1	PROCESSED	57542.9791203704	2016-06-03 23:29:56	55048	2009-08-05 00:00:00	54679.3185763889	2008-08-01 07:38:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503036010/	Quick Look
325	VELA JR P28	133.7109	-46.6037	133.283226	-46.412037	160.667114	-59.788002	266.78076878	-1.01777641	347.0004	54654.1674537037	2008-07-07 04:01:08	54654.4259143518	2008-07-07 10:13:19	503040010	13.093	10	13.101	13.093	0	13.101	1	1	0	1	1	0	0	12.054	12.054	22.296	0	PROCESSED	57542.9904282407	2016-06-03 23:46:13	55048	2009-08-05 00:00:00	54679.3674421296	2008-08-01 08:49:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503040010/	Quick Look
326	VELA JR P29	134.0711	-46.43	133.640871	-46.237075	160.890422	-59.507166	266.80859879	-0.71638658	347	54654.4264814815	2008-07-07 10:14:08	54654.7203703704	2008-07-07 17:17:20	503041010	11.3685	10	11.3802	11.3685	0	11.3802	1	1	0	1	1	0	0	8.2225	8.2225	25.3679	0	PROCESSED	57542.9909606482	2016-06-03 23:46:59	55048	2009-08-05 00:00:00	54679.3958217593	2008-08-01 09:29:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503041010/	Quick Look
327	VELA JR P38	132.2003	-47.2308	131.782721	-47.04451	159.617188	-60.877835	266.60579829	-2.21244802	347.0003	54657.2423958333	2008-07-10 05:49:03	54657.5209953704	2008-07-10 12:30:14	503050010	14.0436	10	14.0436	14.0436	0	14.0596	1	1	0	1	1	0	0	11.426	11.426	24.0639	0	PROCESSED	57543.0197800926	2016-06-04 00:28:29	55037	2009-07-25 00:00:00	54670.2561111111	2008-07-23 06:08:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503050010/	Quick Look
328	RCW 38	134.7638	-47.5154	134.339139	-47.320051	162.870038	-60.148721	267.93999829	-1.06526988	109.8553	54788.5064351852	2008-11-18 12:09:16	54790.699525463	2008-11-20 16:47:19	503054010	81.5377	80	81.5495	81.5377	0	81.5415	2	2	0	2	1	0	0	60.9281	60.9281	189.4597	1	PROCESSED	57544.5092013889	2016-06-05 12:13:15	55171	2009-12-06 00:00:00	54811.741099537	2008-12-11 17:47:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030069	We propose to make Suzaku observation of HII region RCW 38 for 80 ksec in order to study non-thermal phenomena in a massive star-forming region. The region is thought to be a site of high energy particle acceleration by interaction of strong stellar wind from high-mass stars. The main purpose is to observe extended emission from RCW 38. The high resolution spectroscopy by XIS enables us to distinguish non-thermal emission from thermal component and to obtain properties of non-thermal component. In addition, HXD will detect non-thermal radiation from RCW 38.	GALACTIC DIFFUSE EMISSION	5	C	HIROKAZU ODAKA		JAP	3	AO3	SEARCH FOR NONTHERMAL RADIATION FROM MASSIVE STAR-FORMING REGION RCW 38	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503054010/	Quick Look
329	CYGNUS LOOP (P21)	313.196	32.4197	312.684204	32.23006	328.688835	47.452326	75.60030214	-7.75821821	61.9243	54619.9401967593	2008-06-02 22:33:53	54620.2975	2008-06-03 07:08:24	503057010	16.1703	15	16.1783	16.1703	0	16.1783	1	1	0	1	1	0	0	12.8903	12.8903	30.8639	0	PROCESSED	57542.700474537	2016-06-03 16:48:41	55003	2009-06-21 00:00:00	54636.2238078704	2008-06-19 05:22:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503057010/	Quick Look
330	RABBIT	214.6544	-60.9713	213.733054	-60.740946	236.398817	-43.82174	313.31134091	0.131367	105.7763	54876.850787037	2009-02-14 20:25:08	54877.5224421296	2009-02-15 12:32:19	503071010	21.274	20	21.282	21.274	0	21.29	1	1	0	1	1	0	0	18.0126	18.0126	57.984	0	PROCESSED	57545.5405439815	2016-06-06 12:58:23	55330	2010-05-14 00:00:00	54892.945162037	2009-03-02 22:41:02	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030076	K3/PSR J1420-6048 is one of the TeV gamma-ray pulsar wind nebulae detected by HESS, which are thought to be main particle accelerators to the Galactic Cosmic rays. It was also detected by EGRET and its X-ray spectrum is very hard. In order to reveal the radiation mechanism, we propose to observe the extended source for 50 ksec on HXD nominal position and contamination source for 20 ksec on XIS nominal position. The main purpose of this observation is to obtain the hard X-ray spectrum up to about 40 keV.	GALACTIC DIFFUSE EMISSION	5	C	TETSUICHI KISHISHITA		JAP	3	AO3	SUZAKU OBSERVATION OF TEV GAMMA-RAY PWN K3/PSR J1420-6048	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503071010/	Quick Look
331	HESS_J1809-193_N	272.4044	-19.3551	271.665869	-19.36499	272.264534	4.066746	11.02929838	0.07166066	112.001	54556.5874421296	2008-03-31 14:05:55	54557.6877662037	2008-04-01 16:30:23	503078010	51.5309	40	51.5389	51.5309	0	51.5461	2	2	0	2	1	0	0	34.8186	34.8186	95.0518	2	PROCESSED	57542.0290740741	2016-06-03 00:41:52	54950	2009-04-29 00:00:00	54571.3638888889	2008-04-15 08:44:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030126	A survey of the Galactic plane with H.E.S.S. has revealed the existance of several new very-high-energy (VHE) gamma-ray sources. As gamma rays are produced by interactions of relativistic particles, observing VHE emission reveals the acceleration sites of particles. Although it had been thought that such acceleration occur in the shock of SNR, it became clear that several VHE sources are pulsar wind nebulae (PWNe). This indicates that PWNe are also the acceleration sites of particles. HESS J1809-193 is a diffuse and a pulsar wind nebula candidate source, but details of the VHE emission mechanisms have been unclear yet. With the high sensitivity of XIS, we investigate spatial distribution of the spectrum around HESS J1809-193 and reveal its nature and the VHE emission mechanism.	GALACTIC DIFFUSE EMISSION	5	A	TAKAYASU ANADA		JAP	3	AO3	INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503078010/	Quick Look
332	VICINITY_OF_PKS_2155-1	329.2367	-30.5281	328.510685	-30.766467	320.669664	-16.905257	17.16872193	-51.86657338	55.8337	54585.7726736111	2008-04-29 18:32:39	54588.3542592593	2008-05-02 08:30:08	503082010	90.1812	80	90.1812	90.1812	0	90.1812	2	2	0	2	1	0	0	76.7921	76.7921	223.0237	4	PROCESSED	57542.4840277778	2016-06-03 11:37:00	54975	2009-05-24 00:00:00	54608.3373726852	2008-05-22 08:05:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030135	The highly ionized absorption lines of OVII, OVIII, and NeIX at z = 0 have been unambiguously detected toward the bright AGN PKS 2155-304 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII, OVIII and NeIX emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas.	GALACTIC DIFFUSE EMISSION	5	A	TOSHISHIGE HAGIHARA		JAP	3	AO3	STUDY OF WARM-HOT GAS TOWARD PKS 2155-304	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503082010/	Quick Look
333	SGR_B2	266.8788	-28.4436	266.087557	-28.426518	267.23571	-5.032452	0.63679	-0.09938091	266.4718	55096.836412037	2009-09-22 20:04:26	55102.6667592593	2009-09-28 16:00:08	504004020	202.0945	200	202.0945	202.1025	0	202.0945	3	4	0	3	1	0	0	178.2831	178.2831	303.5437	4	PROCESSED	57548.82125	2016-06-09 19:42:36	55500	2010-10-31 00:00:00	55133.4505092593	2009-10-29 10:48:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040002	The Galactic center diffuse X-ray emission (GCDX) consists of the hot plasma, neutral iron line, and hard tail. While we have demonstrated the hot plasma truly extending, origins of the others are still under discussion. We found time variability of the neutral Fe line intensity and marginally detected neutral lines of S, Ar, and Ca from Sagittarius B2. Our purpose is to clearly detect the neutral lines of S, Ar, Ca, and time variability of the hard tail of the GCDX up to 40 keV. This observation will resolve the remaining mysteries of the GCDX.	GALACTIC DIFFUSE EMISSION	5	A	MASAYOSHI NOBUKAWA		JAP	4	AO4	SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION-	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504004020/	Quick Look
334	BLOWOUT1	312.2225	31.7347	311.709294	31.548551	327.170903	47.151978	74.53998499	-7.54540267	244.0864	55158.2754166667	2009-11-23 06:36:36	55158.9655555556	2009-11-23 23:10:24	504011010	24.1854	23	24.2014	24.1854	0	24.1934	2	2	0	2	1	0	0	19.4768	19.4768	59.6039	1	PROCESSED	57549.5243055556	2016-06-10 12:35:00	55545	2010-12-15 00:00:00	55176.2112731482	2009-12-11 05:04:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504011010/	Quick Look
335	BLOWOUT3	311.7021	31.3134	311.187829	31.12914	326.330215	46.937186	73.92913651	-7.4588166	242.4356	55160.1363888889	2009-11-25 03:16:24	55160.4723611111	2009-11-25 11:20:12	504013010	16.1599	16	16.1599	16.1599	0	16.1599	2	2	0	2	1	0	0	11.8101	11.8101	29.0219	0	PROCESSED	57549.5443634259	2016-06-10 13:03:53	55545	2010-12-15 00:00:00	55176.2365740741	2009-12-11 05:40:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504013010/	Quick Look
336	FESI1	313.4345	30.6099	312.913405	30.419428	327.914732	45.71047	74.31119672	-9.05841998	226.3696	55182.5546180556	2009-12-17 13:18:39	55183.3334837963	2009-12-18 08:00:13	504017010	32.2876	24	32.2876	32.2876	0	32.2876	2	2	0	2	1	0	0	27.2129	27.2129	67.2859	0	PROCESSED	57549.881099537	2016-06-10 21:08:47	55575	2011-01-14 00:00:00	55204.4679976852	2010-01-08 11:13:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040007	The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	4	AO4	OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504017010/	Quick Look
337	HESS J1731-347 N	262.8483	-34.6425	262.016963	-34.605825	263.993904	-11.350062	353.56257635	-0.49517094	91.6366	55244.8937037037	2010-02-17 21:26:56	55245.7189699074	2010-02-18 17:15:19	504032010	41.5263	40	41.5263	41.5263	0	41.5263	2	2	0	2	1	0	0	32.8653	32.8653	71.2719	0	PROCESSED	57550.6405555556	2016-06-11 15:22:24	55623	2011-03-03 00:00:00	55257.0108449074	2010-03-02 00:15:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040026	Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1731-347 is one of only 3 TeV SNRs which have a radio shell and possible thermal X-rays. With good statistics and low background observation of Suzaku XIS, we will detect thermal X-rays from the shell of HESS J1731-347 for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition.	GALACTIC DIFFUSE EMISSION	5	B	AYA BAMBA		JAP	4	AO4	DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504032010/	Quick Look
338	GALACTICDISC3-1	15.309	67.9759	14.492554	67.706941	51.801719	54.210388	123.85392042	5.12169353	244.2747	55214.8348148148	2010-01-18 20:02:08	55216.0225	2010-01-20 00:32:24	504038010	55.2279	50	55.2279	55.2279	0	55.2279	2	2	0	2	1	0	0	43.3329	43.3329	102.5998	2	PROCESSED	57550.2600231482	2016-06-11 06:14:26	55594	2011-02-02 00:00:00	55228.2005092593	2010-02-01 04:48:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040097	To elucidate the vertical structure of the yet-not-understood excess soft X-ray emission from the galactic disk, we propose to observe two offset directions from the plane along l = 123 degree. We expect the spectra contains the 0.75 keV emission component which we discovered in the energy spectra of two midplane observations. The proposed observations will strongly constrain the nature of the sources which are responsible for the excess emission, in particular the vertical distribution in the Galaxy.	GALACTIC DIFFUSE EMISSION	5	C	SHUNSUKE KIMURA		JAP	4	AO4	STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504038010/	Quick Look
339	ASO0505	339.5988	59.0734	339.120995	58.812928	20.160721	59.131044	106.55945745	0.49758229	62.7751	55001.185775463	2009-06-19 04:27:31	55001.7494675926	2009-06-19 17:59:14	504048010	26.3616	20	26.3696	26.3616	0	26.3776	2	2	0	2	1	0	0	23.8416	23.8416	48.6959	1	PROCESSED	57547.5983449074	2016-06-08 14:21:37	55381	2010-07-04 00:00:00	55015.2523148148	2009-07-03 06:03:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040101	Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.	GALACTIC DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504048010/	Quick Look
340	ASO0418	279.775	-5.7085	279.106672	-5.754175	280.186655	17.387028	26.44714681	0.13153934	86.843	54934.6472800926	2009-04-13 15:32:05	54935.7578587963	2009-04-14 18:11:19	504052010	41.0684	40	41.0802	41.0844	0	41.0684	2	2	0	2	1	0	0	33.5258	33.5258	95.9378	0	PROCESSED	57546.1671296296	2016-06-07 04:00:40	55324	2010-05-08 00:00:00	54949.5662268518	2009-04-28 13:35:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040112	We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504052010/	Quick Look
341	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
342	ASO0215	154.6836	-58.9426	154.241353	-58.691332	196.521873	-60.887637	284.32918046	-1.70077172	314.5017	55019.3141782407	2009-07-07 07:32:25	55020.3404976852	2009-07-08 08:10:19	504053010	40.0868	40	40.0868	40.0868	0	40.0868	2	2	0	2	1	0	0	35.4782	35.4782	88.6598	0	PROCESSED	57547.8126851852	2016-06-08 19:30:16	55399	2010-07-22 00:00:00	55029.2468055556	2009-07-17 05:55:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040112	We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504053010/	Quick Look
343	ASO0319	224.8822	-60.8823	223.89321	-60.683278	242.498215	-41.674426	317.89227503	-1.78687667	277.7774	55049.7078125	2009-08-06 16:59:15	55051.0238425926	2009-08-08 00:34:20	504055010	42.3613	40	42.3613	42.3668	0	42.3773	2	2	0	2	1	0	0	37.5233	37.5233	113.6859	0	PROCESSED	57548.1027083333	2016-06-09 02:27:54	55430	2010-08-22 00:00:00	55062.2941782407	2009-08-19 07:03:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040112	We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy.	GALACTIC DIFFUSE EMISSION	5	A	NOBUYUKI KAWAI		JAP	4	AO4	UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504055010/	Quick Look
344	3C_391	282.3812	-0.9417	281.735823	-0.99987	283.351934	21.926784	31.87573789	-0.00377867	261.9952	55491.0759722222	2010-10-22 01:49:24	55493.8224537037	2010-10-24 19:44:20	505007010	99.3887	100	99.4607	99.3887	0	99.4687	2	2	0	2	1	0	0	89.374	89.374	237.2779	2	PROCESSED	57553.8698032407	2016-06-14 20:52:31	55287	2010-04-01 00:00:00	55502.3356597222	2010-11-02 08:03:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050002	We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	5	AO5	RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505007010/	Quick Look
345	CYGNUS LOOP 1	313.2462	32.1399	312.732912	31.950084	328.580357	47.179033	75.40840203	-7.96786776	81.7816	55300.7096759259	2010-04-14 17:01:56	55301.0293402778	2010-04-15 00:42:15	505009010	15.9992	13	15.9992	15.9992	0	15.9992	2	2	0	2	1	0	0	12.242	12.242	27.612	0	PROCESSED	57551.2105787037	2016-06-12 05:03:14	55287	2010-04-01 00:00:00	55362.3098726852	2010-06-15 07:26:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505009010/	Quick Look
346	CYGNUS LOOP 2	312.7259	32.1633	312.213805	31.975338	327.998937	47.37656	75.14683323	-7.61088939	81.0273	55301.0300925926	2010-04-15 00:43:20	55301.2897569444	2010-04-15 06:57:15	505010010	12.932	10	12.932	12.932	0	12.932	1	1	0	1	1	0	0	11.924	11.924	22.4319	0	PROCESSED	57551.2143402778	2016-06-12 05:08:39	55287	2010-04-01 00:00:00	55362.2959375	2010-06-15 07:06:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505010010/	Quick Look
347	CYGNUS LOOP 3	312.9529	31.9301	312.439181	31.741329	328.122092	47.08601	75.08571271	-7.90709143	81.0389	55301.2902777778	2010-04-15 06:58:00	55301.6209953704	2010-04-15 14:54:14	505011010	13.4448	12	13.4448	13.4448	0	13.4448	2	2	0	2	1	0	0	10.427	10.427	28.5719	0	PROCESSED	57551.2233333333	2016-06-12 05:21:36	55287	2010-04-01 00:00:00	55362.3557060185	2010-06-15 08:32:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505011010/	Quick Look
348	CYGNUS LOOP 10	314.1171	30.7461	313.595298	30.553225	328.763604	45.604555	74.79486269	-9.42625359	82.0017	55328.2812152778	2010-05-12 06:44:57	55328.6981134259	2010-05-12 16:45:17	505018010	16.268	16	16.276	16.276	0	16.268	2	2	0	2	1	0	0	12.6551	12.6551	36.012	0	PROCESSED	57551.4785069444	2016-06-12 11:29:03	55287	2010-04-01 00:00:00	55393.3335069445	2010-07-16 08:00:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050005	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505018010/	Quick Look
349	G22.0+0.0	277.823	-9.7151	277.134886	-9.751345	277.921132	13.510599	22.00005623	0.00370699	89.3658	55302.6023842593	2010-04-16 14:27:26	55303.7272222222	2010-04-17 17:27:12	505025010	50.5294	50	50.5294	50.5294	0	50.5294	2	2	0	2	1	0	0	44.6208	44.6208	97.1598	0	PROCESSED	57551.270775463	2016-06-12 06:29:55	55737	2011-06-25 00:00:00	55375.7533101852	2010-06-28 18:04:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050009	ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature.	GALACTIC DIFFUSE EMISSION	5	B	SHIGEO YAMAUCHI		JAP	5	AO5	SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505025010/	Quick Look
350	G37.0-0.1	284.8009	3.5813	284.176842	3.511637	286.494967	26.178305	37.00394757	-0.09218404	68.6266	55303.7327893518	2010-04-17 17:35:13	55304.8814583333	2010-04-18 21:09:18	505027010	50.9694	50	50.9774	50.9774	0	50.9694	2	2	0	2	1	0	0	45.3361	45.3361	99.23	1	PROCESSED	57551.2689699074	2016-06-12 06:27:19	55693	2011-05-12 00:00:00	55326.2903125	2010-05-10 06:58:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050009	ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature.	GALACTIC DIFFUSE EMISSION	5	B	SHIGEO YAMAUCHI		JAP	5	AO5	SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505027010/	Quick Look
351	SGR_C	266.2461	-29.3903	265.44899	-29.370135	266.702279	-5.992122	359.54016882	-0.1184914	267.0744	55464.5256481482	2010-09-25 12:36:56	55466.608599537	2010-09-27 14:36:23	505031010	99.916	100	99.9561	99.916	0	99.956	3	2	0	2	1	0	0	89.0712	89.0712	179.9499	2	PROCESSED	57553.5757175926	2016-06-14 13:49:02	55853	2011-10-19 00:00:00	55484.3402777778	2010-10-15 08:10:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050018	The Sagittarius C Complex (Sgr C) @is composed of many giant molecular clouds (MCs) in two distinct velocity zones, indicating two separate line-of-sight positions of the MCs. Past X-ray flares of Sgr A* likely produced the FeI 6.4 keV emission in the MCs (XRN: X-ray Reflection Nebulae). In Sgr C, the XRN have been solely found in one of the velocity zones. We hence propose to find new XRN in the other velocity zone, which is possibly located at the different distance from the known XRN. With the Suzaku observation, we will determine the 3-dimensional positions of the XRN. Since the presence (or absence) of the XRN largely depends on the epoch of the Sgr A* flares and the 3-dimensional positions of the MCs, Sgr C is a "Rosetta Stone" of the origin and production of the XRN.	GALACTIC DIFFUSE EMISSION	5	A	MASAYOSHI NOBUKAWA		JAP	5	AO5	THE SAGITTARIUS C COMPLEX A ROSETTA STONE OF THE PAST ACTIVITY OF SAGITTARIUS A*	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505031010/	Quick Look
352	BLOWOUT SHELL 1	311.9978	28.9736	311.471635	28.788286	325.391021	44.676168	72.22846422	-9.10440661	48.7676	55360.0953587963	2010-06-13 02:17:19	55361.2627546296	2010-06-14 06:18:22	505055010	52.1945	50	52.2185	52.1945	0	52.2185	1	1	0	1	1	0	0	43.6927	43.6927	100.8559	1	PROCESSED	57552.0261226852	2016-06-13 00:37:37	55741	2011-06-29 00:00:00	55375.7594907407	2010-06-28 18:13:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050088	The Cygnus Loop is a typical shell-like middle-aged SNR. The origin of this SNR is considered to be a cavity explosion. Many previous studies show the abundance of the Cygnus Loop's shell is wholly low (0.2 solar) while that of the ambient medium is typically 0.5 solar. Based on our previous observations, we found some shell regions show 0.5 solar abundances which are consistent with that of the ISM. To explain this result, we formed a hypothesis that the cavity wall density is low in such region and that the forward shock is now propagating outside the cavity, interacting with the ambient medium. In order to verify this hypothesis, we propose to observe the shell of the blowout region which originates from a large break of the cavity wall. We propose to observe two regions for 100ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROYUKI UCHIDA		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP BLOWOUT REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505055010/	Quick Look
