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 229

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	E0102-72	15.9926	-72.0236	15.587314	-72.291594	314.630688	-65.030221	301.56327722	-45.07133229	226.8326	53720.0716203704	2005-12-16 01:43:08	53723.4377199074	2005-12-19 10:30:19	100044010	59.731	20	59.735	125.9195	59.731	59.737	3	3	3	3	1	0	0	115.3302	115.3302	290.8037	1	PROCESSED	57532.5803935185	2016-05-24 13:55:46	54247	2007-05-27 00:00:00	54119.7612615741	2007-01-19 18:16:13	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001097	We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	0	SWG	XIS FLIGHT CAIBRATION PLAN		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100044010/	Quick Look
49	CYGNUS LOOP	314.0345	31.9311	313.518544	31.738505	329.353732	46.719144	75.67403832	-8.61676541	64.2261	53884.1556018518	2006-05-29 03:44:04	53884.3793865741	2006-05-29 09:06:19	100049010	8.3805	10	8.3805	8.3805	8.3805	8.3805	1	1	1	1	1	0	0	6.0211	6.0211	19.304	0	PROCESSED	57534.4628240741	2016-05-26 11:06:28	54258	2007-06-07 00:00:00	54059.411099537	2006-11-20 09:51:59	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015007	Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	1	SWG	XIS FLIGHT CALIBRATION PLAN	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100049010/	Quick Look
50	CYGNUS LOOP	314.0785	32.0438	313.563	31.85105	329.470002	46.807189	75.78588033	-8.57358243	64.2263	53884.3796759259	2006-05-29 09:06:44	53884.6086342593	2006-05-29 14:36:26	100049020	7.8928	10	7.8928	7.8928	7.8928	7.8928	2	2	2	2	1	0	0	7.452	7.452	19.7699	0	PROCESSED	57534.4674884259	2016-05-26 11:13:11	54258	2007-06-07 00:00:00	54088.8429513889	2006-12-19 20:13:51	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015007	Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	1	SWG	XIS FLIGHT CALIBRATION PLAN	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100049020/	Quick Look
51	CYGNUS LOOP	313.9494	32.0818	313.434356	31.889502	329.346118	46.886158	75.74490282	-8.46508453	64.2292	53884.6089236111	2006-05-29 14:36:51	53884.8377777778	2006-05-29 20:06:24	100049030	11.6971	10	11.7051	11.6971	11.7051	11.7051	2	2	2	2	1	0	0	12.2688	12.2688	19.772	0	PROCESSED	57534.4722800926	2016-05-26 11:20:05	54258	2007-06-07 00:00:00	54052.4915046296	2006-11-13 11:47:46	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015007	Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	1	SWG	XIS FLIGHT CALIBRATION PLAN	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100049030/	Quick Look
52	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
53	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
54	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
55	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
56	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
57	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
58	GX 349+2	256.427	-36.366	255.587548	-36.298664	258.786235	-13.451096	349.14511841	2.78820606	85.6584	53808.5453240741	2006-03-14 13:05:16	53809.2216782407	2006-03-15 05:19:13	400003010	25.2308	50	25.2308	25.2332	25.2308	25.2308	1	1	1	1	1	0	0	20.0507	20.0507	58.434	2	PROCESSED	57533.2006365741	2016-05-25 04:48:55	54247	2007-05-27 00:00:00	54041.9132060185	2006-11-02 21:55:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001026	We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure.	GALACTIC POINT SOURCES	4	A	HIROMITSU TAKAHASHI		JAP	0	SWG	SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES)	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400003010/	Quick Look