353	HD110432	190.599	-63.0744	189.861553	-62.800339	224.074847	-51.705731	301.908501	-0.22062002	344.9423	54718.9065740741	2008-09-09 21:45:28	54719.7050231482	2008-09-10 16:55:14	403002010	25.3332	25	25.3332	25.3332	0	25.3332	2	2	0	2	1	0	0	21.3436	21.3436	68.9779	0	PROCESSED	57543.8037615741	2016-06-04 19:17:25	55148	2009-11-13 00:00:00	54780.4451736111	2008-11-10 10:41:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030005	We propose Suzaku observations of gamma Cas analogues. The sources in this class are characterized by extremely high thermal temperature and iron fluorescent line. We aim to identify the hard X-ray production site using the XIS's spectral capability at the iron K complex and the wide-band sensitivity combining XIS and HXD PIN.	GALACTIC POINT SOURCES	4	B	JUNICHIRO MIURA		JAP	3	AO3	SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403002010/	Quick Look
354	BLOWOUT SHELL 2	312.2035	28.7297	311.67582	28.543644	325.497444	44.382569	72.14669544	-9.39669734	48.0881	55361.263599537	2010-06-14 06:19:35	55362.5155439815	2010-06-15 12:22:23	505056010	52.0698	50	52.0698	52.0698	0	52.0698	2	2	0	2	1	0	0	46.0827	46.0827	108.1558	1	PROCESSED	57552.3493634259	2016-06-13 08:23:05	55741	2011-06-29 00:00:00	55375.7627893518	2010-06-28 18:18:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050088	The Cygnus Loop is a typical shell-like middle-aged SNR. The origin of this SNR is considered to be a cavity explosion. Many previous studies show the abundance of the Cygnus Loop's shell is wholly low (0.2 solar) while that of the ambient medium is typically 0.5 solar. Based on our previous observations, we found some shell regions show 0.5 solar abundances which are consistent with that of the ISM. To explain this result, we formed a hypothesis that the cavity wall density is low in such region and that the forward shock is now propagating outside the cavity, interacting with the ambient medium. In order to verify this hypothesis, we propose to observe the shell of the blowout region which originates from a large break of the cavity wall. We propose to observe two regions for 100ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROYUKI UCHIDA		JAP	5	AO5	X-RAY OBSERVATION OF THE CYGNUS LOOP BLOWOUT REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505056010/	Quick Look
355	HE FOCUSING CONE	49.5928	10.9507	48.911727	10.768982	50.111751	-7.072007	170.97872575	-37.85410489	253.7002	55591.1307291667	2011-01-30 03:08:15	55593.7710763889	2011-02-01 18:30:21	505062010	100.1678	100	100.1678	100.1678	0	100.1678	2	2	0	2	1	0	0	82.7852	82.7852	228.1037	2	PROCESSED	57600.8639351852	2016-07-31 20:44:04	55973	2012-02-16 00:00:00	55607.305462963	2011-02-15 07:19:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050129	We propose the observation though the Helium Focusng Cone. This region seems to make the strong enhancement of Solarwind Charge exchange and cause the annual variation of it. We develop the best observation of the cone by using the area where the abosorption by molecular cloud is huge. By this observation, we investigate the mistery of the emission of Our Galaxy.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI YOSHITAKE		JAP	5	AO5	OBSERVATION THROUGH THE HELIUM FOCUSING CONE: SEARCH FOR THE VARIABILITY OF THE HELIOSPHERIC SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505062010/	Quick Look
356	BD+43 3654	308.4185	44.0658	307.988834	43.893641	331.745866	59.550103	82.48241574	2.36274642	104.8287	55655.0785416667	2011-04-04 01:53:06	55657.0925231482	2011-04-06 02:13:14	506004010	97.0478	100	98.9638	97.0478	0	98.9638	3	2	0	2	1	0	0	88.9256	88.9256	173.9877	0	PROCESSED	57601.4465972222	2016-08-01 10:43:06	56037	2012-04-20 00:00:00	55670.3073842593	2011-04-19 07:22:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060010	It is very important to search for possible particle-acceleration sites among the astrophysical objects. Very recently, synchrotron emission has been discovered with the VLA radio observation from a bow shock region of a runaway star, BD+43 3654, having a very fast stellar wind whose velocity reaches up to 2300 km/s. The maximum energy is estimated to be about 10 TeV, and thus the emission should come to the X-ray band. Here, we propose to perform the 100 ksec observation of BD+43 3654 with Suzaku, in order to determine the strength of the shock from the temperature of the post-shock plasma and to determine the maximum energy of the accelerated electrons.	GALACTIC DIFFUSE EMISSION	5	A	YUKIKATSU TERADA		JAP	6	AO6	SUZAKU OBSERVATION OF NON-THERMAL EMISSION FROM A BOW SHOCK REGION OF A RUNAWAY STAR, BD+43 3654	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506004010/	Quick Look
357	JUPITER	28.9811	10.6021	28.315769	10.357786	30.678261	-1.183373	147.5984875	-49.15640747	249.1843	55937.2038773148	2012-01-11 04:53:35	55938.208599537	2012-01-12 05:00:23	506006030	34.8942	160	34.9022	34.9102	0	34.8942	2	2	0	2	1	0	0	32.2081	32.2081	86.7918	2	PROCESSED	57604.3101273148	2016-08-04 07:26:35	56319	2013-01-27 00:00:00	55952.170787037	2012-01-26 04:05:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060017	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter.	GALACTIC DIFFUSE EMISSION	5	B	KUMI ISHIKAWA		JAP	6	AO6	STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006030/	Quick Look
358	CYGNUS LOOP W-B-S	311.1967	30.3719	310.678738	30.189494	325.222144	46.233696	72.9110541	-7.69596159	71.021	55693.7715277778	2011-05-12 18:31:00	55694.9794212963	2011-05-13 23:30:22	506008010	55.6499	56	55.6499	55.6499	0	55.6499	2	2	0	2	1	0	0	49.8516	49.8516	104.3259	1	PROCESSED	57602.0472916667	2016-08-02 01:08:06	56072	2012-05-25 00:00:00	55705.1847800926	2011-05-24 04:26:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060042	The Cygnus Loop is a prototypical middle-aged SNR. Based on our previous observations, the shell region shows relatively low temperature with low metal abundance. The interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Its abundance non-uniformity indicates the asymmetric explosion. There are two blow-out features: a south-break with one degree diameter and a west-break with half degree diameter. The west-break shows a half-moon shape indicating a rapid expansion in a tenuous plasma. We propose to observe the west-break with SUZAKU for 100 ksec. The plasma in the west-break must be a pure fossil plasma of the SN. We want to study the plasma structure that is almost free from obscuration by the ISM.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	6	AO6	HUNT FOR THE FOSSIL OF THE PROGENITOR STAR IN THE WEST BREAK OF THE CYGNUS LOOP SUPERNOVA REMNANT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506008010/	Quick Look
359	HESSJ1857-B	284.5485	2.7494	283.920534	2.680934	286.113501	25.379812	36.14879968	-0.24805898	252.48	55866.7917592593	2011-11-01 19:00:08	55867.6946990741	2011-11-02 16:40:22	506020010	40.6869	40	40.6869	40.6949	0	40.6949	2	2	0	2	1	0	0	40.0513	40.0513	78.0119	0	PROCESSED	57603.6841435185	2016-08-03 16:25:10	56246	2012-11-15 00:00:00	55879.1725	2011-11-14 04:08:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060061	Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	6	AO6	ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506020010/	Quick Look
360	NGC 7618	349.8326	42.9144	349.23867	42.640678	11.92237	42.546584	105.51742003	-16.82119292	269.9991	55911.4056828704	2011-12-16 09:44:11	55913.6161458333	2011-12-18 14:47:15	506027010	101.1772	100	101.1852	101.1772	0	101.1852	2	2	0	2	1	0	0	95.774	95.774	190.9399	0	PROCESSED	57604.196712963	2016-08-04 04:43:16	56289	2012-12-28 00:00:00	55922.1112847222	2011-12-27 02:40:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060073	We propose to observe nearby merging galaxy group NGC 7618. The asymmetric X-ray shape with a tail and a sharp brightness discontinuity were discoverd by observations of ASCA and Chandra. This is due to a merging with an another galaxy group, UGC 12491, which has similar mass of NGC 7618. The pair is in the primary stage of merging, then we need to obtain the information of the gas outside region to clarify the process of the merging. By taking advantage of low background and high energy resolution of XIS, we estimate accurately distribuion of temperature and metal abundances around both galaxy groups. Then we aim to clarify the process of the merging system of the galaxy groups.	GALACTIC DIFFUSE EMISSION	5	C	KATSUHIRO HAYASHI		JAP	6	AO6	OBSERVATION OF NEARBY MERGING GALAXY GROUP NGC 7618	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506027010/	Quick Look
361	FERMI_BUBBLE_N2	234.4045	4.1242	233.780349	4.287466	230.936286	22.866796	10.25580888	44.20015183	287.5	56145.3990740741	2012-08-06 09:34:40	56145.971099537	2012-08-06 23:18:23	507002010	22.491	20	22.491	22.491	0	22.491	2	2	0	2	1	0	0	22.5	22.5	49.4059	0	PROCESSED	57606.7805555556	2016-08-06 18:44:00	56630	2013-12-04 00:00:00	56264.5602662037	2012-12-03 13:26:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507002010/	Quick Look
362	FERMI_BUBBLE_N3	234.0339	6.0902	233.417441	6.254904	230.000126	24.67426	12.27048516	45.60209416	287.4996	56145.9724537037	2012-08-06 23:20:20	56146.4377893518	2012-08-07 10:30:25	507003010	22.4846	20	22.4846	22.5086	0	22.4926	2	2	0	2	1	0	0	19.836	19.836	40.1959	0	PROCESSED	57606.7866782407	2016-08-06 18:52:49	56535	2013-08-31 00:00:00	56169.009837963	2012-08-30 00:14:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507003010/	Quick Look
363	FERMI_BUBBLE_N6	233.4001	9.0706	232.795243	9.23775	228.456067	27.38567	15.47217439	47.71191257	287.5008	56147.4330324074	2012-08-08 10:23:34	56147.9606134259	2012-08-08 23:03:17	507006010	20.607	20	20.607	20.6246	0	20.619	2	2	0	2	1	0	0	20.3045	20.3045	45.58	0	PROCESSED	57606.8039467593	2016-08-06 19:17:41	56626	2013-11-30 00:00:00	56260.4951851852	2012-11-29 11:53:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507006010/	Quick Look
364	FERMI_BUBBLE_S6	326.677	-46.8481	325.870677	-47.079705	311.980005	-31.325121	351.64382858	-48.94656928	44.0056	56037.1166087963	2012-04-20 02:47:55	56037.6009027778	2012-04-20 14:25:18	507014010	19.6439	20	19.6519	19.6439	0	19.6599	1	1	0	1	1	0	0	14.1827	14.1827	41.8399	1	PROCESSED	57605.2222916667	2016-08-05 05:20:06	56420	2013-05-08 00:00:00	56054.1845833333	2012-05-07 04:25:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070006	Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	7	AO7	SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507014010/	Quick Look
365	GC_SOUTH_2	268.3751	-29.7084	267.575601	-29.69856	268.570633	-6.275404	0.22024801	-1.8703349	273.7998	56192.7899421296	2012-09-22 18:57:31	56194.081412037	2012-09-24 01:57:14	507029010	52.4469	50	52.4629	52.4469	0	52.4549	1	1	0	1	1	0	0	45.2307	45.2307	111.5759	1	PROCESSED	57607.1634259259	2016-08-07 03:55:20	56689	2014-02-01 00:00:00	56321.5121875	2013-01-29 12:17:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070042	We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation.	GALACTIC DIFFUSE EMISSION	5	A	SHINYA NAKASHIMA		JAP	7	AO7	OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507029010/	Quick Look
366	G298.6-0.0	183.3873	-62.6234	182.718198	-62.34531	219.474963	-53.500968	298.59191859	-0.0713547	133.8706	56341.7597222222	2013-02-18 18:14:00	56342.6981712963	2013-02-19 16:45:22	507037020	39.7247	35	39.7247	39.7247	0	39.7247	3	2	0	2	1	0	0	36.2621	36.2621	81.0699	0	PROCESSED	57610.644849537	2016-08-10 15:28:35	56721	2014-03-05 00:00:00	56362.8029861111	2013-03-11 19:16:18	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070047	A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem.	GALACTIC DIFFUSE EMISSION	5	B	AYA BAMBA		JAP	7	AO7	SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507037020/	Quick Look
367	MSH15-56_SW	238.0528	-56.3239	237.060386	-56.174494	248.949341	-35.191477	326.11105465	-1.81589779	86.2015	56326.3325	2013-02-03 07:58:48	56327.8577314815	2013-02-04 20:35:08	507039010	86.0122	100	86.0122	86.0122	0	86.0122	2	2	0	2	1	0	0	88.3912	88.3912	131.7719	2	PROCESSED	57610.534849537	2016-08-10 12:50:11	56714	2014-02-26 00:00:00	56345.5312847222	2013-02-22 12:45:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070055	The magnetic field upstream the shock front of the SN blast wave is the key parameter for discussing particle acceleration. In this study we try to constrain the upstream magnetic field and its amplification based on the ionization parameter of heated ISM just behind the shock. For this purpose, we propose a 100 ks XIS observation of an middle aged SNR MSH 15-56 with non-thermal filaments and an anomalously large ionization age for its dynamical age.	GALACTIC DIFFUSE EMISSION	5	C	YOICHI YATSU		JAP	7	AO7	A STUDY OF PARTICLE ACCELERATION BASED ON THE THERMAL PLASMA BEHIND THE SHOCK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507039010/	Quick Look
368	VELA PWN N1	128.8231	-44.9507	128.399065	-44.776941	153.1311	-60.168643	263.36545364	-2.659461	324.0013	56108.9552083333	2012-06-30 22:55:30	56109.3487962963	2012-07-01 08:22:16	507048010	17.8014	15	17.8094	17.8014	0	17.8094	1	1	0	1	1	0	0	19.2047	19.2047	33.9999	1	PROCESSED	57606.5230439815	2016-08-06 12:33:11	56592	2013-10-27 00:00:00	56226.6327083333	2012-10-26 15:11:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070103	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	7	AO7	HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507048010/	Quick Look
369	VELA PWN N2	128.845	-44.6374	128.418547	-44.463562	152.844801	-59.889474	263.12360018	-2.45940596	325.4993	56109.3500115741	2012-07-01 08:24:01	56109.7210185185	2012-07-01 17:18:16	507049010	18.4118	15	18.4198	18.4118	0	18.4198	1	1	0	1	1	0	0	18.7623	18.7623	32.024	0	PROCESSED	57606.5242939815	2016-08-06 12:34:59	56493	2013-07-20 00:00:00	56127.0941319444	2012-07-19 02:15:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070103	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	7	AO7	HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507049010/	Quick Look
370	VELA PWN N3	128.8419	-44.3423	128.413265	-44.168478	152.550585	-59.63427	262.88578161	-2.28439697	325.9006	56109.7216782407	2012-07-01 17:19:13	56110.0161574074	2012-07-02 00:23:16	507050010	12.3984	15	12.3984	12.3984	0	12.3984	1	1	0	1	1	0	0	13.2454	13.2454	25.4319	1	PROCESSED	57606.5311805556	2016-08-06 12:44:54	56493	2013-07-20 00:00:00	56127.104849537	2012-07-19 02:30:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070103	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	7	AO7	HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507050010/	Quick Look
371	VELA PWN N6	128.8205	-43.4604	128.385504	-43.286672	151.68228	-58.872108	262.17003306	-1.76832201	122.021	56258.4379050926	2012-11-27 10:30:35	56258.805625	2012-11-27 19:20:06	507053010	15.3401	15	15.3481	15.3481	0	15.3401	1	1	0	1	1	0	0	13.9013	13.9013	31.7599	0	PROCESSED	57608.0978819444	2016-08-08 02:20:57	56641	2013-12-15 00:00:00	56275.6586111111	2012-12-14 15:48:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070103	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	7	AO7	HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507053010/	Quick Look
372	3C 397	286.9092	7.1226	286.301586	7.04303	289.342559	29.434869	41.11337729	-0.33398163	251.9939	56595.6848611111	2013-10-30 16:26:12	56597.9106828704	2013-11-01 21:51:23	508001010	103.5157	100	103.5157	103.5157	0	103.5157	2	2	0	2	1	0	0	98.6753	98.6753	192.2937	2	PROCESSED	57613.2313425926	2016-08-13 05:33:08	57012	2014-12-21 00:00:00	56645.6863541667	2013-12-19 16:28:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080011	3C 397 is a Galactic Supernova remnant (SNR) ,whose X-ray spectrum has prominent Fe K line emission. We analyzed Suzaku AO5 data, it resulted in finding of Fe Lya Line. This is a symptomatic of over-ionized (recombining) plasma. On the other hand, the Fe K line center indicates under-ionized (ionizing) plasma. This means that 3C 397 may consisting of two opposite type of plasma: ionizing and recombining. Such a strange state of plasma is not discovered in any SNR.This discovery will be a key to uncovering a mystery of the origin of recombining plasma. However, we still not detect Fe Radiative recombination continuum (RRC),which is a evidence of recombining plasma. To detect the Fe RRC, we propose 150 ks additional observation of 3C 397.	GALACTIC DIFFUSE EMISSION	5	C	RYUSUKE SUGAWARA		JAP	8	AO8	THE INDICATION OF RECOMBINING PLASMA COEXISTING WITH IONIZING PLASMA IN 3C 397	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508001010/	Quick Look
373	W44_EAST	284.1459	1.2991	283.51111	1.232548	285.500202	23.981686	34.67473844	-0.5521979	254.9985	56583.3375231482	2013-10-18 08:06:02	56584.8897337963	2013-10-19 21:21:13	508004010	58.2965	60	58.3045	58.2965	0	58.3149	3	2	0	3	1	0	0	52.7276	52.7276	134.0958	2	PROCESSED	57613.0782407407	2016-08-13 01:52:40	57004	2014-12-13 00:00:00	56637.6520949074	2013-12-11 15:39:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080012	W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks.	GALACTIC DIFFUSE EMISSION	5	A	HIROYUKI UCHIDA		JAP	8	AO8	MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508004010/	Quick Look
374	NW_SRC	221.7499	-1.3162	221.105287	-1.10746	219.72393	14.106437	351.9522425	50.22344256	289.0003	56499.3402430556	2013-07-26 08:09:57	56499.8412037037	2013-07-26 20:11:20	508007010	23.554	20	23.554	23.5554	0	23.554	2	2	0	2	1	0	0	24.103	24.103	43.274	0	PROCESSED	57612.0357986111	2016-08-12 00:51:33	56955	2014-10-25 00:00:00	56587.4553819444	2013-10-22 10:55:45	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080020	Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble.	GALACTIC DIFFUSE EMISSION	5	B	MASAYA TAHARA		JAP	8	AO8	SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508007010/	Quick Look
375	SE_SRC	287.3947	-27.2493	286.61657	-27.330736	285.457559	-4.737737	9.97288902	-15.74410072	84.5985	56404.7026967593	2013-04-22 16:51:53	56405.330775463	2013-04-23 07:56:19	508009010	20.3287	20	20.3287	20.3287	0	20.3287	2	2	0	2	1	0	0	17.5938	17.5938	54.2639	1	PROCESSED	57611.1595833333	2016-08-11 03:49:48	56792	2014-05-15 00:00:00	56425.5555092593	2013-05-13 13:19:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080020	Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble.	GALACTIC DIFFUSE EMISSION	5	B	MASAYA TAHARA		JAP	8	AO8	SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508009010/	Quick Look
376	SE_BGD	288.7458	-25.773	287.977196	-25.860714	286.843449	-3.422342	11.87589948	-16.28754896	81.8427	56405.3324537037	2013-04-23 07:58:44	56405.8329050926	2013-04-23 19:59:23	508010010	20.9653	20	20.9693	20.9653	0	20.9733	2	2	0	2	1	0	0	18.7626	18.7626	43.234	0	PROCESSED	57618.7907291667	2016-08-18 18:58:39	56792	2014-05-15 00:00:00	56425.5426851852	2013-05-13 13:01:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080020	Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble.	GALACTIC DIFFUSE EMISSION	5	B	MASAYA TAHARA		JAP	8	AO8	SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508010010/	Quick Look
377	HESS J1534-571 2	233.1754	-57.1	232.193457	-56.931173	246.039407	-36.679353	323.50919975	-0.81659232	295.9986	56544.0219212963	2013-09-09 00:31:34	56544.6695949074	2013-09-09 16:04:13	508014010	38.9186	40	38.9426	38.9186	0	38.9506	2	2	0	2	1	0	0	36.8565	36.8565	55.9539	0	PROCESSED	57612.5722916667	2016-08-12 13:44:06	56990	2014-11-29 00:00:00	56622.6062268518	2013-11-26 14:32:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080024	Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	8	AO8	RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508014010/	Quick Look
378	HESSJ1858-B	284.4324	2.2013	283.801854	2.133387	285.919657	24.847772	35.60820996	-0.39516335	251.7997	56593.9763310185	2013-10-28 23:25:55	56595.1313541667	2013-10-30 03:09:09	508022010	52.595	50	52.619	52.611	0	52.595	3	2	0	2	1	0	0	49.9941	49.9941	99.7858	2	PROCESSED	57613.1665393518	2016-08-13 03:59:49	56975	2014-11-14 00:00:00	56608.7129166667	2013-11-12 17:06:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080052	HESS J1858+020 is one of the unidentified TeV objects which are candidates for the origin of the cosmic-ray protons. Recently a supernova remnant G35.6-0.4 and molecular clouds were discovered in the vicinity of HESSJ1858+020. The TeV emission may be generated through the interaction between protons accelerated in the SNR and the molecular clouds. However, a star forming region in the cloud was also discovered by an infrared observation, and the region may be responsible for the acceleration of protons. We propose Suzaku observations of HESSJ1858+020 to clarify what particles are the origin of the TeV emission, and to clarify what accelerates the particles.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	8	AO8	DECISION OF PARTICLE ACCELERATION SOURCE OF HESS J1858+020 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508022010/	Quick Look
379	JUPITER	104.0103	23.0994	103.254149	23.165009	102.868934	0.282188	192.60135744	11.26438783	264.454	56763.7225	2014-04-16 17:20:24	56764.0627083333	2014-04-17 01:30:18	508023060	8.8696	160	8.8776	8.8696	0	8.8856	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57614.9524652778	2016-08-14 22:51:33	57212	2015-07-09 00:00:00	56846.5928472222	2014-07-08 14:13:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023060/	Quick Look
380	JUPITER	104.4171	23.0664	103.66133	23.133929	103.244601	0.2859	192.79210183	11.59024455	264.5983	56766.7815972222	2014-04-19 18:45:30	56767.1147916667	2014-04-20 02:45:18	508023100	9.3759	160	9.3839	9.3919	0	9.3759	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57614.9623263889	2016-08-14 23:05:45	57212	2015-07-09 00:00:00	56782.4942824074	2014-05-05 11:51:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080061	Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter.	GALACTIC DIFFUSE EMISSION	5	A	YUICHIRO EZOE		JAP	8	AO8	SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023100/	Quick Look
381	VELA JR WEST3	131.773	-46.2743	131.349543	-46.08957	158.06279	-60.232297	265.67717372	-1.83917649	116.21	56620.0804861111	2013-11-24 01:55:54	56620.7320949074	2013-11-24 17:34:13	508038010	34.9611	30	34.9911	34.9611	0	34.9611	1	1	0	1	1	0	0	40.4434	40.4434	56.2959	0	PROCESSED	57613.4017708333	2016-08-13 09:38:33	56995	2014-12-04 00:00:00	56629.6399421296	2013-12-03 15:21:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080082	We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution.	GALACTIC DIFFUSE EMISSION	5	C	HIDETOSHI SANO		JAP	8	AO8	FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508038010/	Quick Look
382	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
383	VELA PWN W5	126.0444	-45.2057	125.630533	-45.042674	149.898743	-61.36183	262.42223435	-4.39970467	94.9992	56591.8819560185	2013-10-26 21:10:01	56592.3202777778	2013-10-27 07:41:12	508046010	15.8569	15	15.8729	15.8569	0	15.8809	1	1	0	1	1	0	0	12.7358	12.7358	37.8639	0	PROCESSED	57613.1438657407	2016-08-13 03:27:10	57009	2014-12-18 00:00:00	56643.6567824074	2013-12-17 15:45:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080090	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered.	GALACTIC DIFFUSE EMISSION	5	B	KOJI MORI		JAP	8	AO8	SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508046010/	Quick Look
384	VELA PWN W6	125.6171	-45.2116	125.2045	-45.05026	149.354915	-61.513653	262.25511101	-4.65051542	95.0008	56592.3208912037	2013-10-27 07:42:05	56592.8209722222	2013-10-27 19:42:12	508047010	17.2398	15	17.2478	17.2398	0	17.2398	1	1	0	1	1	0	0	16.2299	16.2299	43.1999	0	PROCESSED	57613.1284606482	2016-08-13 03:04:59	57011	2014-12-20 00:00:00	56645.5849421296	2013-12-19 14:02:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080090	We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered.	GALACTIC DIFFUSE EMISSION	5	B	KOJI MORI		JAP	8	AO8	SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508047010/	Quick Look
385	W49B	287.7839	9.1153	287.185543	9.031646	290.654077	31.289696	43.2808507	-0.18308455	82.0062	57122.7467013889	2015-04-10 17:55:15	57125.7127777778	2015-04-13 17:06:24	509001010	81.4763	400	81.4763	113.9098	0	113.9162	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.986724537	2016-08-17 23:40:53	56748	2014-04-01 00:00:00	57136.5735300926	2015-04-24 13:45:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090007	W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	9	AO9	DEEP OBSERVATIONS OF W49B	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001010/	Quick Look
386	W49B	287.7843	9.1147	287.18594	9.031044	290.654435	31.289046	43.28050127	-0.18371216	82.0064	57128.6891203704	2015-04-16 16:32:20	57131.6619328704	2015-04-19 15:53:11	509001030	100.9959	400	100.9959	106.4207	0	106.3967	4	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.0043518518	2016-08-18 00:06:16	56748	2014-04-01 00:00:00	57220.3809722222	2015-07-17 09:08:36	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090007	W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	9	AO9	DEEP OBSERVATIONS OF W49B	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001030/	Quick Look
387	G1.9+0.3	267.1939	-27.1714	266.410492	-27.155866	267.488865	-3.754805	1.87009843	0.31910459	104.2133	57099.6072569445	2015-03-18 14:34:27	57101.7854976852	2015-03-20 18:51:07	509003010	92.0313	100	92.0313	97.0859	0	97.0699	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8499189815	2016-08-17 20:23:53	57527	2016-05-19 00:00:00	57160.6404861111	2015-05-18 15:22:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090030	We propose a Suzaku observations of the youngest supernova remnant (SNR) G1.9+0.3. We aim to detect flux increase and spectral hardening of synchrotron X-rays since 2011 when the previous Suzaku observation was performed. The measurement should provide us with important information about the maximum acceleration energy attainable by diffusive shock acceleration in SNRs. Suzaku XIS is the most suitable detector since it has the large effective area even in the hard band up to 10 keV. If X-ray flux increase is significantly larger than that measured in the radio band, we can conclude that maximum acceleration energy is becoming higher at present.	GALACTIC DIFFUSE EMISSION	5	A	TAKAAKI TANAKA	YASUNOBU UCHIYAMA	JAP	9	AO9	MEASUREMENT OF TIME VARIABILITY OF SYNCHROTRON X-RAYS FROM THE YOUNGEST SUPERNOVA REMNANT G1.9+0.3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509003010/	Quick Look
388	VELA PWN GEV5	128.1777	-45.5057	127.759875	-45.334391	152.900781	-60.876983	263.54099229	-3.35509044	120.3003	56987.5594328704	2014-11-26 13:25:35	56987.9009490741	2014-11-26 21:37:22	509015010	16.1889	15	16.1889	16.2127	0	16.1969	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.822025463	2016-08-16 19:43:43	57368	2015-12-12 00:00:00	57002.4333564815	2014-12-11 10:24:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090046	We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended.	GALACTIC DIFFUSE EMISSION	5	C	KOJI MORI		JAP	9	AO9	X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509015010/	Quick Look
389	G166.0+4.3_SE	81.6718	42.6436	80.778042	42.601144	83.516564	19.390604	166.37682371	4.1455421	266.8508	57094.5870486111	2015-03-13 14:05:21	57095.305	2015-03-14 07:19:12	509024020	26.0329	27	26.0329	27.3929	0	27.3929	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.780625	2016-08-17 18:44:06	57478	2016-03-31 00:00:00	57108.4092939815	2015-03-27 09:49:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090092	Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation.	GALACTIC DIFFUSE EMISSION	5	A	AKIHIRO TAKATA		JAP	9	AO9	G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509024020/	Quick Look
390	CIZA J1358.9-4750_NE	209.8984	-47.6059	209.108141	-47.363535	225.843523	-32.945776	314.66509294	13.70714471	293.0012	56879.8864467593	2014-08-10 21:16:29	56880.8606481482	2014-08-11 20:39:20	509025010	40.2748	40	40.2828	40.2828	0	40.2748	2	2	0	2	1	0	0	7.7468	7.7468	19.736	0	PROCESSED	57616.4833333333	2016-08-16 11:36:00	57270	2015-09-05 00:00:00	56902.1990972222	2014-09-02 04:46:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090102	Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS.	GALACTIC DIFFUSE EMISSION	5	B	YUICHI KATO		JAP	9	AO9	OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509025010/	Quick Look
391	VERJ2019_P2	305.0647	36.873	304.594845	36.714007	321.75914	54.196272	75.14540231	0.26023113	251.4317	56970.0347453704	2014-11-09 00:50:02	56971.0419097222	2014-11-10 01:00:21	509029010	40.4941	40	40.4941	40.5021	0	40.5021	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7544791667	2016-08-16 18:06:27	57436	2016-02-18 00:00:00	57071.4171527778	2015-02-18 10:00:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090120	The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at elongated TeV gamma-ray emission found by Milagro and recently resolved by VERITAS. Although an energetic pulsar PSR J2021+3651 coincides with one of TeV peaks, most of gamma-ray emission still remains unexplained. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we aim to detect X-ray counterparts, presumably unknown pulsar wind nebulae. Connection with a Wolf-Rayet star and an HII region inside this region, which positionally coincide with the gamma-ray peak, will also be investigated.	GALACTIC DIFFUSE EMISSION	5	C	TSUNEFUMI MIZUNO		JAP	9	AO9	SEARCH FOR TEV ACCELERATORS IN NEARBY STAR-FORMING REGION CYGNUS-X WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509029010/	Quick Look
392	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
393	PKS 0558-504	89.9335	-50.4395	89.62999	-50.44058	89.864093	-73.881363	257.95137808	-28.57681508	212.4401	54121.9091203704	2007-01-21 21:49:08	54122.3529976852	2007-01-22 08:28:19	701011050	19.5154	20	19.5314	19.5154	0	19.5314	1	1	0	1	1	0	0	16.1236	16.1236	38.312	0	PROCESSED	57536.8983217593	2016-05-28 21:33:35	54735	2008-09-26 00:00:00	54137.0453240741	2007-02-06 01:05:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010057	Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	C	YOSHITO HABA		JAP	1	AO1	SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011050/	Quick Look
394	SWIFT J0350.1-5019	57.6662	-50.2998	57.309175	-50.449494	28.967165	-67.019674	259.65657878	-48.95336771	180.7044	54062.0888078704	2006-11-23 02:07:53	54062.5647453704	2006-11-23 13:33:14	701017020	19.271	23	19.271	19.271	0	19.271	1	1	0	1	1	0	0	16.74	16.74	41.097	0	PROCESSED	57536.1549768518	2016-05-28 03:43:10	54750	2008-10-11 00:00:00	54088.5939583333	2006-12-19 14:15:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010133	Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background".	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	1	AO1	DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017020/	Quick Look
395	OJ 287 FLARE	133.7115	20.1695	132.996174	20.360602	130.493887	2.661227	206.74425687	35.84822718	98.7868	54411.475	2007-11-07 11:24:00	54413.896099537	2007-11-09 21:30:23	702008010	112.044	100	112.052	112.06	0	112.044	2	2	0	2	1	0	0	102.9238	102.9238	209.1519	3	PROCESSED	57540.5116087963	2016-06-01 12:16:43	54791	2008-11-21 00:00:00	54423.3848032407	2007-11-19 09:14:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020024	OJ 287 is a promissing candidate of a suppermassive binary black hole, based on its periodic flare with a cycle of about 12 years. The next flare is predicted to take place on the fall, 2007. Therefore, two Suzaku exposures on OJ 287 is proposed, coordinated with radio, optical and very high energy gamma-ray observations. The first observation is on the spring to obtained the multi-wavelength spectrum of the target in its quiescent phase. The second is planned to be in a form of ToO observation on the fall, which will be triggered by an optical flare. The nature of the flare will be extensively investigated in these observatsions.	EXTRAGALACTIC COMPACT SOURCES	7	A	NAOKI ISOBE		JAP	2	AO2-TOO	MULTI-WAVELENGTH OBSERVATION OF PREDICTED FLARE OF SUPERMASSIVE BINARY BLACK HOLE CANDIDATE, OJ 287	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702008010/	Quick Look
396	IC 3639	190.1935	-36.8078	189.517353	-36.533453	205.04698	-29.556314	300.55692841	26.01476797	293.9494	54293.1966435185	2007-07-12 04:43:10	54294.4133564815	2007-07-13 09:55:14	702011010	53.3912	50	53.3912	53.3912	0	53.3912	2	2	0	2	1	0	0	48.4852	48.4852	105.11	1	PROCESSED	57539.1904050926	2016-05-31 04:34:11	54709	2008-08-31 00:00:00	54339.5331365741	2007-08-27 12:47:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020034	Seyfert 2 galaxies often have an nucleus obscured by thick matter. Risaliti et al. found that Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy s population by studying the distribution of absorbing column densities among Seyfert 2 galaxies. This result is important to discuss on the structure and evolution of active galactic nuclei. However, it is difficult to classify Seyfert 2 galaxies into Compton thick and thin objects only by using their X-ray spectra below 10 keV. Therefore, there may be Compton thin objects among Risaliti s Compton thick sample. In order to make the distribuion of the column density more reliable, we propose the Suzaku observations of heavily obscured AGNs with NH >1E25cm-2.	EXTRAGALACTIC COMPACT SOURCES	7	B	HISAMITSU AWAKI		JAP	2	AO2	SUZAKU OBSERVATIONS OF THE HEAVILY OBSCURED AGNS WITH NH>1E25 CM-2	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702011010/	Quick Look
397	PKS2126-15	322.2988	-15.6437	321.609655	-15.862975	319.629627	-0.752825	35.92993079	-41.86589251	72.3882	54576.0912384259	2008-04-20 02:11:23	54578.4238310185	2008-04-22 10:10:19	703001010	81.9214	80	81.9214	81.9364	0	81.9454	2	2	0	2	1	0	0	71.5414	71.5414	201.5279	3	PROCESSED	57542.3941087963	2016-06-03 09:27:31	54961	2009-05-10 00:00:00	54594.3427777778	2008-05-08 08:13:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030003	We propose intensive Suzaku observations (80ksec each) of two "primitive" blazars at z > 3.3, with a highly unusual SED. ROXA J081009.9 (z=4.0) was recently found by a short Swift/XRT exposure (6 ksec) with a luminosity well in excess of 10^47 ergs/s, but its synchrotron power peaking above 10 keV. This may suggest the bulk Lorentz factor of the jet could reach ~1000 like GRBs, though quite conspicuous among the AGN jets. Meanwhile, unusual SED of PKS2126-15 (z=3.3) , where the synchrotron peaking at GHz and the inverse Compton peaks at ~10 keV, is most likely due to the presence of ultra-massive black hole with 2x10^10 Ms. These new-types are only found in highly distant universe, and maybe categorized as primitive blazars.	EXTRAGALACTIC COMPACT SOURCES	7	B	JUN KATAOKA		JAP	3	AO3	UNVEILING NEW-TYPE "PRIMITIVE" BLAZARS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703001010/	Quick Look
398	SWIFT J2009.0-6103	302.158	-61.0495	301.087298	-61.195509	289.575526	-39.777943	335.84532046	-32.77756596	73.0628	54563.6948148148	2008-04-07 16:40:32	54564.600775463	2008-04-08 14:25:07	703015010	43.7268	40	43.7268	43.7268	0	43.7268	2	2	0	2	1	0	0	36.1996	36.1996	78.268	1	PROCESSED	57542.2661342593	2016-06-03 06:23:14	54953	2009-05-02 00:00:00	54580.2454976852	2008-04-24 05:53:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030045	Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	3	AO3	DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703015010/	Quick Look
399	1739+518	264.9784	52.1719	264.694846	52.196929	257.680013	75.396251	79.52646168	31.85370007	22.9152	54985.7571759259	2009-06-03 18:10:20	54986.3641087963	2009-06-04 08:44:19	704008010	22.4868	20	22.4948	22.4948	0	22.4868	2	2	0	2	1	0	0	28.2378	28.2378	52.4319	0	PROCESSED	57547.4536458333	2016-06-08 10:53:15	55367	2010-06-20 00:00:00	54998.1968634259	2009-06-16 04:43:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040049	We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	4	AO4	SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704008010/	Quick Look
400	CENTAURUS_A	201.3322	-43.0688	200.598815	-42.808768	217.137097	-31.383435	309.48334217	19.37141452	298.7164	55048.3079513889	2009-08-05 07:23:27	55049.7029398148	2009-08-06 16:52:14	704018020	51.2787	50	51.2787	51.2947	0	51.2867	2	2	0	2	1	0	0	43.7332	43.7332	120.5059	1	PROCESSED	57548.0839699074	2016-06-09 02:00:55	55430	2010-08-22 00:00:00	55062.3520023148	2009-08-19 08:26:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040085	We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku.	EXTRAGALACTIC COMPACT SOURCES	7	A	YASUSHI FUKAZAWA		JAP	4	AO4	SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704018020/	Quick Look
401	PBC J0216.1+5124	34.0954	51.5104	33.261431	51.278784	50.779826	35.406451	136.13174863	-9.17115539	78.3815	55421.9728356482	2010-08-13 23:20:53	55423.4168171296	2010-08-15 10:00:13	705006010	72.7733	80	72.7964	72.7733	0	72.7964	2	2	0	2	1	0	0	73.5582	73.5582	124.7258	3	PROCESSED	57553.114375	2016-06-14 02:44:42	55804	2011-08-31 00:00:00	55435.2980092593	2010-08-27 07:09:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050024	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	5	AO5	BROAD BAND SPECTRA OF SWIFT/BAT SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705006010/	Quick Look
402	EMS1164	265.9438	-76.3446	264.162094	-76.320567	268.39939	-52.925114	317.07818058	-22.45515073	114.3984	55300.0111689815	2010-04-14 00:16:05	55300.6980439815	2010-04-14 16:45:11	705013010	42.3783	40	42.3836	42.3783	0	42.389	2	2	0	2	1	0	0	39.0487	39.0487	59.3439	1	PROCESSED	57551.2223958333	2016-06-12 05:20:15	55675	2011-04-24 00:00:00	55309.1947453704	2010-04-23 04:40:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050050	We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators".	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5	SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705013010/	Quick Look
403	EMS1395	310.8148	17.1786	310.239098	16.997696	318.830842	33.961912	61.89528011	-15.30299533	74.9546	55319.8076736111	2010-05-03 19:23:03	55320.4342476852	2010-05-04 10:25:19	705015010	23.3002	20	23.3002	23.3002	0	23.3002	2	2	0	2	1	0	0	19.4944	19.4944	54.1299	0	PROCESSED	57551.3813773148	2016-06-12 09:09:11	55696	2011-05-15 00:00:00	55330.2005208333	2010-05-14 04:48:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050050	We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators".	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5	SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705015010/	Quick Look
404	MRK 509	311.0469	-10.7401	310.365769	-10.921688	310.545768	7.110758	35.95684044	-29.86794514	252.3716	55521.595625	2010-11-21 14:17:42	55523.8155092593	2010-11-23 19:34:20	705025010	102.1205	100	102.1285	102.1285	0	102.1205	2	2	0	2	1	0	0	92.0625	92.0625	191.7697	0	PROCESSED	57554.2039930556	2016-06-15 04:53:45	55916	2011-12-21 00:00:00	55550.2628356482	2010-12-20 06:18:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050113	We propose the observation of one of the typical Seyferts I Mrk 509 for 100 ksec to understand how a vry hard component component that varies independently of power-law is created and how the physical structure near SMBH in Seyferts is. The hard component has been found by carrying out timing analysis of hard X-ray band to explain the extremely broad iron line feature of several Seyferts. Taking this component into account, we succeeded to explain the data of MCG 6-30-15 without the extremely broad iron line, though the origin of this component has not been identified yet. Because Mrk 509 has strong flux and large amplitude of hard X-ray variation, we found it is the most suitable object to verify this component and to get alternative interpretation to the extremely broad iron line.	EXTRAGALACTIC COMPACT SOURCES	7	C	HIROFUMI NODA		JAP	5	AO5	VERIFICATION OF A HARD COMPONENT THAT VARIES INDEPENDENTLY OF POWER-LAW IN TYPE I SEYFERT MRK 509	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705025010/	Quick Look