59	SS CYG	325.6789	43.5736	325.187819	43.344381	350.451149	52.649921	90.55119171	-7.12024619	276.5788	53676.0503703704	2005-11-02 01:12:32	53676.9856944444	2005-11-02 23:39:24	400006010	39.4512	40	39.4512	39.4512	39.4512	39.4512	2	2	2	2	1	0	0	32.0472	32.0472	80.81	1	PROCESSED	57527.7175925926	2016-05-19 17:13:20	54247	2007-05-27 00:00:00	54036.9898148148	2006-10-28 23:45:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001043	Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst.	GALACTIC POINT SOURCES	4	A	MANABU ISHIDA		JAP	0	SWG	SS CYG OBSERVATION IN QUIESCENCE		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400006010/	Quick Look
60	X1630-472	248.4706	-47.343	247.550146	-47.238721	254.054156	-25.085181	336.93140696	0.30212129	69.0657	53781.9791087963	2006-02-15 23:29:55	53782.5474305556	2006-02-16 13:08:18	400010020	21.429	200	21.429	21.485	21.429	21.429	2	2	2	2	1	0	0	17.0223	17.0223	49.1019	0	PROCESSED	57533.0117592593	2016-05-25 00:16:56	54247	2007-05-27 00:00:00	54041.4892013889	2006-11-02 11:44:27	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001058	We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		JAP	0	SWG-TOO	FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010020/	Quick Look
61	NGC 4051	180.8556	44.5807	180.217538	44.859022	159.275193	40.404023	148.68917976	70.06918189	135.3482	53684.8015509259	2005-11-10 19:14:14	53687.4315277778	2005-11-13 10:21:24	700004010	119.578	150	119.61	119.61	119.586	119.578	2	2	2	2	1	0	0	120.0047	120.0047	227.1918	3	PROCESSED	57528.0225810185	2016-05-20 00:32:31	54247	2007-05-27 00:00:00	54037.5713078704	2006-10-29 13:42:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001012	We propose to obtain a broad band spectrum of the narrow-line Seyfert 1 (NLS1) NGC 4051. NLS1s are often presumed that they host a relatively small black hole with a very high accretion rate. Such a class would have played an important role in the growth of black holes in a cosmological context. We will measure the intrinsic photon index, amount of reflection, and high energy cutoff for the first time to investigate an accretion disk under a high accretion rate and compare them with conventional broad-line Seyferts.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	0	SWG	THE ACCRETION IN THE NARROW-LINE SEYFERT 1 NGC 4051 PROBED BY A BROAD BAND SPECTRUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700004010/	Quick Look
62	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
63	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
64	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
65	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
66	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
67	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
68	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
69	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
70	CAS A	350.8761	58.8091	350.310124	58.534509	27.390357	54.841399	111.74552355	-2.13963884	214.5537	53783.6003472222	2006-02-17 14:24:30	53783.9218055556	2006-02-17 22:07:24	100043020	14.155	10	14.155	14.155	14.155	14.155	1	1	1	1	1	0	0	17.3713	17.3713	27.768	0	PROCESSED	57533.0311805556	2016-05-25 00:44:54	54247	2007-05-27 00:00:00	54041.4627893518	2006-11-02 11:06:25	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001097	We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	0	SWG	XIS FLIGHT CAIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100043020/	Quick Look
71	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
72	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
73	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
74	TYCHO SNR HXD BKGD	9.2173	64.3076	8.488109	64.032592	44.61366	53.051862	121.35322514	1.48051733	84.2005	53915.6541782407	2006-06-29 15:42:01	53916.7606944444	2006-06-30 18:15:24	500025010	51.0088	50	51.0088	51.0088	51.0088	51.0088	2	2	2	2	1	0	0	48.7224	48.7224	95.5939	2	PROCESSED	57534.8010300926	2016-05-26 19:13:29	54302	2007-07-21 00:00:00	54052.5940509259	2006-11-13 14:15:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001099	We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		JAP	0	SWG	SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500025010/	Quick Look