405	NGC6251_LOBE_BGD2	245.2973	82.3586	246.565183	82.472103	101.108878	73.211894	115.82251183	31.60630628	26.9772	55667.4343981482	2011-04-16 10:25:32	55667.8230902778	2011-04-16 19:45:15	706005010	12.0103	20	12.0183	12.0103	0	12.0263	1	1	0	1	1	0	0	17.5851	17.5851	33.5759	0	PROCESSED	57601.5154976852	2016-08-01 12:22:19	56058	2012-05-11 00:00:00	55690.9834490741	2011-05-09 23:36:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060004	We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	6	AO6	SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706005010/	Quick Look
406	IC 4518A	224.419	-43.1269	223.597719	-42.926611	234.851401	-25.085272	326.11466585	13.99053707	102.9822	55959.1723263889	2012-02-02 04:08:09	55961.0002777778	2012-02-04 00:00:24	706012010	64.3986	60	64.3986	64.3986	0	64.3986	2	2	0	2	1	0	0	57.2381	57.2381	157.9058	1	PROCESSED	57604.5692708333	2016-08-04 13:39:45	56434	2013-05-22 00:00:00	56068.6321064815	2012-05-21 15:10:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060040	We propose to observe the Compton-thin AGN IC 4518A with a very small L_X/L_IR ratio, which has often been employed as an indicator of the presence of a Compton-thick AGN. Our aim is to examine the recent argument that L_X/L_IR is not a good measure of absorption column densities and that this ratio is more dependent on the covering fraction of absorber and intrinsic spectral shape. We measure the spectral slope, covering fraction, and NH, and compare them with the prediction of Monte-Carlo simulations to test the validity of L_X/L_IR as a measure of Compton thickness.	EXTRAGALACTIC COMPACT SOURCES	7	C	YOSHITAKA HIRATA		JAP	6	AO6	BROAD-BAND SPECTRA OF THE COMPTON-THIN AGN IC 4518A WITH A SMALL L_X/L_IR: TESTING VALIDITY OF A COMPTON-THICK INDICATOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706012010/	Quick Look
407	RX J1633+4718	248.3303	47.3072	247.970126	47.410772	228.761848	67.666439	73.53738657	42.62611906	329.4078	55743.8204050926	2011-07-01 19:41:23	55744.8460069444	2011-07-02 20:18:15	706027010	39.9916	40	39.9916	39.9916	0	39.9916	2	2	0	2	1	0	0	39.6531	39.6531	88.6059	1	PROCESSED	57602.4692013889	2016-08-02 11:15:39	56144	2012-08-05 00:00:00	55775.3057407407	2011-08-02 07:20:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060089	RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time.	EXTRAGALACTIC COMPACT SOURCES	7	A	KIYOSHI HAYASHIDA		JAP	6	AO6	X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027010/	Quick Look
408	3C 236 WEST LOBE	151.329	34.9949	150.593371	35.23826	140.67974	21.703249	189.91194492	53.83302535	299.9981	56053.9465740741	2012-05-06 22:43:04	56055.7862384259	2012-05-08 18:52:11	707005010	83.9935	80	83.9935	83.9935	0	83.9935	2	2	0	2	1	0	0	80.4248	80.4248	158.9318	2	PROCESSED	57605.4100925926	2016-08-05 09:50:32	56436	2013-05-24 00:00:00	56070.2690856482	2012-05-23 06:27:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070014	Through the Suzaku observations of giant radio galaxies, of which the size is larger than about 1 Mpc, we are going to reveal a picture that the jets in radio galaxies become inactive as they evolve from 500 kpc to 1 Mpc. However, the current Suzaku sample of the giant radio galaxies is far from being satisfactory to make a definite conclusion. Therefore, we propose a Suzaku observation of 3C 236, one of the most giant radio galaxy in the Universe.	EXTRAGALACTIC COMPACT SOURCES	7	A	NAOKI ISOBE		JAP	7	AO7	INVESTIGATION INTO EVOLUTION OF THE JET ENERGETICS, THROUGH THE SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 236	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707005010/	Quick Look
409	2FGL J0037.8+1238	9.4591	12.6426	8.808625	12.367737	13.671851	7.875917	117.75617703	-50.09241086	67.2998	56108.005787037	2012-06-30 00:08:20	56108.9432523148	2012-06-30 22:38:17	707010010	28.6039	30	28.6039	28.6039	0	28.6039	2	2	0	2	1	0	0	30.0977	30.0977	80.972	1	PROCESSED	57606.5224768518	2016-08-06 12:32:22	56493	2013-07-20 00:00:00	56127.1415625	2012-07-19 03:23:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070034	We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN).	EXTRAGALACTIC COMPACT SOURCES	7	B	JUN KATAOKA		JAP	7	AO7	FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707010010/	Quick Look
410	NGC1365	53.4072	-36.1471	52.929884	-36.314043	36.805891	-53.04754	237.96723255	-54.59318142	57.2979	56125.3876273148	2012-07-17 09:18:11	56125.896087963	2012-07-17 21:30:22	707017030	26.7672	30	26.7672	26.7672	0	26.7672	2	2	0	2	1	0	0	25.2112	25.2112	43.9239	1	PROCESSED	57606.6299537037	2016-08-06 15:07:08	56582	2013-10-17 00:00:00	56212.7663194444	2012-10-12 18:23:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070095	NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. }	EXTRAGALACTIC COMPACT SOURCES	7	B	YASUSHI FUKAZAWA		JAP	7	AO7	MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017030/	Quick Look
411	NGC 3516	166.6556	72.561	165.802341	72.831319	123.361761	57.969661	133.25565935	42.40250412	335.7404	56391.9675925926	2013-04-09 23:13:20	56393.0460185185	2013-04-11 01:06:16	708006010	51.386	50	51.402	51.386	0	51.402	2	2	0	2	1	0	0	49.1015	49.1015	93.1638	1	PROCESSED	57611.0515856482	2016-08-11 01:14:17	56383	2013-04-01 00:00:00	56421.6947106482	2013-05-09 16:40:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080066	We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	8	AO8	THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006010/	Quick Look
412	NGC 3516	166.6684	72.5566	165.815394	72.826934	123.372761	57.969452	133.25443095	42.40827092	314.5458	56409.0119560185	2013-04-27 00:17:13	56409.446087963	2013-04-27 10:42:22	708006020	19.103	50	19.119	19.103	0	19.119	3	2	0	2	1	0	0	20.2121	20.2121	30.7239	0	PROCESSED	57611.1744907407	2016-08-11 04:11:16	56383	2013-04-01 00:00:00	56457.6034375	2013-06-14 14:28:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080066	We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	8	AO8	THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006020/	Quick Look
413	NGC 3516	166.6764	72.5574	165.823506	72.827743	123.374751	57.971749	133.25110438	42.40886909	307.603	56424.0155555556	2013-05-12 00:22:24	56425.1044328704	2013-05-13 02:30:23	708006030	50.4283	50	50.4283	50.4283	0	50.4283	1	1	0	1	1	0	0	57.2275	57.2275	94.076	0	PROCESSED	57611.3108680556	2016-08-11 07:27:39	56383	2013-04-01 00:00:00	56436.6511805556	2013-05-24 15:37:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080066	We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	8	AO8	THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006030/	Quick Look
414	NGC6552	270.0757	66.6036	270.078264	66.603205	60.706525	89.950181	96.43339546	29.78135373	217.6129	56610.8399884259	2013-11-14 20:09:35	56613.0126851852	2013-11-17 00:18:16	708014010	105.7767	100	105.7767	105.7767	0	105.7767	2	2	0	2	1	0	0	102.2797	102.2797	187.7079	1	PROCESSED	57613.3907060185	2016-08-13 09:22:37	57019	2014-12-28 00:00:00	56653.7413078704	2013-12-27 17:47:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080092	We propose to observe the interesting Seyfert 2 galaxy NGC6552, which has multi fluorescence lines in the X-ray band. There ara only three objects, including NGC6552, which has multi fluorescence lines in the X-ray band. We aim to detect emission lines finely and study the chemical evolution of the galaxy. We also aim measurements of hard X-ray continuum to constrain the reflection component and other nonthermal emission asscciated with jet or starburst activity.	EXTRAGALACTIC COMPACT SOURCES	7	C	TAKAFUMI KAWANO		JAP	8	AO8	OBSERVATION OF THE MULTI EMISSION LINES FROM SEYFERT 2 GALAXY: NGC6552	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708014010/	Quick Look
415	SN 2006JD	120.5317	0.8109	119.887421	0.950976	122.551734	-19.245465	220.45479917	16.05743863	101.8795	56954.8286458333	2014-10-24 19:53:15	56958.31125	2014-10-28 07:28:12	709001010	144.4894	150	144.4894	151.0361	0	151.0521	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7014351852	2016-08-16 16:50:04	57435	2016-02-17 00:00:00	57066.4298032407	2015-02-13 10:18:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090005	We propose a 150 ks observation of a supernova (SN) 2006jd, a bright SN IIn discovered on October 12, 2006. It is a rare SN that remains bright in X-rays over several years, hence provides us with a rare opportunity to study the dense medium that was ejected by the progenitor star before the SN explosion. Our analysis of archival data taken by Suzaku in 2008 and XMM-Newton in 2009 has indicated interesting spectral evolution, i.e., spectral softening and an increasing centroid of Fe-K lines complex. Our proposed observation will show much clearer spectral variation than that seen in the previous Suzaku and XMM-Newton data, allowing us to understand the details of spectral evolution. The dataset will become a reference for the study of late-time X-ray spectroscopy of SN IIn.	EXTRAGALACTIC COMPACT SOURCES	7	B	SATORU KATSUDA		JAP	9	AO9	PROBING LATE-TIME X-RAY SPECTRUM OF SN 2006JD	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709001010/	Quick Look
416	NGC 2655	133.9038	78.2094	132.281402	78.399558	105.125039	57.091904	134.93858201	32.69360092	275.5561	56789.4281828704	2014-05-12 10:16:35	56791.0731712963	2014-05-14 01:45:22	709003010	76.8371	80	76.8371	76.8371	0	76.8371	2	2	0	2	0	0	0	0	0	2.1539	0	PROCESSED	57615.0904398148	2016-08-15 02:10:14	57173	2015-05-31 00:00:00	56807.6198726852	2014-05-30 14:52:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090017	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	9	AO9	BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709003010/	Quick Look
417	ARP318	32.3792	-10.1586	31.765368	-10.394539	26.44249	-21.810803	173.95964772	-64.97329044	75.9989	56873.8890509259	2014-08-04 21:20:14	56875.8252662037	2014-08-06 19:48:23	709009010	80.2195	80	80.2195	80.2195	0	80.222	2	2	0	2	1	0	0	15.3811	15.3811	43.076	0	PROCESSED	57616.4808217593	2016-08-16 11:32:23	57267	2015-09-02 00:00:00	56898.4603703704	2014-08-29 11:02:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090037	We propose Suzaku/XIS and PIN observations of nearby two radio-quiet AGNs with very weak mid-infrared emission, which might represent a new class of hot dust free AGNs. We found hot dust free AGN candidates by combining the Swift/BAT hard X-ray all-sky AGN catalog with mid-infrared (MIR) all-sky surveys. Three out of 503 sources are not detected in their MIR bands, even in the high sensitivity of WISE. One source is radio-loud AGNs and the other two radio-quiet sources are also observed in 2-10 keV band with Swift/XRT, and no significant Fe Ka line emission is detected. The scientific goal of this proposal is to obtain the first Fe Ka detection or strong constraints of the emission, which will give us a direct evidence that these sources have very small amount or even lack of torus.	EXTRAGALACTIC COMPACT SOURCES	7	B	KOHEI ICHIKAWA		JAP	9	AO9	THE FIRST BROADBAND X-RAY OBSERVATIONS OF HOT DUST FREE AGNS IN THE LOCAL UNIVERSE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709009010/	Quick Look
418	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
419	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
420	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
421	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
422	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
423	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
424	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
425	VELA JR SE3	133.7724	-47.2478	133.349347	-47.055911	161.448089	-60.302336	267.30006641	-1.40128647	110.0008	56629.9618055556	2013-12-03 23:05:00	56630.5806828704	2013-12-04 13:56:11	508062010	27.3638	25	27.3644	27.3638	0	27.3658	2	2	0	2	1	0	0	21.7141	21.7141	53.4599	1	PROCESSED	57613.4843055556	2016-08-13 11:37:24	57005	2014-12-14 00:00:00	56639.5938888889	2013-12-13 14:15:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080117	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr.	GALACTIC DIFFUSE EMISSION	5	C	TARO FUKUYAMA		JAP	8	AO8	OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR.	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508062010/	Quick Look
426	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
427	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
428	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
429	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
430	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
431	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
432	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
433	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
434	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
435	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
436	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
437	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
438	W51SW	290.8908	14.1062	290.315286	14.008227	295.206632	35.736826	49.1149541	-0.54215584	104.3698	55285.3081944444	2010-03-30 07:23:48	55286.3752314815	2010-03-31 09:00:20	504067010	43.7287	40	43.7287	43.7287	0	43.7287	2	2	0	2	1	0	0	9.8137	9.8137	92.1799	0	PROCESSED	57551.0856597222	2016-06-12 02:03:21	55671	2011-04-20 00:00:00	55302.2468055556	2010-04-16 05:55:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040129	We propose to observe the supernova remnant (SNR) W51C with Suzaku XIS. The thermal energy of plasma in W51C, ~3x10^51ergs, is much larger than typical kinetic energy of supernova and can give a large amount of energy to cosmic-ray acceleration. The SNR interactes with the giant molecler cloud and is expected to emit gamma-rays from cosmic-ray interaction. We search for non-thermal X-ray diffuse emission from electron bremsstrahlung or synchrotron emission of secondary electrons produced by decaying charged pions created by p-p interaction.	GALACTIC DIFFUSE EMISSION	5	C	HIDEAKI KATAGIRI		JAP	4	AO4	ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504067010/	Quick Look
439	SGR1806-20	272.1595	-20.349	271.415501	-20.357687	272.017973	3.076639	10.0481975	-0.20823053	88.7483	54189.6305555556	2007-03-30 15:08:00	54190.0627199074	2007-03-31 01:30:19	401021010	19.2889	20	19.2889	19.595	0	19.3563	1	1	0	1	1	0	0	16.5071	16.5071	37.3279	1	PROCESSED	57538.0253587963	2016-05-30 00:36:31	54561	2008-04-05 00:00:00	54209.5169212963	2007-04-19 12:24:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010124	We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs.	GALACTIC POINT SOURCES	4	A	YUJIN NAKAGAWA		JAP	1	AO1-TOO	PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR"	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401021010/	Quick Look
440	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
441	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
442	Crab nebula	83.2708	21.9976	82.518718	21.963167	83.762776	-1.29769	184.39063256	-6.07689385	86.7331	53607.7165162037	2005-08-25 17:11:47	53607.9167361111	2005-08-25 22:00:06	100010050	9.3469	5	9.3469	9.3469	9.3469	9.3469	1	1	1	1	1	0	0	6.653	6.653	17.2879	0	PROCESSED	57526.9	2016-05-18 21:36:00	54247	2007-05-27 00:00:00	54122.4223611111	2007-01-22 10:08:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000010	Crab nebula multi pointings	CALIBRATION	1	A	SWG		JAP	0	SWG	Crab Offset 1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010050/	Quick Look
443	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
444	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
445	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
446	GC_SGR_B_NORTH	266.6958	-28.383	265.90497	-28.365031	267.072823	-4.975469	0.60519276	0.06967717	271.4415	53999.7284837963	2006-09-21 17:29:01	54001.2863425926	2006-09-23 06:52:20	501040010	61.3753	62	61.3913	61.3753	61.3833	61.3913	2	2	2	2	1	0	0	53.867	53.867	134.5818	2	PROCESSED	57535.7042361111	2016-05-27 16:54:06	54735	2008-09-26 00:00:00	54021.2828472222	2006-10-13 06:47:18	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010060	We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	1	AO1	OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501040010/	Quick Look
447	EX HYA	193.0706	-29.2994	192.395685	-29.027802	203.848452	-21.746269	303.15288952	33.57198642	300.0004	54299.8912152778	2007-07-18 21:23:21	54302.4377199074	2007-07-21 10:30:19	402001010	100.5157	100	100.5237	100.5157	0	100.5237	2	2	0	2	1	0	0	91.1135	91.1135	219.9599	1	PROCESSED	57539.3319097222	2016-05-31 07:57:57	54707	2008-08-29 00:00:00	54339.5139467593	2007-08-27 12:20:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020008	The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS.	GALACTIC POINT SOURCES	4	A	MANABU ISHIDA		JAP	2	AO2	MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402001010/	Quick Look
448	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
449	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
450	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
451	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
452	VELA SOUTHWEST 1	126.2671	-48.2152	125.877652	-48.051248	153.532268	-63.870386	264.99036518	-5.99332729	119.5649	55164.9700925926	2009-11-29 23:16:56	55165.818900463	2009-11-30 19:39:13	504063010	32.7331	30	32.7492	32.7331	0	32.7411	3	2	0	2	1	0	0	23.7674	23.7674	73.3099	0	PROCESSED	57549.6219791667	2016-06-10 14:55:39	55546	2010-12-16 00:00:00	55179.268587963	2009-12-14 06:26:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040121	We propose 2 pointing-observations of south western part of Vela supernova remnant. Vela SNR has the largest angular size of 8 degree in diameter, so it is suitable to carry out spatial resolved spectroscopy with Suzaku.	GALACTIC DIFFUSE EMISSION	5	C	JUNKO HIRAGA		JAP	4	AO4	X-RAY STUDY ON THE NEAREST SUPERNOVA REMNANT, VELA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504063010/	Quick Look
453	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
454	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
455	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
456	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
457	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
458	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
459	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
460	(L,B)=(-20,0)	276.6688	-11.87	275.969796	-11.90065	276.648122	11.416809	19.56512772	0.0074406	263.6004	56215.5456944444	2012-10-15 13:05:48	56219.7479861111	2012-10-19 17:57:06	507044010	171.8231	200	171.8231	171.8231	0	171.8231	2	2	0	2	1	0	0	147.1192	147.1192	363.0377	4	PROCESSED	57607.9036342593	2016-08-07 21:41:14	56602	2013-11-06 00:00:00	56238.7999884259	2012-11-07 19:11:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070084	We will observe the region at (l,b)=(19.57, 0.0112) to measure spatial and temporal fluctuations of the Galactic Ridge X-ray Emission (GRXE). Measuring these fluctuations is a good test to check the scenarios of point sources and star flare for the GRXE origin. Combined with archival data of XMM-Newton, 200 ks observation of Suzaku makes us able to detect the fluctuations lager than 3% of the GRXE flux. The observation mode of XIS is planed to be a normal clocking mode with no window option.	GALACTIC DIFFUSE EMISSION	5	B	HIDEKI UCHIYAMA		JAP	7	AO7	SUZAKU STUDY OF SPATIAL AND TEMPORAL FLUCTUATIONS IN THE GALACTIC RIDGE X-RAY EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507044010/	Quick Look
461	MCG-6-30-15	203.9795	-34.2919	203.263096	-34.036775	215.177217	-22.538878	313.29805273	27.68293005	295.971	53599.6735300926	2005-08-17 16:09:53	53601.1459027778	2005-08-19 03:30:06	100004010	46.6987	40	46.7009	50.9169	46.6987	46.7254	3	3	3	3	1	0	0	46.4846	46.4846	127.0999	0	PROCESSED	57520.7326388889	2016-05-12 17:35:00	54247	2007-05-27 00:00:00	54035.7991782407	2006-10-27 19:10:49	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000004		CALIBRATION	1	A	SWG		JAP	0	SWG	MCG-60-30-15		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100004010/	Quick Look
462	PSR B1259-63	195.6782	-63.8867	194.888688	-63.618059	227.727553	-50.938083	304.17237227	-1.04211039	282.6534	54290.6852083333	2007-07-09 16:26:42	54291.1876041667	2007-07-10 04:30:09	402014020	19.4817	20	19.4817	19.4817	0	19.4817	2	2	0	2	1	0	0	26.9111	26.9111	43.378	1	PROCESSED	57539.1396759259	2016-05-31 03:21:08	54696	2008-08-18 00:00:00	54328.5032060185	2007-08-16 12:04:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014020/	Quick Look
463	PSR B1259-63	195.6089	-63.8685	194.820162	-63.599771	227.67155	-50.942181	304.14267075	-1.0226082	321.9333	54348.2308449074	2007-09-05 05:32:25	54348.6043287037	2007-09-05 14:30:14	402014080	18.3327	20	18.3407	18.3487	0	18.3327	1	1	0	1	1	0	0	22.3513	22.3513	32.26	0	PROCESSED	57539.9271412037	2016-05-31 22:15:05	54724	2008-09-15 00:00:00	54356.1999537037	2007-09-13 04:47:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014080/	Quick Look
464	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
465	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
466	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
467	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
468	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
469	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
470	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
471	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
472	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
473	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
474	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
475	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
476	HETEJ1900.1-2455	285.0506	-24.9802	284.284146	-25.050704	283.615122	-2.248458	11.25454685	-12.90928139	259.4192	54389.5913425926	2007-10-16 14:11:32	54390.5071064815	2007-10-17 12:10:14	402016010	41.7591	40	41.7788	41.7591	0	41.7751	2	2	0	2	1	0	0	39.9063	39.9063	79.1058	1	PROCESSED	57540.3158564815	2016-06-01 07:34:50	54771	2008-11-01 00:00:00	54403.1292708333	2007-10-30 03:06:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020068	We propose a 40 ks observation of the accreting millisecond pulsar HETE J1900.1-2455, which was discovered by HETE-2 only recently. Good sensitivity in 10-100keV and enough timing resolution of HXD on Suzaku allow us to measure the light curve and the phase resolved spectra of its hard X-ray pulsation, with which we study the physical parameters of the Comptonizing plasma that is considered as the source of the hard X-ray emission of accreting millisecond pulsars. With XIS, we study the radiation from the accretion disk and the neutron star surface, and search for spectral features such as emission lines or absorption edges, which will provide information on the binary environment.	GALACTIC POINT SOURCES	4	B	MOTOKO SUZUKI		JAP	2	AO2	HARD X-RAY PULSATION OF ACCRETION-DRIVEN MILLISECOND PULSAR HETE J1900.1-2455	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402016010/	Quick Look
477	TEVJ2032+4130	308.0461	41.5016	307.599311	41.330897	328.972015	57.41697	80.25613164	1.05964615	221.0839	54451.984212963	2007-12-17 23:37:16	54452.9176157407	2007-12-18 22:01:22	402031010	40.0439	40	40.0439	40.0439	0	40.0439	2	2	0	2	1	0	0	37.3091	37.3091	80.6419	1	PROCESSED	57540.8865625	2016-06-01 21:16:39	54828	2008-12-28 00:00:00	54460.6569675926	2007-12-26 15:46:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020150	Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku.	GALACTIC POINT SOURCES	4	C	SHUNJI KITAMOTO		JAP	2	AO2	STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402031010/	Quick Look
478	RXJ1713.7-3946	258.074	-39.935	257.205787	-39.875387	260.458717	-16.88737	347.05133682	-0.37925502	269.9977	53639.6563194444	2005-09-26 15:45:06	53641.2960648148	2005-09-28 07:06:20	100026010	68.4959	80	68.4959	68.5653	68.5119	68.5253	2	2	2	2	1	0	0	56.2382	56.2382	141.6619	0	PROCESSED	57527.4561921296	2016-05-19 10:56:55	54247	2007-05-27 00:00:00	54037.0750694445	2006-10-29 01:48:06	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000026	RXJ1713 is very important sources in which we can study particle accelerator in the universe. X-ray synchrotron spectrum suggest the existence of distribution of high energy electron. Very similar TeV and ASCA morphologies show close connection between these energy bands. The interaction with molecular cloud suggests that proton accelerator resides in this object. The photon index of RXJ1713 seems to be difficult in the frame work of standard diffusive shock scenario. To obtain precise spectrum in the hard X-ray region is therefore very important to determine the energy cut off and to study the mechanism that produce such high energy electrons.	CALIBRATION	1	A	SWG		JAP	0	SWG	Observation of RXJ1713.7-3946		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100026010/	Quick Look
479	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
480	GC17	267.2896	-29.5968	266.49097	-29.581693	267.620125	-6.178087	359.83441438	-1.00224826	260.2809	54384.0425578704	2007-10-11 01:01:17	54384.480787037	2007-10-11 11:32:20	502005010	20.6035	20	20.6035	20.6035	0	20.6035	2	2	0	2	1	0	0	18.1743	18.1743	37.854	1	PROCESSED	57540.245787037	2016-06-01 05:53:56	54777	2008-11-07 00:00:00	54402.5689583333	2007-10-29 13:39:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020013	We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated.	GALACTIC DIFFUSE EMISSION	5	B	MOTOHIDE KOKUBUN		JAP	2	AO2	HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502005010/	Quick Look
481	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
482	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
483	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
484	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
485	SAGITTARIUS A*	266.4146	-29.0061	265.619899	-28.986758	266.840195	-5.604294	359.94468967	-0.04360372	105.8159	57113.0215162037	2015-04-01 00:30:59	57113.6827662037	2015-04-01 16:23:11	409011050	28.6706	20	28.6706	28.6706	0	28.6866	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.891712963	2016-08-17 21:24:04	56748	2014-04-01 00:00:00	57125.4008796296	2015-04-13 09:37:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090048	With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	9	AO9	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011050/	Quick Look
486	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
487	MARS-P8	103.1682	25.1356	102.40007	25.197197	101.91311	2.237602	190.38738197	11.42154102	298.1062	54559.9031365741	2008-04-03 21:40:31	54560.0072222222	2008-04-04 00:10:24	403006080	2.7489	100	2.7538	2.7578	0	2.7489	2	2	0	2	1	0	0	2.2864	2.2864	8.984	0	PROCESSED	57542.0500578704	2016-06-03 01:12:05	54953	2009-05-02 00:00:00	54577.1637615741	2008-04-21 03:55:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006080/	Quick Look
488	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
489	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
490	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
491	MARS-P20	103.6685	25.0732	102.900981	25.137167	102.37032	2.21732	190.63848879	11.80707935	298.2779	54560.9100347222	2008-04-04 21:50:27	54560.9932175926	2008-04-04 23:50:14	403006200	1.849	100	1.849	1.849	0	1.849	1	1	0	1	1	0	0	1.222	1.222	7.1839	0	PROCESSED	57542.0733101852	2016-06-03 01:45:34	54953	2009-05-02 00:00:00	54578.0575231482	2008-04-22 01:22:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006200/	Quick Look
492	SN1006 NE-Rim	225.9645	-41.7797	225.146779	-41.584709	235.587114	-23.452842	327.82254414	14.6038019	294.6606	53622.1683217593	2005-09-09 04:02:23	53623.5835532407	2005-09-10 14:00:19	100019020	42.8442	50	42.8442	42.8526	42.8522	42.8482	2	2	2	2	1	0	0	37.6156	37.6156	122.196	7	PROCESSED	57527.2923611111	2016-05-19 07:01:00	54247	2007-05-27 00:00:00	54034.9646875	2006-10-26 23:09:09	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000019		CALIBRATION	1	A	SWG		JAP	0	SWG	SN1006 observation with XIS and HXD		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019020/	Quick Look
493	KS1741-293(GCBGD2)	266.2067	-29.3539	265.409831	-29.333545	266.666806	-5.956639	359.55327497	-0.0701996	265.0162	53643.254537037	2005-09-30 06:06:32	53643.3203703704	2005-09-30 07:41:20	100037030	2.97	5	2.994	2.986	2.978	2.97	2	2	2	2	1	0	0	2.8244	2.8244	5.6799	0	PROCESSED	57527.4480439815	2016-05-19 10:45:11	54247	2007-05-27 00:00:00	54035.7774189815	2006-10-27 18:39:29	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000037		CALIBRATION	1	A	SWG		JAP	0	SWG	Suzaku Obseration of Galactic Center region 2		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037030/	Quick Look
494	Sgr_A_East	266.5133	-28.9266	265.719082	-28.907738	266.92496	-5.522692	0.05752244	-0.07594372	264.7159	53643.3215393518	2005-09-30 07:43:01	53644.2648611111	2005-10-01 06:21:24	100037040	42.9176	50	42.9576	42.9616	42.9176	42.9392	2	2	2	2	1	0	0	39.4533	39.4533	81.494	1	PROCESSED	57527.4753356482	2016-05-19 11:24:29	54247	2007-05-27 00:00:00	54035.7619675926	2006-10-27 18:17:14	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000037		CALIBRATION	1	A	SWG		JAP	0	SWG	Suzaku Obseration of Galactic Center region 2		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037040/	Quick Look
495	MARS-P27	103.964	25.0399	103.196825	25.105264	102.640165	2.209619	190.78318678	12.0366945	298.3836	54561.4933217593	2008-04-05 11:50:23	54561.5418171296	2008-04-05 13:00:13	403006270	1.0998	100	1.1078	1.0998	0	1.1158	1	1	0	1	1	0	0	1.0935	1.0935	4.1839	0	PROCESSED	57542.2332175926	2016-06-03 05:35:50	54953	2009-05-02 00:00:00	54578.1251273148	2008-04-22 03:00:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006270/	Quick Look
496	RX J1712.6-2414	258.1492	-24.2444	257.386071	-24.185404	259.195725	-1.246505	359.8664305	8.74215246	94.4586	54889.4875925926	2009-02-27 11:42:08	54892.2710532407	2009-03-02 06:30:19	403021010	110.4813	100	110.4893	110.4813	0	110.4893	2	2	0	2	1	0	0	89.4584	89.4584	240.4418	4	PROCESSED	57545.7503587963	2016-06-06 18:00:31	55330	2010-05-14 00:00:00	54908.5588310185	2009-03-18 13:24:43	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030106	We propose to observe a peculiar Intermediate Polar, RX J1712.6-2414, which has no accretion disk around the white dwarf. This source shows the X-ray modulation only at the beat period and broad Fe-K emission lines in the phase-averaged spectrum. Our goal is to obtain a clear picture about the accretion flow geometry, which can explain the timing and spectral properties, utilizing the fine phase-resolved spectra. Furthermore, we examine the non-thermal emission from the source, since the magnetized white dwarf is a promising candidate of particle acceleration sites.	GALACTIC POINT SOURCES	4	B	HIDEYUKI MORI		JAP	3	AO3	ACCRETION FLOW AND EMISSION MECHANISM OF A DISKLESS INTERMEDIATE POLAR, RX J1712.6-2414	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403021010/	Quick Look
497	HESS J1356-645 2	208.8016	-64.5041	207.885224	-64.258991	235.51443	-48.210014	309.72820731	-2.47708999	123.7329	56340.1852430556	2013-02-17 04:26:45	56341.4863425926	2013-02-18 11:40:20	507020010	51.2594	50	51.2636	51.2594	0	51.2594	2	2	0	2	1	0	0	45.1505	45.1505	112.4059	2	PROCESSED	57610.6176157407	2016-08-10 14:49:22	56718	2014-03-02 00:00:00	56352.5089930556	2013-03-01 12:12:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070017	Recently, pulsar wind nebulae is focused on one of the electron accelerators in our Galaxy. Especially TeV pulsar wind nebulae are supposed to have a largely extended X-ray emission. Since the X-ray emission is much larger than the size considering the typical electron lifetime, high energy electrons strangely seem to be transferred too fast or without cooling. To study the electron diffusion of young pulsar wind nebula, we propose observations of HESS J1356-645, which is off the Galactic plane and is free from the Galactic ridge X-ray emission.	GALACTIC DIFFUSE EMISSION	5	C	TAKAHISA FUJINAGA		JAP	7	AO7	OFF-PLANE TEV GAMMA-RAY SOURCE HESS J1356-645	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507020010/	Quick Look
498	RXJ1713-3946	257.7765	-39.428	256.912609	-39.366986	260.174712	-16.402181	347.32530765	0.10490445	268.0003	53990.7111689815	2006-09-12 17:04:05	53991.0488888889	2006-09-13 01:10:24	501067010	21.1796	20	21.1876	21.1796	21.1931	21.1956	1	1	1	1	1	0	0	21.9861	21.9861	29.1679	0	PROCESSED	57535.5530902778	2016-05-27 13:16:27	54526	2008-03-01 00:00:00	54020.8250925926	2006-10-12 19:48:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501067010/	Quick Look
499	G1.9+0.3	267.1951	-27.1633	266.411742	-27.147772	267.489777	-3.746686	1.87759006	0.32236452	104.4114	55643.1608217593	2011-03-23 03:51:35	55645.2856481482	2011-03-25 06:51:20	505053010	100.9235	100	100.9235	100.9315	0	100.9315	2	2	0	2	1	0	0	83.4251	83.4251	183.5657	1	PROCESSED	57601.3345833333	2016-08-01 08:01:48	56025	2012-04-08 00:00:00	55658.2502546296	2011-04-07 06:00:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050084	We propose to observe the youngest (100yr) SNR G1.9+0.3 with Suzaku for 100 ks. The expected scientific fruits are to reveal the earliest stage of SNR evolution via the time variation of synchrotron emission, and to investigate the nuclear synthesis in the SN explosion via the detection of gamma-ray lines from 44Ti.	GALACTIC DIFFUSE EMISSION	5	A	MOTOHIDE KOKUBUN		JAP	5	AO5	INVESTIGATION OF THE YOUNGEST SNR G1.9+0.3 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505053010/	Quick Look
500	PSR J1429-5911	217.5051	-59.1899	216.584342	-58.967616	237.077372	-41.598198	315.26780851	1.30018252	101.124	55588.2265625	2011-01-27 05:26:15	55588.7001157407	2011-01-27 16:48:10	405012010	30.3824	30	30.3904	30.3984	0	30.3824	1	1	0	1	1	0	0	28.7923	28.7923	40.9039	0	PROCESSED	57600.7562384259	2016-07-31 18:08:59	55968	2012-02-11 00:00:00	55602.1404513889	2011-02-10 03:22:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050047	Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.	GALACTIC POINT SOURCES	4	C	NOBUYUKI KAWAI		JAP	5	AO5	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405012010/	Quick Look
501	BG CMI	112.8488	9.8847	112.163161	9.991257	113.00147	-11.750081	208.51997296	13.31865509	292.793	54932.5078703704	2009-04-11 12:11:20	54933.5710532407	2009-04-12 13:42:19	404029010	47.0791	40	47.0871	47.0791	0	47.0871	1	1	0	1	1	0	0	45.0346	45.0346	91.808	2	PROCESSED	57546.1223958333	2016-06-07 02:56:15	55324	2010-05-08 00:00:00	54949.5279050926	2009-04-28 12:40:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040113	We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.	GALACTIC POINT SOURCES	4	A	TAKAYUKI YUASA		JAP	4	AO4	SURVEY OBSERVATION OF INTERMEDIATE POLARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404029010/	Quick Look
502	XSS J17223-7301	259.6949	-73.4263	258.137466	-73.372744	265.419963	-50.147658	319.10640118	-19.70481928	106.6643	55302.152650463	2010-04-16 03:39:49	55302.5939467593	2010-04-16 14:15:17	405033010	33.3861	30	33.3861	33.3861	0	33.3861	2	2	0	2	1	0	0	25.5889	25.5889	38.1279	0	PROCESSED	57551.2373726852	2016-06-12 05:41:49	55692	2011-05-11 00:00:00	55326.1437731482	2010-05-10 03:27:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050116	Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	5	AO5	QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405033010/	Quick Look
503	AQL X-1	287.8278	0.5718	287.189492	0.488033	289.388601	22.82037	35.71173466	-4.15890942	243.2618	55858.7269328704	2011-10-24 17:26:47	55859.5786921296	2011-10-25 13:53:19	406010030	8.495	40	8.495	9.5383	0	9.5566	1	1	0	1	1	0	0	36.4768	36.4768	73.5819	2	PROCESSED	57603.6460416667	2016-08-03 15:30:18	56241	2012-11-10 00:00:00	55874.1380555556	2011-11-09 03:18:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060036	We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object.	GALACTIC POINT SOURCES	4	A	KAZUTAKA YAMAOKA		JAP	6	AO6-TOO	SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406010030/	Quick Look
504	OAO1657-415	255.2026	-41.6667	254.323073	-41.593508	258.36169	-18.820662	344.36019061	0.31327103	285.9012	55830.3988425926	2011-09-26 09:34:20	55832.6667939815	2011-09-28 16:00:11	406011010	84.7299	80	84.7337	84.7299	0	84.7417	2	2	0	2	1	0	0	74.5885	74.5885	195.9297	2	PROCESSED	57603.3220023148	2016-08-03 07:43:41	56226	2012-10-26 00:00:00	55858.2768518518	2011-10-24 06:38:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060037	We propose Suzaku observation of accretion-powered pulsar OAO 1657-415 to study matter accretion onto the neutron star. This object is a unique high mass X-ray binary (HMXB) that shows intermediate characteristics between wind-fed accretion pulsars and disk-fed accretion pulsars. High S/N spectra obtained by XIS, HXD-PIN/GSO with short exposure time (1 ks) allow us to investigate short-time variability of physical states of the accretion column, which is close to the neutron star surface. The proposed observation also reveals the matter distribution in the HMXB by using a 6.4-keV iron fluorescence line and hard X-rays. The data at the phase of eclipse egress provide essential information about the stellar wind and atmosphere of the companion star to constrain its stellar type in question.	GALACTIC POINT SOURCES	4	B	HIROKAZU ODAKA		JAP	6	AO6	WIDE-BAND X-RAY OBSERVATION OF HIGH MASS X-RAY BINARY PULSAR OAO 1657-415	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406011010/	Quick Look
505	GC SOUTH	266.5016	-29.1694	265.705845	-29.150477	266.920624	-5.765664	359.84485124	-0.1935349	265.0006	54004.5960185185	2006-09-26 14:18:16	54007.8925231482	2006-09-29 21:25:14	501008010	129.5773	130	129.5773	129.5773	129.5773	129.5773	2	2	2	2	1	0	0	111.2591	111.2591	284.8038	5	PROCESSED	57535.7712731482	2016-05-27 18:30:38	54744	2008-10-05 00:00:00	54021.0929050926	2006-10-13 02:13:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010044	Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	1	AO1	SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501008010/	Quick Look
506	HESS J1745-303	266.2629	-30.3722	265.459457	-30.352101	266.742769	-6.973282	358.71029443	-0.64354718	263.6011	54015.0950462963	2006-10-07 02:16:52	54016.4300810185	2006-10-08 10:19:19	501010010	50.6707	50	50.6707	50.6707	50.6707	50.6707	1	1	1	1	1	0	0	45.6897	45.6897	115.3119	1	PROCESSED	57535.8009837963	2016-05-27 19:13:25	54526	2008-03-01 00:00:00	54021.698587963	2006-10-13 16:45:58	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010046	So far, the evidence for hadron acceleration up to near the knee energy has not yet obtained. Recent galactic plane survey in the TeV gamma-ray band reveals several new unidentified sources like HESS J1745-303. It is extended, hence likely a supernova remnant. Also it coincides with an EGRET unidentified source (3EG J1744-3011), which may suggest that it is a source of accelerated protons. However, HESS J1745-303 shows rather hard spectrum that cannot be explained by the simplest version of the diffusive shock acceleration model. X-ray study on HESS J1745-303 is necessary for further discussions. We might find that observed data requires modification of the common picture that young supernova remnants are the dominant source of high-energy protons.	GALACTIC DIFFUSE EMISSION	5	A	RYO YAMAZAKI		JAP	1	AO1	X-RAY STUDY ON THE TEV UNIDENTIFIED SOURCE HESS J1745-303	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501010010/	Quick Look