75	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
76	BULGE 2	270.6176	-29.5847	269.818763	-29.585758	270.530563	-6.144879	1.30042786	-3.49803376	83.2679	53801.7493981482	2006-03-07 17:59:08	53802.0689699074	2006-03-08 01:39:19	500002010	13.028	10	13.052	13.044	13.036	13.028	1	1	1	1	1	0	0	10.6741	10.6741	27.5999	1	PROCESSED	57533.1394444444	2016-05-25 03:20:48	54247	2007-05-27 00:00:00	54041.664525463	2006-11-02 15:56:55	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001014	Leading .	GALACTIC DIFFUSE EMISSION	5	A	DAN MCCAMMON		JAP	0	SWG	THE SOFT GALACTIC BULGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500002010/	Quick Look
77	CYGNUS LOOP	313.9037	31.9696	313.388205	31.777464	329.228113	46.799115	75.63250703	-8.50670526	64.2245	53884.8380671296	2006-05-29 20:06:49	53885.0891666667	2006-05-30 02:08:24	100049040	11.7656	10	11.7816	11.7816	11.7736	11.7656	1	1	1	1	1	0	0	9.788	9.788	21.6879	0	PROCESSED	57534.4771296296	2016-05-26 11:27:04	54258	2007-06-07 00:00:00	54052.5201157407	2006-11-13 12:28:58	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015007	Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	1	SWG	XIS FLIGHT CALIBRATION PLAN	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100049040/	Quick Look
78	A3376 WEST RELIC	90.0363	-39.9917	89.629297	-39.992531	90.071049	-63.433501	246.43145562	-26.38385089	126.3601	54034.3950231482	2006-10-26 09:28:50	54035.9176388889	2006-10-27 22:01:24	800011020	62.2648	60	62.2648	62.2648	62.2648	62.2648	2	2	2	2	1	0	0	55.5629	55.5629	131.5378	2	PROCESSED	57535.9705902778	2016-05-27 23:17:39	54694	2008-08-16 00:00:00	54090.2671643518	2006-12-21 06:24:43	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001039	We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA		JAP	0	SWG	SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800011020/	Quick Look
79	GRB060105	297.6095	46.3384	297.227077	46.210211	319.460988	65.110067	80.2506255	9.98748628	191.1906	53740.5089351852	2006-01-05 12:12:52	53741.5002083333	2006-01-06 12:00:18	900001010	42.2208	40	42.2208	42.2208	42.2208	42.2208	2	2	2	2	1	0	0	37.718	37.718	85.6419	2	PROCESSED	57532.6415856482	2016-05-24 15:23:53	54247	2007-05-27 00:00:00	54039.776712963	2006-10-31 18:38:28	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001008	(i) Early break in lightcurve of X-ray afterglows using HXD. Recent Swift/XRT observations reveal that early X-ray afterglows of GRB has flat portion with very shallow decay. It may suggest continuous energy input from the central engine. The transition from its phase to general afterglow may display hard-to-soft evolution reflecting the cooling frequency. Thus multi wavelength observation will provide a key to the physics of central engine activity. (ii) Emission lines in the afterglows. The confirmation of line existence should be a matter of great importance because there remains unanswered questions. Some data may indicate a prominent iron line but others seem to suggest significant lower energy lines instead without iron lines.	EXTRAGALACTIC COMPACT SOURCES	9	A	TOSHIO MURAKAMI		JAP	0	SWG-TOO	TOO OBSERVATIONS OF GAMMA-RAY BURSTS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/900001010/	Quick Look
80	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
81	ABELL 1795 Far North	207.223	26.9995	206.646903	27.247656	193.71055	35.352954	35.63943573	77.21561208	130.4264	53715.3208796296	2005-12-11 07:42:04	53715.9730092593	2005-12-11 23:21:08	800012030	30.6406	30	30.6486	30.6406	30.6639	30.6566	2	2	2	2	1	0	0	27.8833	27.8833	56.3379	1	PROCESSED	57532.4195833333	2016-05-24 10:04:12	54247	2007-05-27 00:00:00	54039.1003703704	2006-10-31 02:24:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012030/	Quick Look
82	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
83	BULGE 3	274.7046	-31.4846	273.893726	-31.505472	274.041648	-8.109784	1.3002625	-7.49777303	80.4025	53800.3437962963	2006-03-06 08:15:04	53801.7474421296	2006-03-07 17:56:19	500001010	51.8468	50	51.8548	51.8548	51.8548	51.8468	2	2	2	2	1	0	0	45.0783	45.0783	121.2459	0	PROCESSED	57533.1540972222	2016-05-25 03:41:54	54247	2007-05-27 00:00:00	54041.7128703704	2006-11-02 17:06:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001014	Leading .	GALACTIC DIFFUSE EMISSION	5	A	DAN MCCAMMON		JAP	0	SWG	THE SOFT GALACTIC BULGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500001010/	Quick Look
84	SN1006 NW	225.6364	-41.8003	224.819551	-41.604176	235.339658	-23.546444	327.59294648	14.70833496	115.0008	53766.4881365741	2006-01-31 11:42:55	53767.55375	2006-02-01 13:17:24	500017010	53.0194	50	53.0194	53.0277	53.0273	53.0273	2	2	2	2	1	0	0	60.4123	60.4123	92.0679	0	PROCESSED	57532.8347685185	2016-05-24 20:02:04	54247	2007-05-27 00:00:00	54040.7669675926	2006-11-01 18:24:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001062	We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		JAP	0	SWG	THE EJECTA IN SN1006	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500017010/	Quick Look
85	A 2218 OFFSETB	249.9091	65.2119	249.835523	65.307656	180.044789	81.713752	96.37864193	38.09205953	233.3309	53670.1916319444	2005-10-27 04:35:57	53670.4620833333	2005-10-27 11:05:24	800020010	14.9215	15	14.9375	14.9335	14.9215	14.9415	2	2	2	2	1	0	0	14.1931	14.1931	23.3561	0	PROCESSED	57527.6596180556	2016-05-19 15:49:51	54247	2007-05-27 00:00:00	54036.8343981482	2006-10-28 20:01:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001096	To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI		JAP	0	SWG	SEARCH FOR OXYGEN LINES FROM WARM IGM		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800020010/	Quick Look
86	CAS A	350.8729	58.8094	350.30695	58.534812	27.388607	54.842749	111.74406014	-2.13880346	214.7372	53768.5363657407	2006-02-02 12:52:22	53768.833599537	2006-02-02 20:00:23	100043010	0	10	0	0	0	0	0	0	0	0	1	0	0	10.3268	10.3268	25.6739	1	PROCESSED	57532.8451736111	2016-05-24 20:17:03	54247	2007-05-27 00:00:00	54040.7488888889	2006-11-01 17:58:24	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001097	We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	0	SWG	XIS FLIGHT CAIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100043010/	Quick Look
87	A 2218 CENTER	249.0052	66.205	248.955095	66.304813	172.75657	81.615548	97.72589248	38.11630228	233.3294	53669.4904050926	2005-10-26 11:46:11	53670.1905555556	2005-10-27 04:34:24	800019010	31.9354	35	31.9434	31.9434	31.9354	31.9434	2	2	2	2	1	0	0	28.9371	28.9371	60.4879	1	PROCESSED	57527.6471990741	2016-05-19 15:31:58	54247	2007-05-27 00:00:00	54036.9596990741	2006-10-28 23:01:58	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001096	To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI		JAP	0	SWG	SEARCH FOR OXYGEN LINES FROM WARM IGM		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800019010/	Quick Look
88	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
89	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
90	NGC 2992	146.4207	-14.2696	145.81924	-14.038457	154.003817	-26.061971	249.65504756	28.81616071	88.7924	53693.8781597222	2005-11-19 21:04:33	53694.9759722222	2005-11-20 23:25:24	700005020	37.4935	120	37.6565	39.6915	37.4935	37.8205	1	1	1	1	1	0	0	33.8991	33.8991	94.8479	1	PROCESSED	57528.0334490741	2016-05-20 00:48:10	54247	2007-05-27 00:00:00	54037.7316087963	2006-10-29 17:33:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001013	NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	0	SWG	THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005020/	Quick Look
91	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