507	1RXSJ175911.0-344921	269.7922	-34.8194	268.957803	-34.816359	269.8163	-11.378443	356.38251758	-5.46102238	72.1205	55993.9029513889	2012-03-07 21:40:15	55994.912650463	2012-03-08 21:54:13	406019010	40.1813	40	40.1813	40.1813	0	40.1813	2	2	0	2	1	0	0	34.751	34.751	87.2339	1	PROCESSED	57604.8358564815	2016-08-04 20:03:38	56385	2013-04-03 00:00:00	56016.6680787037	2012-03-30 16:02:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060085	We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test accretion disk theories at intermediate mass accretion rates.	GALACTIC POINT SOURCES	4	C	HIDEYUKI MORI		JAP	6	AO6	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406019010/	Quick Look
508	PSR B1259-63	195.6777	-63.8873	194.888189	-63.618658	227.727854	-50.938694	304.1721261	-1.04270018	282.6527	54292.6291319444	2007-07-11 15:05:57	54293.1910763889	2007-07-12 04:35:09	402014030	22.7217	20	22.7217	22.7217	0	22.7217	2	2	0	2	1	0	0	24.2808	24.2808	48.5459	0	PROCESSED	57539.1606712963	2016-05-31 03:51:22	54707	2008-08-29 00:00:00	54339.0273842593	2007-08-27 00:39:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014030/	Quick Look
509	CYGNUS_LOOP_P7	312.0838	30.7678	311.566097	30.58216	326.462182	46.307536	73.70103145	-8.0534172	239.9966	54416.1673032407	2007-11-12 04:00:55	54416.7223263889	2007-11-12 17:20:09	501018010	24.1545	22	24.1545	24.1545	0	24.1545	2	2	0	2	1	0	0	18.861	18.861	47.92	0	PROCESSED	57540.4878587963	2016-06-01 11:42:31	54798	2008-11-28 00:00:00	54430.1343287037	2007-11-26 03:13:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501018010/	Quick Look
510	1RXSJ165256.3-264503	253.236	-26.7533	252.46137	-26.671186	255.025143	-4.179065	355.1420085	10.81079439	277.5876	54337.0024421296	2007-08-25 00:03:31	54338.0419444444	2007-08-26 01:00:24	402004010	49.5822	40	49.5822	49.5822	0	49.5822	2	2	0	2	1	0	0	46.6581	46.6581	89.7779	2	PROCESSED	57539.6777083333	2016-05-31 16:15:54	54723	2008-09-14 00:00:00	54350.4155092593	2007-09-07 09:58:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020015	We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, which were detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the Suzaku fine spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test acrretion disk theories at intermediate mass accretion rates.	GALACTIC POINT SOURCES	4	C	HIDEYUKI MORI		JAP	2	AO2	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402004010/	Quick Look
511	PSR B1259-63	195.6402	-63.8787	194.8511	-63.61001	227.698758	-50.941899	304.15600524	-1.03339065	289.9992	54315.2640856482	2007-08-03 06:20:17	54316.0419444444	2007-08-04 01:00:24	402014060	24.0388	20	24.0388	24.0388	0	24.0388	2	2	0	2	1	0	0	21.5808	21.5808	67.1959	1	PROCESSED	57539.3969675926	2016-05-31 09:31:38	54722	2008-09-13 00:00:00	54347.6946527778	2007-09-04 16:40:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020059	We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		JAP	2	AO2	THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014060/	Quick Look
512	HESS J1825-137	276.5031	-13.6997	275.794781	-13.729527	276.397624	9.596588	17.87105596	-0.70261201	269.3213	54025.8175462963	2006-10-17 19:37:16	54027.1682291667	2006-10-19 04:02:15	501044010	50.293	50	50.293	50.293	50.293	50.293	2	2	2	2	1	0	0	42.9557	42.9557	116.694	1	PROCESSED	57535.8789351852	2016-05-27 21:05:40	54526	2008-03-01 00:00:00	54055.4418634259	2006-11-16 10:36:17	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010073	We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	1	AO1	SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501044010/	Quick Look
513	RXJ1713-3946	257.7744	-39.7271	256.908127	-39.666071	260.20044	-16.700257	347.08325974	-0.07081205	268.0001	53990.3113310185	2006-09-12 07:28:19	53990.7106944444	2006-09-12 17:03:24	501066010	20.9207	20	20.9407	20.9207	20.926	20.9447	2	2	2	2	1	0	0	20.699	20.699	34.504	1	PROCESSED	57535.5600347222	2016-05-27 13:26:27	54526	2008-03-01 00:00:00	54020.8077546296	2006-10-12 19:23:10	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501066010/	Quick Look
514	GALACTIC CENTER	265.5037	-30.2156	264.701457	-30.191826	266.078204	-6.8356	358.49956421	-0.00336241	269.0005	54018.2813541667	2006-10-10 06:45:09	54018.887662037	2006-10-10 21:18:14	501052010	19.2451	20	19.2611	19.2611	19.2531	19.2451	2	2	2	2	1	0	0	16.0462	16.0462	52.3799	1	PROCESSED	57535.818275463	2016-05-27 19:38:19	54735	2008-09-26 00:00:00	54053.5074537037	2006-11-14 12:10:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501052010/	Quick Look
515	H1743-322	266.5662	-32.2338	265.750329	-32.21514	267.05149	-8.827747	357.25541352	-1.83396197	273.6881	56210.6462268518	2012-10-10 15:30:34	56211.5862731482	2012-10-11 14:04:14	407005020	21.1922	40	21.1922	21.1922	0	21.1922	3	2	0	2	1	0	0	41.517	41.517	81.2159	2	PROCESSED	57607.7447337963	2016-08-07 17:52:25	56595	2013-10-30 00:00:00	56226.5882291667	2012-10-26 14:07:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070002	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	7	AO7-TOO	MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407005020/	Quick Look
516	XTE J1855-206	283.8765	-2.601	283.223287	-2.666237	284.773693	20.130658	31.07954127	-2.09022498	75.074	57134.7127199074	2015-04-22 17:06:19	57137.3453125	2015-04-25 08:17:15	409022010	87.725	90	87.725	89.3274	0	89.3194	3	3	0	3	0	0	0	0	0	0	0	PROCESSED	57618.1026157407	2016-08-18 02:27:46	57593	2016-07-24 00:00:00	57224.4343171296	2015-07-21 10:25:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090101	Most of High mass X-ray binaries (HMXBs) have strong magnetic fields (~10^12 G) and detected cyclotron resonance scattering features (CRSFs). Many HMXBs with CRSFs have been observed by Suzaku and we derived a new method for estimating magnetic field strength using the observational data. In this observation, we try to observe candidates of strongly magnetized neutron star in HMXBs, EXO 1722-363 and XTE J1855-206 and examine the method.	GALACTIC POINT SOURCES	4	C	MAKOTO SASANO		JAP	9	AO9	EXAMINATION OF A NEW METHOD FOR ESTIMATING MAGNETIC FIELD STRENGTH WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409022010/	Quick Look
517	SWIFT J0601.9-8636	91.1523	-86.6779	95.292028	-86.662252	269.78546	-69.879444	299.2555588	-27.75439578	292.1727	53838.6834259259	2006-04-13 16:24:08	53839.0779976852	2006-04-14 01:52:19	701018010	19.7657	20	19.7817	19.7817	19.7657	19.7737	2	2	2	2	1	0	0	16.6614	16.6614	34.0599	0	PROCESSED	57533.4511226852	2016-05-25 10:49:37	54397	2007-10-24 00:00:00	53905.4682060185	2006-06-19 11:14:13	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010133	Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background".	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	1	AO1	DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701018010/	Quick Look
518	HEN 3-461	159.7779	-51.4088	159.258813	-51.147936	190.933881	-53.401362	282.90269516	6.2428626	116.1715	56278.1336342593	2012-12-17 03:12:26	56278.906400463	2012-12-17 21:45:13	407007010	45.7348	40	45.7348	45.7348	0	45.7348	2	2	0	2	1	0	0	46.6774	46.6774	66.7619	0	PROCESSED	57608.3071990741	2016-08-08 07:22:22	56018	2012-04-01 00:00:00	56303.5505902778	2013-01-11 13:12:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070021	Hard X-ray emitting symbiotic stars have been identified to emit 6.4 keV iron line with similar equivalent width of the 6.4 keV line of the Galactic Ridge X-ray Emission (GRXE). Only four of such hard X-ray emitting symbiotic stars have been observed with Suzaku. We propose to use Suzaku observations of all the eight newly discovered hard X-ray emitting symbiotic stars to ascertain if they have similar equivalent width of the 6.4 keV line of the GRXE. We will also confirm the emission of hard X-rays above 10 keV using the HXD PIN and use this feature to test for non-thermal emission in these objects.	GALACTIC POINT SOURCES	4	C	ROMANUS EZE		JAP	7	AO7	SEARCH FOR 6.4 KEV IRON EMISSION LINE IN THE NEWLY DISCOVERED HARD X-RAY EMITTING SYMBIOTIC STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407007010/	Quick Look
519	AX J1622.1-5005	245.5334	-50.0932	244.591386	-49.975777	252.45498	-28.129926	333.60606211	-0.20489946	274.3812	56160.9968402778	2012-08-21 23:55:27	56161.9398148148	2012-08-22 22:33:20	407018010	39.1263	40	40.5366	40.5366	0	39.1263	2	2	0	2	1	0	0	37.476	37.476	81.4619	0	PROCESSED	57606.9317824074	2016-08-06 22:21:46	56667	2014-01-10 00:00:00	56300.5637731482	2013-01-08 13:31:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070043	Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution.	GALACTIC POINT SOURCES	4	A	KAZUO MAKISHIMA		JAP	7	AO7	ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407018010/	Quick Look
520	GX 339-4	255.7293	-48.7348	254.78204	-48.663918	259.585808	-25.807191	338.99236079	-4.30539701	107.9544	54915.3430555556	2009-03-25 08:14:00	54916.2711111111	2009-03-26 06:30:24	403011020	39.0792	40	39.1165	39.0792	0	39.1165	1	1	0	1	1	0	0	34.7852	34.7852	80.1658	0	PROCESSED	57545.909849537	2016-06-06 21:50:11	55330	2010-05-14 00:00:00	54930.1609490741	2009-04-09 03:51:46	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030046	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	3	AO3-TOO	MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403011020/	Quick Look
521	H1743-322	266.5676	-32.2352	265.751719	-32.216547	267.052722	-8.829118	357.25483145	-1.83570092	273.6877	56204.7822800926	2012-10-04 18:46:29	56205.6078240741	2012-10-05 14:35:16	407005010	20.811	40	20.811	20.811	0	20.811	2	2	0	2	1	0	0	42.4337	42.4337	71.3219	0	PROCESSED	57607.2960300926	2016-08-07 07:06:17	56595	2013-10-30 00:00:00	56226.5596296296	2012-10-26 13:25:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070002	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	7	AO7-TOO	MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407005010/	Quick Look
522	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
523	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
524	MARS-P5	103.045	25.1496	102.276729	25.210613	101.800688	2.241477	190.32670814	11.32616716	298.0638	54559.6600462963	2008-04-03 15:50:28	54559.7432407407	2008-04-03 17:50:16	403006050	1.9562	100	1.9562	1.9562	0	1.9562	2	2	0	2	1	0	0	1.9926	1.9926	7.1679	0	PROCESSED	57542.0421527778	2016-06-03 01:00:42	54953	2009-05-02 00:00:00	54577.1345486111	2008-04-21 03:13:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006050/	Quick Look
525	MARS-P9	103.2195	25.1275	102.451442	25.18934	101.960133	2.233755	190.41473742	11.46031922	298.1247	54560.0073726852	2008-04-04 00:10:37	54560.0766666667	2008-04-04 01:50:24	403006090	2.1506	100	2.1506	2.1746	0	2.1506	1	1	0	1	1	0	0	1.8919	1.8919	5.9759	0	PROCESSED	57542.0488888889	2016-06-03 01:10:24	54953	2009-05-02 00:00:00	54577.1428009259	2008-04-21 03:25:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006090/	Quick Look
526	V4641 SGR	274.8371	-25.4052	274.064433	-25.426808	274.361493	-2.037678	6.77442002	-4.78571714	84.0004	56741.9737152778	2014-03-25 23:22:09	56744.8959722222	2014-03-28 21:30:12	408002010	49.2237	100	49.2237	49.2706	0	49.2242	3	3	0	3	1	0	0	89.7439	89.7439	252.4556	1	PROCESSED	57614.1632291667	2016-08-14 03:55:03	57190	2015-06-17 00:00:00	56821.8685532407	2014-06-13 20:50:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080009	We propose a 100 ksec Suzaku observation of the Galactic microquasar V4641 Sgr in an outburst. V4641 Sgr has many unique charactersitics: 1)giant X-ray outbursts with fast rise and decay times, 2)violent variability in X-ray and optical bands, and 3)remarkable iron-K disk-line profiles in the X-ray spectrum. However, it is hardly understood due to the poor X-ray coverage which results from its short outburst duration and rapid intensity variations. Hence, we collaborate closely with VSNET, MAXI/GSC, Swift/XRT and Swift/BAT team for a rapid trigger. The moderate energy resolution and wideband energy coverage of Suzaku enable us to clarify the radiation mechanisms of V4641 Sgr. This observation is now planned simultaneously with Swift, many radio and optical/NIR observatories.	GALACTIC POINT SOURCES	4	A	KAZUTAKA YAMAOKA		JAP	8	AO8-TOO	THE LARGEST-EVER CAMPAIGN OF THE GALACTIC MICROQUASAR V4641 SGR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408002010/	Quick Look
527	MARS-P14	103.4188	25.1057	102.650967	25.168485	102.141964	2.228596	190.5119865	11.61511049	298.1941	54560.410150463	2008-04-04 09:50:37	54560.4933333333	2008-04-04 11:50:24	403006140	4.8252	100	4.8492	4.8252	0	4.8572	1	1	0	1	1	0	0	3.7214	3.7214	7.1759	0	PROCESSED	57542.063125	2016-06-03 01:30:54	54953	2009-05-02 00:00:00	54577.9434722222	2008-04-21 22:38:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006140/	Quick Look
528	VELA JR P9	133.4161	-45.7633	132.983285	-45.572688	159.43463	-59.191033	266.00615013	-0.63304204	347.0009	54287.7015856482	2007-07-06 16:50:17	54287.9516666667	2007-07-06 22:50:24	502031010	13.2524	10	13.2684	13.2524	0	13.2684	1	1	0	1	1	0	0	9.8877	9.8877	21.5999	0	PROCESSED	57539.1152546296	2016-05-31 02:45:58	54703	2008-08-25 00:00:00	54333.4413657407	2007-08-21 10:35:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502031010/	Quick Look
529	VELA JR P5	132.9105	-45.488	132.477402	-45.299188	158.564821	-59.145564	265.56829981	-0.72857938	347.002	54286.4486458333	2007-07-05 10:46:03	54286.7502777778	2007-07-05 18:00:24	502027010	10.977	10	10.977	10.977	0	10.977	1	1	0	1	1	0	0	10.7858	10.7858	26.0539	0	PROCESSED	57539.1013541667	2016-05-31 02:25:57	54696	2008-08-18 00:00:00	54328.4697800926	2007-08-16 11:16:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502027010/	Quick Look
530	VELA JR P12	132.2515	-46.051	131.824752	-45.864543	158.385677	-59.866647	265.71195175	-1.4410688	347.0011	54289.0722106482	2007-07-08 01:43:59	54289.4078009259	2007-07-08 09:47:14	502034010	9.9479	10	9.9479	9.9479	0	9.9479	1	1	0	1	1	0	0	10.494	10.494	28.9839	0	PROCESSED	57539.1227546296	2016-05-31 02:56:46	54696	2008-08-18 00:00:00	54328.4792939815	2007-08-16 11:30:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502034010/	Quick Look
531	HE FOCUSING CONE	49.5833	10.9603	48.902196	10.778547	50.105188	-7.060313	170.9618047	-37.8533007	73.6953	55410.7011921296	2010-08-02 16:49:43	55413.1439699074	2010-08-05 03:27:19	505061010	101.9651	100	101.9731	101.9731	0	101.9651	2	2	0	2	1	0	0	89.1452	89.1452	211.0459	2	PROCESSED	57552.9158796296	2016-06-13 21:58:52	55808	2011-09-04 00:00:00	55441.4075694444	2010-09-02 09:46:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050129	We propose the observation though the Helium Focusng Cone. This region seems to make the strong enhancement of Solarwind Charge exchange and cause the annual variation of it. We develop the best observation of the cone by using the area where the abosorption by molecular cloud is huge. By this observation, we investigate the mistery of the emission of Our Galaxy.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI YOSHITAKE		JAP	5	AO5	OBSERVATION THROUGH THE HELIUM FOCUSING CONE: SEARCH FOR THE VARIABILITY OF THE HELIOSPHERIC SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505061010/	Quick Look
532	MARS-P22	103.7541	25.0677	102.986656	25.132072	102.448087	2.219161	190.67657625	11.87528798	298.3117	54561.0767013889	2008-04-05 01:50:27	54561.1598842593	2008-04-05 03:50:14	403006220	4.0246	100	4.0406	4.0246	0	4.0476	1	1	0	1	1	0	0	4.102	4.102	7.1839	0	PROCESSED	57542.0781712963	2016-06-03 01:52:34	54953	2009-05-02 00:00:00	54578.0665625	2008-04-22 01:35:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030015	We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.	GALACTIC POINT SOURCES	4	A	YUICHIRO EZOE		JAP	3	AO3	SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006220/	Quick Look
533	4U 0614+091	94.2826	9.1348	93.597318	9.153924	94.364565	-14.241394	200.88027144	-3.36263018	270.7227	56737.0982291667	2014-03-21 02:21:27	56738.4584259259	2014-03-22 11:00:08	408009020	15.6689	60	15.8314	15.6689	0	15.8205	4	3	0	3	1	0	0	60.5574	60.5574	117.5018	2	PROCESSED	57614.0787152778	2016-08-14 01:53:21	57144	2015-05-02 00:00:00	56778.6809606482	2014-05-01 16:20:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080028	We propose an Suzaku observation of LMXB 4U 0614+091 for the study of Neutron Star Binary (NSB) in the low/hard state. An aim of this observation is to reveal a physical model of the NSB low/hard state in a same analogy of Black-Hole Binary (BHB) low/hard state. In the BHB Cyg X-1, the spectra in low/hard state radiate from a cool accretion disk and a hot comptonizing corona. A spectra of NS in low/hard state would have the same structure as Cyg X-1, but it is hard to study the fine structure of the spectra because of low luminosity. Suzaku can determine the low temperature of the disk and the high temperature of the corona, thanks to wide-band and high sensitivity detectors: XIS/BI and HXD. This observation is important for an unified model between BHB and NSB.	GALACTIC POINT SOURCES	4	B	SATOSHI SUGITA		JAP	8	AO8	THE SPECTRAL STUDY OF LMXB 4U 0614+091 IN THE LOW/HARD STATE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408009020/	Quick Look
534	VELA JR P17	133.087	-46.0455	132.657371	-45.856052	159.351353	-59.55196	266.0760896	-0.98967894	347.0002	54291.7369444444	2007-07-10 17:41:12	54291.9238773148	2007-07-10 22:10:23	502039010	13.0326	10	13.0645	13.0646	0	13.0326	1	1	0	1	1	0	0	8.8272	8.8272	16.1439	0	PROCESSED	57539.1455555556	2016-05-31 03:29:36	54707	2008-08-29 00:00:00	54333.4040277778	2007-08-21 09:41:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502039010/	Quick Look
535	HESS J0632+057	98.2456	5.8062	97.576893	5.844512	98.600946	-17.388931	205.66072349	-1.43796588	289.8173	54579.6856828704	2008-04-23 16:27:23	54580.6877199074	2008-04-24 16:30:19	403018010	44.076	40	44.076	44.076	0	44.076	2	2	0	2	1	0	0	41.4758	41.4758	86.5658	0	PROCESSED	57542.3746643518	2016-06-03 08:59:31	54961	2009-05-10 00:00:00	54594.1596990741	2008-05-08 03:49:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030080	We propose a 40 ks observation on HESS J0632+057, the newly discovered TeV gamma-ray source in the interacting region of Monoceros SNR and Rosette Nebula. Although this point-like source is found inside the error circle of an unidentified EGRET source 3EG J0634+0521, it has no clear counterpart at other wavelengths. Two sources, a weak X-ray source 1RXS J063258.3+05487 and a Be-star MCW 148, are found inside the error circle of HESS. The aim of the Suzaku observation is to obtain a clue to solve the yet feasible three scenarios of the TeV gamma-ray source.	GALACTIC POINT SOURCES	4	A	MOTOHIDE KOKUBUN		JAP	3	AO3	INVESTIGATION ON HESS J0632+057 IN MONOCEROS/ROSETTE REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403018010/	Quick Look