92	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
93	A3376 WEST RELIC	90.0415	-39.9946	89.634521	-39.995405	90.079962	-63.436398	246.43569548	-26.38071178	132.0018	53681.5938078704	2005-11-07 14:15:05	53684.7883912037	2005-11-10 18:55:17	800011010	126.9969	150	126.9969	127.1809	127.0769	127.0289	2	2	2	2	1	0	0	112.9113	112.9113	230.9397	3	PROCESSED	57528.0013541667	2016-05-20 00:01:57	54247	2007-05-27 00:00:00	54037.6050231482	2006-10-29 14:31:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001039	We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA		JAP	0	SWG	SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800011010/	Quick Look
94	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
95	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
96	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
97	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
98	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
99	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
100	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
101	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
102	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
103	E0102-72	16.027	-72.0223	15.622199	-72.290248	314.64413	-65.039289	301.54815221	-45.07189388	294.0751	53768.8467592593	2006-02-02 20:19:20	53769.4065393518	2006-02-03 09:45:25	100044030	20.8277	20	20.8357	20.8437	20.8437	20.8277	2	2	2	2	1	0	0	20.2688	20.2688	48.36	1	PROCESSED	57532.8615740741	2016-05-24 20:40:40	54247	2007-05-27 00:00:00	53905.6764351852	2006-06-19 16:14:04	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001097	We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	0	SWG	XIS FLIGHT CAIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100044030/	Quick Look
104	ETA CARINAE	161.248	-59.6859	160.761598	-59.422588	202.142	-58.929196	287.58997588	-0.63475906	156.124	53769.4163194444	2006-02-03 09:59:30	53769.9481944444	2006-02-03 22:45:24	100045010	21.3678	20	21.3678	21.3678	21.3678	21.3678	2	2	2	2	1	0	0	18.1458	18.1458	45.9459	1	PROCESSED	57532.9369907407	2016-05-24 22:29:16	54247	2007-05-27 00:00:00	54040.9846643518	2006-11-01 23:37:55	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001097	We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	0	SWG	XIS FLIGHT CAIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100045010/	Quick Look
105	BULGE 6	282.6839	-33.8925	281.860158	-33.951684	280.687841	-10.9215	1.99857856	-14.59644221	88.3467	53802.7373032407	2006-03-08 17:41:43	53803.0466087963	2006-03-09 01:07:07	500003010	14.2617	10	14.2617	14.2617	14.2617	14.2617	2	2	2	2	1	0	0	11.414	11.414	26.7159	1	PROCESSED	57533.1570833333	2016-05-25 03:46:12	54247	2007-05-27 00:00:00	54041.7424305556	2006-11-02 17:49:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001014	Leading .	GALACTIC DIFFUSE EMISSION	5	A	DAN MCCAMMON		JAP	0	SWG	THE SOFT GALACTIC BULGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500003010/	Quick Look
106	X1630-472	248.4772	-47.3405	247.556757	-47.236251	254.058584	-25.081993	336.93627828	0.30053306	75.5959	53794.9708333333	2006-02-28 23:18:00	53795.6968055556	2006-03-01 16:43:24	400010030	21.5216	200	21.5216	21.5216	21.5216	21.5216	2	2	2	2	1	0	0	19.0328	19.0328	62.718	0	PROCESSED	57533.1079050926	2016-05-25 02:35:23	54247	2007-05-27 00:00:00	54041.5956018518	2006-11-02 14:17:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001058	We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		JAP	0	SWG-TOO	FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010030/	Quick Look