536	GC_G0.9+0.1	266.9332	-28.1474	266.1438	-28.130586	267.277369	-4.735296	0.91503767	0.01290063	105.8953	54536.2637152778	2008-03-11 06:19:45	54540.229375	2008-03-15 05:30:18	502051010	138.7614	133	138.7614	138.7614	0	138.7614	2	2	0	2	1	0	0	122.2214	122.2214	342.5768	1	PROCESSED	57541.9299305556	2016-06-02 22:19:06	54919	2009-03-29 00:00:00	54550.6988078704	2008-03-25 16:46:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020071	The Suzaku PV observations found that the diffuse X-rays (6.7 and 6.9 keV-lines) from the GC region can well be explained by a thermal emission from hot plasma (6-7 keV). The most plausible energy injection source is multiple SNe. The huge thermal energy (10^54 ergs) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm this scenario, we propose to observe the shell of G0.9+0.1 and the connecting region of Sgr B and D. The first objective is to detect a thermal emission from the shell of G0.9+0.1 and the second is to discover new SNRs.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	2	AO2	SNR G0.9+0.1 AND THE CONNECTING REGION OF SGR B AND D	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502051010/	Quick Look
537	SAGITTARIUS A*	266.4166	-29.0014	265.621928	-28.982068	266.841834	-5.599552	359.94961276	-0.04264831	285.0058	56547.2597337963	2013-09-12 06:14:01	56547.6558101852	2013-09-12 15:44:22	408017020	19.276	20	19.2823	19.2901	0	19.276	3	3	0	3	1	0	0	21.0834	21.0834	34.218	0	PROCESSED	57612.6033796296	2016-08-12 14:28:52	56956	2014-10-26 00:00:00	56588.7462152778	2013-10-23 17:54:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017020/	Quick Look
538	M17 EAST	275.3895	-16.2062	274.668063	-16.230609	275.205572	7.137102	15.15230897	-0.92571433	271.9996	54377.3569907407	2007-10-04 08:34:04	54380.0940277778	2007-10-07 02:15:24	502052010	114.5695	107	114.5775	114.5695	0	114.5775	2	2	0	2	1	0	0	100.8873	100.8873	236.4498	3	PROCESSED	57540.2317939815	2016-06-01 05:33:47	54771	2008-11-01 00:00:00	54403.5436111111	2007-10-30 13:02:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020085	We continue our XIS study of the soft extended X-ray emission in M17. The first study conducted in a region close to the OB association brought a detailed surface brightness distribution and the highest S/N ratio spectrum of the diffuse emission. In this proposed study, we move our eyes to the west to observe another bright emission outside of the previously studied regions. DSS and ROSAT all-sky survey images suggest that this is a shocked region, in which OB stellar winds impinge upon ISM. We aim to obtain the surface brightness map of this region and measure the plasma temperature difference in and out of the possible shocked region.	GALACTIC DIFFUSE EMISSION	5	A	MASAHIRO TSUJIMOTO		JAP	2	AO2	FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS -	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502052010/	Quick Look
539	VELA JR P32	133.3695	-46.8865	132.945153	-46.696038	160.585523	-60.152729	266.8467839	-1.37881435	347.0018	54655.3279166667	2008-07-08 07:52:12	54655.5648032407	2008-07-08 13:33:19	503044010	11.2649	10	11.2729	11.2649	0	11.2809	1	1	0	1	1	0	0	8.3375	8.3375	20.4559	0	PROCESSED	57543.0006828704	2016-06-04 00:00:59	55048	2009-08-05 00:00:00	54679.381087963	2008-08-01 09:08:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503044010/	Quick Look
540	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
541	ETA CARINAE	161.1825	-59.711	160.696763	-59.447791	202.133764	-58.970475	287.57247158	-0.67238651	329.3001	56476.1821296296	2013-07-03 04:22:16	56479.0417361111	2013-07-06 01:00:06	408018010	97.524	180	97.524	97.524	0	97.524	2	2	0	2	1	0	0	87.8367	87.8367	247.0497	2	PROCESSED	57611.768912037	2016-08-11 18:27:14	56861	2014-07-23 00:00:00	56492.7286921296	2013-07-19 17:29:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080081	Eta Carinae is a binary system containing two very massive main sequence stars orbiting with a period of 5.5 years. As reported by Sekiguchi et al. 2009 and Reitberger et al. 2012 based on Suzaku and Fermi data respectively, the system shows intense non-thermal emission extending from 20 keV to 200 GeV. Although detailed mechanism of this non-thermal emission has been clarified yet, it is now obvious that electrons and highly probably protons are accelerated to high energies by the collision of stellar winds. The aim of the present observation is to measure the spectral shape and flux of the non-thermal hard X-ray tail with the HXD, and compare with previous Suzaku observations. Based on a time variability (or non-variability), we examine proposed acceleration and emission mechanisms.	GALACTIC POINT SOURCES	4	B	TAKAYUKI YUASA		JAP	8	AO8	DETAILED SPECTROSCOPY OF NON-THERMAL HARD X-RAY EMISSION OF ETA CARINAE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408018010/	Quick Look
542	V2301 OPH	270.155	8.1565	269.554142	8.157196	270.169577	31.596745	34.53366867	14.97765204	262.0679	56576.0003009259	2013-10-11 00:00:26	56577.3452314815	2013-10-12 08:17:08	408024020	53.1884	110	53.1884	53.1884	0	53.1884	2	2	0	2	1	0	0	47.2892	47.2892	116.1898	0	PROCESSED	57612.9583333333	2016-08-12 23:00:00	57184	2015-06-11 00:00:00	56631.6754282407	2013-12-05 16:12:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080107	It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion.	GALACTIC POINT SOURCES	4	A	TAKAYUKI HAYASHI		JAP	8	AO8	MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408024020/	Quick Look
543	V2301 OPH	270.1437	8.1764	269.542941	8.17715	270.156471	31.616658	34.54710657	14.99643028	71.9008	56752.9922800926	2014-04-05 23:48:53	56754.6945949074	2014-04-07 16:40:13	408024030	62.9253	57	62.9413	62.9253	0	62.9413	2	2	0	2	1	0	0	56.5037	56.5037	147.0677	1	PROCESSED	57614.2091666667	2016-08-14 05:01:12	57184	2015-06-11 00:00:00	56817.8149884259	2014-06-09 19:33:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080107	It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion.	GALACTIC POINT SOURCES	4	A	TAKAYUKI HAYASHI		JAP	8	AO8	MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408024030/	Quick Look
544	WR140	305.1942	43.809	304.771615	43.649401	327.418451	60.430238	80.92425741	4.10518752	220.5408	54812.4360069444	2008-12-12 10:27:51	54813.5523148148	2008-12-13 13:15:20	403032010	52.9106	40	52.9106	52.9106	0	52.9106	3	3	0	3	1	0	0	48.2609	48.2609	96.4318	0	PROCESSED	57544.9612847222	2016-06-05 23:04:15	55192	2009-12-27 00:00:00	54826.2481365741	2008-12-26 05:57:19	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030157	WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	3	AO3	X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403032010/	Quick Look
545	X 1630-472	248.5011	-47.3955	247.580071	-47.291357	254.086008	-25.133666	336.90685721	0.25132488	88.6334	57080.103125	2015-02-27 02:28:30	57081.1542824074	2015-02-28 03:42:10	409007030	5.1108	40	5.128	5.1452	0	5.1108	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.7393634259	2016-08-17 17:44:41	57458	2016-03-11 00:00:00	57091.4579513889	2015-03-10 10:59:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090015	Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.	GALACTIC POINT SOURCES	4	A	YOSHIHIRO UEDA		JAP	9	AO9-TOO	MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409007030/	Quick Look
546	SAGITTARIUS A*	266.415	-29.0091	265.620279	-28.98976	266.840621	-5.607284	359.94231116	-0.0454652	105.8502	57103.3174537037	2015-03-22 07:37:08	57103.7690162037	2015-03-22 18:27:23	409011040	23.2422	20	23.2422	23.2465	0	23.2465	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.8342824074	2016-08-17 20:01:22	56748	2014-04-01 00:00:00	57114.6078472222	2015-04-02 14:35:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090048	With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	9	AO9	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011040/	Quick Look
547	1RXSJ013106.4+612035	22.7619	61.3591	21.928492	61.101677	49.598028	47.010357	127.66105316	-1.14841945	76.8129	55765.7032175926	2011-07-23 16:52:38	55766.0182060185	2011-07-24 00:26:13	406034010	13.2963	20	13.2963	13.2963	0	13.2963	1	1	0	1	1	0	0	15.8829	15.8829	27.1999	0	PROCESSED	57602.6424884259	2016-08-02 15:25:11	56374	2013-03-23 00:00:00	55784.9886458333	2011-08-11 23:43:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060097	We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray.	GALACTIC POINT SOURCES	4	B	HIROMITSU TAKAHASHI		JAP	6	AO6	SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406034010/	Quick Look
548	1RXSJ173916.2-214746	264.8155	-21.7912	264.064028	-21.764222	265.175612	1.563021	5.33311568	4.97377326	96.7097	57115.0060069444	2015-04-03 00:08:39	57115.2681712963	2015-04-03 06:26:10	409015010	12.328	12	12.349	12.3523	0	12.328	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8972800926	2016-08-17 21:32:05	57493	2016-04-15 00:00:00	57126.415625	2015-04-14 09:58:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090051	We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	B	HIDEYUKI MORI		JAP	9	AO9	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409015010/	Quick Look
549	UX ARIETIS	51.6466	28.6421	50.887812	28.467932	56.479497	9.555722	159.59610539	-22.97107378	272.6966	55229.7116666667	2010-02-02 17:04:48	55231.7321064815	2010-02-04 17:34:14	404008010	87.7993	90	87.7993	87.7993	0	87.7993	2	2	0	2	1	0	0	79.7429	79.7429	174.5399	0	PROCESSED	57550.5166203704	2016-06-11 12:23:56	55616	2011-02-24 00:00:00	55249.830150463	2010-02-22 19:55:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040036	We propose a hard X-ray observation of RS CVn-type active binary UX Arietis. Detection of nonthermal hard X-ray radiation is essentially important to solve the generation mechanism of stellar flares. UX Ari has a high coronal activity with a high temperature of ~2keV, and large stellar flares were frequently observed in the radio, UV, and X-ray band. Therefore, UX Ari is very suitable for hard X-ray observation of stellar flares. Large X-ray flares were observed by BeppoSAX, ASCA and Ginga sattellite, and hard X-ray emission upto ~50keV is detected by BeppoSAX. If a flare is large such as the events of former X-ray observations, we can detect the nonthermal hard X-ray emssion by Suzaku HXD.	GALACTIC POINT SOURCES	4	C	SHIN-NOSUKE ISHIKAWA		JAP	4	AO4	STUDY ON GENERATION MECHANISM OF STELLAR FLARES BY HARD X-RAY OBSERVATION OF ACTIVE BINARY UX ARIETIS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404008010/	Quick Look
550	HESS J0632+057	98.2448	5.8057	97.576095	5.844008	98.600145	-17.389477	205.66080027	-1.43890266	289.9631	54941.5631944444	2009-04-20 13:31:00	54944.1542708333	2009-04-23 03:42:09	404027010	100.0343	100	100.0343	100.0343	0	100.0343	2	2	0	2	1	0	0	82.3918	82.3918	223.8419	6	PROCESSED	57546.2406481482	2016-06-07 05:46:32	55336	2010-05-20 00:00:00	54966.5323958333	2009-05-15 12:46:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040102	We propose a coordinate observation of HESS J0632+057 with Suzaku and VLA. This source is recently discovered as a fourth gamma-ray binary with HESS and XMM-Newton, and our results obtained in Suzaku AO-3 also confirmed a gradual variety of X-ray intensity, possibly associated with the binary period. With a combined observation with VLA, we will for the first time obtain a "real-time" variety from both of image and spectrum of this interesting source.	GALACTIC POINT SOURCES	4	A	MOTOHIDE KOKUBUN		JAP	4	AO4	SIMULTANEOUS OBSERVATION OF HESS J0632+057 WITH SUZAKU AND VLA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404027010/	Quick Look
551	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
552	GC_LARGEPROJECT6	266.2992	-29.9408	265.498546	-29.920884	266.763082	-6.541223	359.09468885	-0.44519015	265.9621	54723.8160532407	2008-09-14 19:35:07	54725.0348842593	2008-09-16 00:50:14	503012010	57.6855	50	57.6935	57.6855	0	57.6981	2	2	0	2	1	0	0	51.9032	51.9032	105.2878	1	PROCESSED	57543.8433217593	2016-06-04 20:14:23	54557	2008-04-01 00:00:00	54780.6521643518	2008-11-10 15:39:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503012010/	Quick Look
553	HESS_J1825-137_3	276.1966	-13.9971	275.486722	-14.025442	276.082794	9.312755	17.46909054	-0.57831059	271.0001	54758.195775463	2008-10-19 04:41:55	54759.7917476852	2008-10-20 19:00:07	503030010	55.4996	50	55.4996	55.4996	0	55.4996	2	2	0	2	1	0	0	47.3252	47.3252	137.8379	1	PROCESSED	57544.2257407407	2016-06-05 05:25:04	55148	2009-11-13 00:00:00	54780.7804050926	2008-11-10 18:43:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030044	The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons.	GALACTIC DIFFUSE EMISSION	5	B	TAKAAKI TANAKA		JAP	3	AO3	MAPPING OBSERVATIONS OF HESS J1825-137	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503030010/	Quick Look
554	V1280 SCO	254.4172	-32.3368	253.607248	-32.260102	256.681689	-9.612724	351.33470039	6.5596985	97.7451	55605.3662615741	2011-02-13 08:47:25	55608.0501851852	2011-02-16 01:12:16	405029010	99.683	100	99.699	99.683	0	99.699	2	2	0	2	1	0	0	86.9306	86.9306	231.8739	2	PROCESSED	57600.9978472222	2016-07-31 23:56:54	55983	2012-02-26 00:00:00	55617.4142361111	2011-02-25 09:56:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050110	We propose a 100 ks observation of the C-rich classical nova V1280 Sco. Using Suzaku's excellent spectral performance in the soft X-ray energy band, we aim to detect and to resolve emission lines from C, N, and O.	GALACTIC POINT SOURCES	4	A	DAI TAKEI		JAP	5	AO5	X-RAY SPECTROSCOPY OF THE C-RICH CLASSICAL NOVA V1280 SCO	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405029010/	Quick Look
555	HESS J1800-240A	270.4845	-23.9659	269.719972	-23.966397	270.433159	-0.525758	6.13495239	-0.62617494	86.9255	54558.6209606482	2008-04-02 14:54:11	54559.3266087963	2008-04-03 07:50:19	503025010	34.7822	30	34.7822	34.7902	0	34.7902	2	2	0	2	1	0	0	25.7033	25.7033	60.9679	0	PROCESSED	57542.0259837963	2016-06-03 00:37:25	54953	2009-05-02 00:00:00	54574.0504861111	2008-04-18 01:12:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030043	H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region.	GALACTIC DIFFUSE EMISSION	5	A	TAKAAKI TANAKA		JAP	3	AO3	OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503025010/	Quick Look
556	HESS J1800-240C	269.7173	-24.0469	268.95232	-24.043667	269.732245	-0.606264	5.71665641	-0.05804766	87.3071	54563.0147337963	2008-04-07 00:21:13	54563.6877662037	2008-04-07 16:30:23	503027010	30.9755	30	30.9755	30.9755	0	30.9755	2	2	0	2	1	0	0	27.8155	27.8155	58.1239	1	PROCESSED	57542.2510185185	2016-06-03 06:01:28	54953	2009-05-02 00:00:00	54580.1897453704	2008-04-24 04:33:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030043	H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region.	GALACTIC DIFFUSE EMISSION	5	A	TAKAAKI TANAKA		JAP	3	AO3	OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503027010/	Quick Look
557	24M2791	334.9577	63.2629	334.551329	63.011149	23.890285	63.530312	106.81877019	5.23758822	230.0008	55947.3704513889	2012-01-21 08:53:27	55948.0926388889	2012-01-22 02:13:24	406023010	34.6017	30	34.6177	34.6017	0	34.6097	2	2	0	2	1	0	0	35.0595	35.0595	62.3919	0	PROCESSED	57604.5087847222	2016-08-04 12:12:39	56340	2013-02-17 00:00:00	55973.1102893518	2012-02-16 02:38:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060087	We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object.	GALACTIC POINT SOURCES	4	C	MASANORI OHNO		JAP	6	AO6	SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406023010/	Quick Look
558	VELA JR P23	132.7881	-46.3947	132.362089	-46.206312	159.378374	-59.957558	266.21323714	-1.3716571	347.0013	54652.3896759259	2008-07-05 09:21:08	54652.7710416667	2008-07-05 18:30:18	503035010	15.6901	10	15.6981	15.6901	0	15.7061	1	1	0	1	1	0	0	11.039	11.039	32.9439	1	PROCESSED	57542.9759490741	2016-06-03 23:25:22	55031	2009-07-19 00:00:00	54664.7904513889	2008-07-17 18:58:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503035010/	Quick Look
559	PSR J0614-33	93.5386	-33.5015	93.081964	-33.485438	95.411067	-56.876431	240.50300829	-21.83180137	119.1484	55498.9719675926	2010-10-29 23:19:38	55499.6140740741	2010-10-30 14:44:16	405014010	31.2109	30	31.2109	31.2109	0	31.2109	2	2	0	2	1	0	0	27.3314	27.3314	55.4499	0	PROCESSED	57553.8985763889	2016-06-14 21:33:57	55875	2011-11-10 00:00:00	55509.0359722222	2010-11-09 00:51:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050047	Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.	GALACTIC POINT SOURCES	4	C	NOBUYUKI KAWAI		JAP	5	AO5	X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405014010/	Quick Look
560	EMS0918	211.2948	-61.3938	210.393622	-61.154695	234.671242	-44.951341	311.64055354	0.22486043	106.822	55589.5588310185	2011-01-28 13:24:43	55590.0834837963	2011-01-29 02:00:13	405025010	24.5425	20	24.5505	24.5425	0	24.5585	2	2	0	2	1	0	0	23.2811	23.2811	45.3099	1	PROCESSED	57600.7734606482	2016-07-31 18:33:47	55972	2012-02-15 00:00:00	55602.2015046296	2011-02-10 04:50:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050104	Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV.	GALACTIC POINT SOURCES	4	A	YASUYUKI TANAKA		JAP	5	AO5	SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405025010/	Quick Look
561	VELA JR P35	132.966	-46.9473	132.543542	-46.75827	160.188354	-60.35477	266.71715615	-1.62954887	347.0008	54656.2642592593	2008-07-09 06:20:32	54656.5141087963	2008-07-09 12:20:19	503047010	11.5621	10	11.5861	11.5621	0	11.5941	1	1	0	1	1	0	0	9.6198	9.6198	21.5839	0	PROCESSED	57543.0120486111	2016-06-04 00:17:21	55037	2009-07-25 00:00:00	54670.2319212963	2008-07-23 05:33:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030048	We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	3	AO3	COMPLETING SUZAKU MAPPING OF VELA JR SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503047010/	Quick Look
562	HIGH LAT. DIFFUSE A	246.1745	43.4846	245.775383	43.597905	228.822222	63.555652	68.4171583	44.39202319	129.9994	53780.2926388889	2006-02-14 07:01:24	53781.9640509259	2006-02-15 23:08:14	500027010	73.5787	70	73.5867	73.5867	73.5787	73.5867	2	2	2	2	1	0	0	67.3993	67.3993	144.3979	3	PROCESSED	57533.0379976852	2016-05-25 00:54:43	54247	2007-05-27 00:00:00	54041.3110416667	2006-11-02 07:27:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000044	We propose observing the diffse background at two locations where the low temperature component is particularly string. One of the these enhancement is ostensibly an extension of the local bubble, while the other it is probably due to a region of very bright emission in the halo (z> 400 pc). We can verify the thermal nature of these sources, and look for CNO abyndance ratio differences between local disk and halo gas. It is critical to make these abundance determinations before the low energy response deteriorates any further. Note that this observation should also allow a calibration of the XIS response below the carbon edge to ~20%.	GALACTIC DIFFUSE EMISSION	5	A	SWG		JAP	0	SWG	HIGH LATTITUDE DIFFUSE A & B	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500027010/	Quick Look
563	EMS1308	293.0393	19.2567	292.487947	19.148974	299.013622	40.405253	54.62289289	0.10827332	90.0001	55313.4365740741	2010-04-27 10:28:40	55313.9766203704	2010-04-27 23:26:20	405028010	23.8987	20	23.9067	23.9067	0	23.8987	3	2	0	2	1	0	0	23.209	23.209	46.652	1	PROCESSED	57551.306400463	2016-06-12 07:21:13	55693	2011-05-12 00:00:00	55327.1789930556	2010-05-11 04:17:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050104	Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV.	GALACTIC POINT SOURCES	4	A	YASUYUKI TANAKA		JAP	5	AO5	SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405028010/	Quick Look
564	GALACTIC CENTER	266.0341	-30.1068	265.232432	-30.085596	266.53657	-6.713302	358.83318764	-0.33628911	269.0002	54019.4218402778	2006-10-11 10:07:27	54020.1446064815	2006-10-12 03:28:14	501057010	20.4884	20	20.4884	20.4964	20.4964	20.4964	2	2	2	2	1	0	0	19.086	19.086	62.4379	0	PROCESSED	57535.8262037037	2016-05-27 19:49:44	54735	2008-09-26 00:00:00	54053.6059837963	2006-11-14 14:32:37	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501057010/	Quick Look
565	CYG X-1	299.5787	35.2024	299.108699	35.065978	313.648056	54.25343	71.3307159	3.0753508	59.5691	56419.0925578704	2013-05-07 02:13:17	56419.6071643518	2013-05-07 14:34:19	407015020	1.5124	20	3.2442	1.5124	0	21.48	2	2	0	1	1	0	0	20.9258	20.9258	44.458	0	PROCESSED	57611.2625347222	2016-08-11 06:18:03	56808	2014-05-31 00:00:00	56442.9715509259	2013-05-30 23:19:02	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070030	We propose to observe Cyg X-1 for 85 ks, utilizing P-sum mode for XIS3. Our aim is to perform shot analysis, which is originally invented by Negoro et al. 1995 with Ginga, and obtain high-quality wide-band spectra for several phases in less than 1 sec; for example, 0.1 sec before the peak, +/- 0.05 sec at the peak, and after the peak. With these spectra, we will quantify changes in five spectral components: hard Comptonization, soft Comptonization, disk emission, Fe-K lines, and reflection. This will be a clue to know long-standing mystery on rapid variability in black holes.	GALACTIC POINT SOURCES	4	A	SHINYA YAMADA		JAP	7	AO7	INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407015020/	Quick Look
566	CYGNUS LOOP (P26)	314.1252	30.3135	313.601346	30.1206	328.529731	45.204244	74.46090737	-9.70687059	49.7995	54599.1203587963	2008-05-13 02:53:19	54599.5474421296	2008-05-13 13:08:19	503062010	16.9247	15	16.9247	16.9327	0	16.9327	2	2	0	2	1	0	0	15.441	15.441	36.892	1	PROCESSED	57542.5181944444	2016-06-03 12:26:12	54975	2009-05-24 00:00:00	54609.1293981482	2008-05-23 03:06:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030074	The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks.	GALACTIC DIFFUSE EMISSION	5	B	HIROSHI TSUNEMI		JAP	3	AO3	SUZAKU OBSERVATIONS OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503062010/	Quick Look
567	GC SOUTH BGD	266.1893	-28.9082	265.395265	-28.887768	266.639666	-5.511508	359.92534776	0.17564926	265.0003	54007.8931365741	2006-09-29 21:26:07	54009.2884143518	2006-10-01 06:55:19	501009010	51.19	50	51.198	51.206	51.19	51.198	2	2	2	2	1	0	0	47.7157	47.7157	120.5479	0	PROCESSED	57535.7087847222	2016-05-27 17:00:39	54735	2008-09-26 00:00:00	54020.9371064815	2006-10-12 22:29:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010044	Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	1	AO1	SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501009010/	Quick Look
568	G344.7-0.1	255.9588	-41.7032	255.078113	-41.633558	258.959028	-18.797881	344.67682908	-0.15577285	89.2821	54152.1890393518	2007-02-21 04:32:13	54153.2919097222	2007-02-22 07:00:21	501011010	42.1336	40	42.1336	42.1336	0	42.1336	2	2	0	2	1	0	0	34.2016	34.2016	95.28	1	PROCESSED	57537.4329050926	2016-05-29 10:23:23	54777	2008-11-07 00:00:00	54158.2352662037	2007-02-27 05:38:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010050	We propose an observation of a supernova remnant (SNR) G344.7-0.1 with Suzaku. In addition to emission lines from highly ionized ions (Si, S, and so on), we found a strong emission line at 6.4 keV in the spectra obtained with ASCA and XMM-Newton. This line is thought to be a K-line from the low-ionized Fe, but the origin is still unknown. Precise measurements of the line energy and the spectral parameters with the XIS will provide us with understanding the origin of the Fe-K line and the physical process in the SNR.	GALACTIC DIFFUSE EMISSION	5	C	SHIGEO YAMAUCHI		JAP	1	AO1	SUZAKU OBSERVATION OF G344.7-0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501011010/	Quick Look
569	CYGNUS_LOOP_P13	313.4901	31.0708	312.971102	30.880128	328.238327	46.115492	74.70349314	-8.80441033	68.2467	53865.1416666667	2006-05-10 03:24:00	53865.5321643518	2006-05-10 12:46:19	501030010	17.073	17	17.073	17.081	17.089	17.089	1	1	1	1	1	0	0	14.269	14.269	33.7279	0	PROCESSED	57534.2605092593	2016-05-26 06:15:08	54394	2007-10-21 00:00:00	53914.0847569444	2006-06-28 02:02:03	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501030010/	Quick Look
570	Sgr_A_East	266.5146	-28.9267	265.720381	-28.907844	266.926105	-5.522764	0.05802898	-0.07696746	264.7152	53636.3044560185	2005-09-23 07:18:25	53637.462025463	2005-09-24 11:05:19	100027010	44.785	50	44.801	44.8523	44.785	44.8283	2	2	2	2	1	0	0	37.8543	37.8543	100.0139	1	PROCESSED	57527.4188657407	2016-05-19 10:03:10	54247	2007-05-27 00:00:00	54035.502662037	2006-10-27 12:03:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000027	We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.	CALIBRATION	1	A	SWG		JAP	0	SWG	Suzaku Observation of Galactic Center Region		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027010/	Quick Look
571	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
572	CAS A	351.0231	59.0265	350.456601	58.751794	27.744986	54.948342	111.88943817	-1.95981315	208.1115	54876.0965740741	2009-02-14 02:19:04	54876.8363310185	2009-02-14 20:04:19	503080010	30.0355	30	30.0355	30.0355	0	30.0355	2	2	0	2	1	0	0	30.0731	30.0731	63.9139	0	PROCESSED	57545.551087963	2016-06-06 13:13:34	55330	2010-05-14 00:00:00	54892.9889699074	2009-03-02 23:44:07	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030127	Cas A is the youngest supernova remnant(SNR) in our Galaxy. Recently, the Spitzer Space Telescope discovered moving structures nearly at the speed of light outside the shell of the SNR. These structures are likely infrared echoes, where interstellar dust is heated by the outward moving photon shell of a bright flash. The bright flash is probably due to a giant flare from the central point source of Cas A, and if so, it requires that the central point source is a magnetar. Magnetars are known to emit luminous flares in the X-ray band, so it is expected that we can detect Fe-K fluorescence emission accompanied by IR echo. Here, we propose to observe on IR-emitting cloud around Cas A for 30ks to search for Fe-K emission which is naturally expected if the central point source is a magnetar.	GALACTIC DIFFUSE EMISSION	5	C	HIROYUKI AONO		JAP	3	AO3	INVESTIGATION OF A X-RAY ECHO NEAR THE SUPERNOVA REMNANT CASSIOPEIA A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503080010/	Quick Look
573	3C 326	238.0402	20.0989	237.485976	20.247377	230.081092	39.212111	33.27596058	48.22956027	119.5805	54484.6775	2008-01-19 16:15:36	54486.215462963	2008-01-21 05:10:16	702006010	61.7381	60	61.7381	61.7381	0	61.7381	2	2	0	2	1	0	0	53.4126	53.4126	132.8598	1	PROCESSED	57541.3565162037	2016-06-02 08:33:23	54888	2009-02-26 00:00:00	54515.0338078704	2008-02-19 00:48:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020014	Suzaku observations of two giant radio galaxies, 3C 326 and 3C 35, are proposed. In 60 ks exposure on the individual targets, inverse Component X-ray emission from their lobes is detected with high signal statistics. As a result, the energy densities of electrons and magnetic fields in these lobesare precisely deteremined. The size of these radio galaxies are significantly larger than that of the previous sample. Therefore, the size dependence of energetics in the lobes will be investigated.	EXTRAGALACTIC COMPACT SOURCES	7	C	NAOKI ISOBE		JAP	2	AO2	SUZAKU OBSERVATIONS OF LOBES OF GIANT RADIO GALAXIES, 3C 326 AND 3C 35	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702006010/	Quick Look
574	Crab Nebula	83.6442	22.0129	82.891939	21.980268	84.10941	-1.298101	184.56435264	-5.77651077	84.9978	53614.830775463	2005-09-01 19:56:19	53614.9098263889	2005-09-01 21:50:09	100015040	2.9786	5	2.9786	2.9786	2.9786	2.9786	1	1	1	1	1	0	0	3.0493	3.0493	6.8079	0	PROCESSED	57527.2502430556	2016-05-19 06:00:21	54247	2007-05-27 00:00:00	54109.1815625	2007-01-09 04:21:27	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000015		CALIBRATION	1	A	SWG		JAP	0	SWG	HXD boresight check with Crab		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015040/	Quick Look
575	HESS J1745-303 1	266.2249	-30.1096	265.423171	-30.089321	266.702778	-6.71164	358.91712668	-0.478438	70.5005	54527.7555555556	2008-03-02 18:08:00	54529.7363310185	2008-03-04 17:40:19	502016010	70.5291	67	70.5371	70.5291	0	70.5451	2	2	0	2	1	0	0	61.7932	61.7932	171.0959	3	PROCESSED	57541.8000810185	2016-06-02 19:12:07	54908	2009-03-18 00:00:00	54539.3190509259	2008-03-14 07:39:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020023	A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku.	GALACTIC DIFFUSE EMISSION	5	B	RYO YAMAZAKI		JAP	2	AO2	SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502016010/	Quick Look
576	ANTICENTER	113.3357	-19.5305	112.785719	-19.421448	119.46206	-40.613154	234.9976882	0.00424804	280.7829	54212.8606481482	2007-04-22 20:39:20	54215.4197222222	2007-04-25 10:04:24	502021010	89.5429	80	89.5509	89.5589	0	89.5429	2	2	0	2	1	0	0	78.9887	78.9887	221.0508	3	PROCESSED	57538.5236689815	2016-05-30 12:34:05	54744	2008-10-05 00:00:00	54223.2040046296	2007-05-03 04:53:46	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020032	We propose to observe diffuse radiation from the Galactic plane in the general direction of the anticenter. Absolute measurement of the O VII and O VIII line fluxes will help establish the origin of this mysterious component of the diffuse background. This will allow a search for spectral signatures of non-thermal emission, i.e. charge- exchange emission, in the 3/4 keV band and the determination of abundances in hot gas thermal emission without risk of confusion by emission from hot gas in the Galactic Bulge.	GALACTIC DIFFUSE EMISSION	5	B	KENSUKE MASUI		JAP	2	AO2	SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502021010/	Quick Look
577	VELA JR P1	131.9787	-45.8064	131.551046	-45.620931	157.807694	-59.76004	265.40235777	-1.43438498	347.0031	54285.3151273148	2007-07-04 07:33:47	54285.6904398148	2007-07-04 16:34:14	502023010	10.6496	10	10.6496	10.6576	0	10.6576	2	2	0	2	1	0	0	9.0446	9.0446	32.4199	0	PROCESSED	57539.086412037	2016-05-31 02:04:26	54696	2008-08-18 00:00:00	54328.4268402778	2007-08-16 10:14:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502023010/	Quick Look
578	1A1742-294(GC_BGD_1)	266.5264	-29.516	265.728429	-29.497192	266.950822	-6.111628	359.56008755	-0.392308	264.8664	53637.463287037	2005-09-24 11:07:08	53637.527962963	2005-09-24 12:40:16	100027030	2.0663	5	2.0663	2.0663	2.0663	2.0663	1	1	1	1	1	0	0	1.8877	1.8877	5.584	0	PROCESSED	57527.4000462963	2016-05-19 09:36:04	54247	2007-05-27 00:00:00	54035.4639583333	2006-10-27 11:08:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000027	We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.	CALIBRATION	1	A	SWG		JAP	0	SWG	Suzaku Observation of Galactic Center Region		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027030/	Quick Look
579	SAGITTARIUS A*	266.415	-29.0052	265.620304	-28.98586	266.840523	-5.603385	359.94564014	-0.04343346	106.9998	56738.4724189815	2014-03-22 11:20:17	56738.9897685185	2014-03-22 23:45:16	408017070	21.5887	20	21.6185	21.5887	0	21.6442	2	2	0	2	1	0	0	19.274	19.274	44.694	0	PROCESSED	57614.0833680556	2016-08-14 02:00:03	57120	2015-04-08 00:00:00	56750.8212268518	2014-04-03 19:42:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080074	With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A. A small gas cloud, G2, is on an orbit almost straight into Sgr A by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.	GALACTIC POINT SOURCES	4	A	YOSHITOMO MAEDA		JAP	8	AO8	SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017070/	Quick Look
580	1RXSJ170047.8-314442	255.196	-31.7452	254.389249	-31.672155	257.283531	-8.954733	352.21229356	6.40020757	90.7944	56341.4932060185	2013-02-18 11:50:13	56341.7501273148	2013-02-18 18:00:11	407027010	8.9262	12	8.9262	8.9262	0	8.9262	2	2	0	2	1	0	0	8.232	8.232	22.186	0	PROCESSED	57610.6225810185	2016-08-10 14:56:31	56718	2014-03-02 00:00:00	56352.4986458333	2013-03-01 11:58:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070052	We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.	GALACTIC POINT SOURCES	4	C	HIDEYUKI MORI		JAP	7	AO7	SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407027010/	Quick Look
581	PBC J0839.7-1214	129.9392	-12.3029	129.345024	-12.125278	136.15221	-29.568931	237.21342575	17.37856511	291.8979	55324.6892824074	2010-05-08 16:32:34	55326.4896990741	2010-05-10 11:45:10	705007010	80.5643	80	80.5643	80.5643	0	80.5643	2	2	0	2	1	0	0	70.7418	70.7418	155.5358	1	PROCESSED	57551.4721759259	2016-06-12 11:19:56	55707	2011-05-26 00:00:00	55341.5690856482	2010-05-25 13:39:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050024	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	5	AO5	BROAD BAND SPECTRA OF SWIFT/BAT SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705007010/	Quick Look
582	VELA JR P8	133.862	-45.8612	133.428362	-45.669016	160.04869	-59.10729	266.28131071	-0.45847751	347.0005	54287.3028240741	2007-07-06 07:16:04	54287.7009722222	2007-07-06 16:49:24	502030010	13.2196	10	13.2196	13.2196	0	13.2196	2	2	0	2	1	0	0	14.441	14.441	34.3919	0	PROCESSED	57539.112662037	2016-05-31 02:42:14	54703	2008-08-25 00:00:00	54333.4507175926	2007-08-21 10:49:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502030010/	Quick Look
583	VELA JR P13	131.851	-46.106	131.426011	-45.92099	157.974394	-60.061119	265.57984888	-1.69160478	347.0011	54290.1290162037	2007-07-09 03:05:47	54290.4411342593	2007-07-09 10:35:14	502035010	9.4089	10	9.4089	9.4089	0	9.4089	2	2	0	2	1	0	0	8.9531	8.9531	26.9639	0	PROCESSED	57539.1321412037	2016-05-31 03:10:17	54696	2008-08-18 00:00:00	54328.4906134259	2007-08-16 11:46:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020049	We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level.	GALACTIC DIFFUSE EMISSION	5	A	YASUNOBU UCHIYAMA		JAP	2	AO2	HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502035010/	Quick Look
584	SN1006	225.7268	-41.9424	224.908794	-41.746586	235.456683	-23.661429	327.58003425	14.55159393	117.0193	54521.6264351852	2008-02-25 15:02:04	54526.8613310185	2008-03-01 20:40:19	502046010	211.7373	200	211.7453	211.7373	0	211.7453	2	2	0	2	1	0	0	184.3622	184.3622	417.2759	6	PROCESSED	57541.8622337963	2016-06-02 20:41:37	54904	2009-03-14 00:00:00	54535.729375	2008-03-10 17:30:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020052	Thermal plasma incident SN1006 has very interesting characteristic. Suzaku PV spectrum revealed ionization parameter of the plasma is significantly low. We investigated the spatial variation of the ionization parameter, and found the outer region of SN1006 has lower ionization parameter than the inner region. However, since the center region of SN1006 is placed on the edge of FOV in the PV observation, the spectra have poor statistics, and the ionization state and the metal abundance cannot be decided with good precision. We propose to observe the center region of SN1006 deeply to decide the physical condition of the plasma of young SNR. Necessary exposure time is 150ksec.	GALACTIC DIFFUSE EMISSION	5	A	HIROYA YAMAGUCHI		JAP	2	AO2	THE CENTER REGION OF SN1006	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502046010/	Quick Look
585	HESS J1702-420	255.6874	-42.0709	254.803902	-41.999975	258.786548	-19.184424	344.26217794	-0.21974248	106.4451	54550.458599537	2008-03-25 11:00:23	54555.625162037	2008-03-30 15:00:14	502049010	215.6932	200	215.7053	215.6932	0	215.7053	2	2	0	2	1	0	0	140.6375	140.6375	395.7215	6	PROCESSED	57542.1678356482	2016-06-03 04:01:41	54933	2009-04-12 00:00:00	54566.9486458333	2008-04-10 22:46:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020067	The Galactic Plane Survey with HESS found several new TeV sources, called as "dark particle accelerators". They must be powerful cosmic-ray accelerators, although their origin is still unknown due to the lack of information in other wavelengths. We investigate one of the most mysterious sample, HESS J1702-420, which has the brightest HESS compact source without clear counterparts. ASCA Galactic plane survey shows no evidence of X-ray emission although the exposure was too short. With the large effective area and the low background of XISs, we will be able to detect quite dim counterpart or make strong upper-limit in the hard X-ray band. This result will lead us to distinguish that HESS J1702-420 is the true "dark" protonic accelerator, or a hypothetical PWN powered by PSR J1702-4128.	GALACTIC DIFFUSE EMISSION	5	B	AYA BAMBA		JAP	2	AO2	RESOLVING THE DARKEST DARK PARTICLE ACCELERATOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502049010/	Quick Look
586	N132D	81.4173	-69.7177	81.522733	-69.759029	311.341106	-85.51708	280.38157857	-32.71705874	53.198	53597.6939814815	2005-08-15 16:39:20	53597.8369328704	2005-08-15 20:05:11	100002030	0	7	0	0	0	0	0	0	0	0	0	0	0	0	0	0	0	PROCESSED	57520.6825231482	2016-05-12 16:22:50	54247	2007-05-27 00:00:00	54230.4133449074	2007-05-10 09:55:13	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000002	HXD HV ON WITH N132D, and 5 pointings with XIS	CALIBRATION	1	A	SWG		JAP	0	SWG	HXD HV ON WITH N132D		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100002030/	Quick Look
587	HESS J1731-347 SW	263.0074	-34.9458	262.173825	-34.909887	264.142527	-11.646447	353.3803333	-0.77058494	92.6086	55245.72	2010-02-18 17:16:48	55246.5231365741	2010-02-19 12:33:19	504031010	41.8615	40	41.8779	41.8615	0	41.8695	2	2	0	2	1	0	0	34.1028	34.1028	69.382	0	PROCESSED	57550.6419675926	2016-06-11 15:24:26	55623	2011-03-03 00:00:00	55257.0493981482	2010-03-02 01:11:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040026	Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1731-347 is one of only 3 TeV SNRs which have a radio shell and possible thermal X-rays. With good statistics and low background observation of Suzaku XIS, we will detect thermal X-rays from the shell of HESS J1731-347 for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition.	GALACTIC DIFFUSE EMISSION	5	B	AYA BAMBA		JAP	4	AO4	DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504031010/	Quick Look
588	TORNADO	265.1272	-30.949	264.32027	-30.923391	265.775878	-7.579198	357.70572925	-0.11631727	269.1137	55072.5037037037	2009-08-29 12:05:20	55075.0093055556	2009-09-01 00:13:24	504036010	125.0692	120	125.0692	125.0772	0	125.0772	2	2	0	2	1	0	0	97.0913	97.0913	216.4598	3	PROCESSED	57548.5178356482	2016-06-09 12:25:41	55454	2010-09-15 00:00:00	55088.3064814815	2009-09-14 07:21:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040076	The Tornado is an unusual and intense radio source located in the galactic center region. It has a polarized non-thermal radio spectrum. t has very unique morphology of elongated and loop-like structure. However, no crucial observational result determining the nature has been obtained. With the Suzaku AO3 observation of the Tornado (50ks), we found interesting signs of 2.45-keV He like S-K line, diffuse emission from the "tail" and the whole "head". The purpose of this observation is to obtain precise spectrum and spatial distribution. If the thermal S-K line is confirmed and it has a high metal abundance, the nature of the Tornado is an SNR. We also investigate the extreme structure of the tail and search for power-law component in spectra.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	4	AO4	REVEALING THE UNUSUAL SOURCE, THE NATURE OF THE "TORNADO", IN THE GALACTIC CENTER REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504036010/	Quick Look
589	GC_LARGEPROJECT1	266.4387	-28.5683	265.646756	-28.549082	266.850456	-5.166114	0.32941305	0.16640393	260.8767	54711.4273958333	2008-09-02 10:15:27	54712.9530555556	2008-09-03 22:52:24	503007010	52.1523	50	52.1523	52.1523	0	52.1523	2	2	0	2	1	0	0	44.1838	44.1838	131.7938	2	PROCESSED	57543.7627546296	2016-06-04 18:18:22	54557	2008-04-01 00:00:00	54780.6858796296	2008-11-10 16:27:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030022	We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	3	AO3	ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503007010/	Quick Look