107	LOCKMANHOLE	163.4063	57.6108	162.636897	57.876997	137.149157	45.549363	148.98193179	53.14624927	119.611	53688.2372337963	2005-11-14 05:41:37	53689.8300694444	2005-11-15 19:55:18	100046010	76.9806	100	76.9806	77.0446	77.0126	77.0206	2	2	2	2	1	0	0	94.5107	94.5107	137.6079	3	PROCESSED	57528.0048148148	2016-05-20 00:06:56	54247	2007-05-27 00:00:00	54037.5889814815	2006-10-29 14:08:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001098	We propose a 100 ks observation of LockmanHole with Suzaku. The main purpose is to obtain a template dataset of HXD background.	CALIBRATION	1	A	MOTOHIDE KOKUBUN		JAP	0	SWG	BACKGROUND ESTABLISHMENT OF HXD	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100046010/	Quick Look
108	AE AQUARII	310.0612	-0.931	309.416636	-1.108991	312.236832	16.82972	45.23545862	-24.46836188	250.6241	54033.2319907407	2006-10-25 05:34:04	54034.3829282407	2006-10-26 09:11:25	400001020	47.9743	50	47.9743	48.5956	48.1316	48.3103	2	2	2	2	1	0	0	45.5384	45.5384	99.4239	1	PROCESSED	57526.8238773148	2016-05-18 19:46:23	54526	2008-03-01 00:00:00	54109.7083449074	2007-01-09 17:00:01	3.0.22.43	9	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001004	We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku.	GALACTIC POINT SOURCES	4	A	YUKIKATSU TERADA		JAP	0	SWG	SEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKU	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400001020/	Quick Look
109	GX 349+2	256.4194	-36.3657	255.579957	-36.298328	258.779942	-13.451385	349.14166441	2.79326977	78.9359	53813.9267708333	2006-03-19 22:14:33	53814.6043402778	2006-03-20 14:30:15	400003020	28.1177	50	28.1177	28.1317	28.1204	28.1204	2	2	2	2	1	0	0	25.6573	25.6573	58.538	0	PROCESSED	57533.2767939815	2016-05-25 06:38:35	54247	2007-05-27 00:00:00	54042.1657407407	2006-11-03 03:58:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001026	We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure.	GALACTIC POINT SOURCES	4	A	HIROMITSU TAKAHASHI		JAP	0	SWG	SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES)	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400003020/	Quick Look
110	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
111	X1630-472	248.4828	-47.3401	247.56235	-47.235876	254.062648	-25.080987	336.93914719	0.29801709	78.3341	53774.6318981482	2006-02-08 15:09:56	53775.1390972222	2006-02-09 03:20:18	400010010	22.1902	200	22.1902	22.1902	22.1902	22.1902	1	1	1	1	1	0	0	22.247	22.247	43.816	0	PROCESSED	57532.9380787037	2016-05-24 22:30:50	54247	2007-05-27 00:00:00	54040.9540856482	2006-11-01 22:53:53	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001058	We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		JAP	0	SWG-TOO	FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010010/	Quick Look
112	73P/SW3	279.6627	33.4734	279.203358	33.427762	284.650097	56.423756	62.35168426	17.03145652	46.5564	53862.4804282407	2006-05-07 11:31:49	53862.5419444444	2006-05-07 13:00:24	500012020	3.248	5	3.248	3.248	3.248	3.248	1	1	1	1	1	0	0	2.1119	2.1119	5.2799	0	PROCESSED	57533.7332407407	2016-05-25 17:35:52	54256	2007-06-05 00:00:00	54042.2282175926	2006-11-03 05:28:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500012020/	Quick Look
113	73P/SW3	316.717	24.6807	316.164001	24.478965	328.484877	39.12074	71.53645371	-15.07849931	72.7087	53868.1752314815	2006-05-13 04:12:20	53868.2085532407	2006-05-13 05:00:19	500013010	2.353	20	2.353	2.353	2.353	2.353	1	1	1	1	1	0	0	2.595	2.595	2.8719	0	PROCESSED	57534.2831597222	2016-05-26 06:47:45	54256	2007-06-05 00:00:00	54042.2312268518	2006-11-03 05:32:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013010/	Quick Look
114	73P/SW3	317.1042	24.5187	316.549923	24.315676	328.827114	38.838912	71.64340536	-15.45205291	72.7099	53868.2091666667	2006-05-13 05:01:12	53868.2752199074	2006-05-13 06:36:19	500013020	3.225	20	3.225	3.225	3.225	3.225	1	1	1	1	1	0	0	3.467	3.467	5.7039	0	PROCESSED	57534.2879398148	2016-05-26 06:54:38	54256	2007-06-05 00:00:00	54042.2634027778	2006-11-03 06:19:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013020/	Quick Look
115	73P/SW3	319.1503	23.6322	318.589279	23.422515	330.602424	37.314629	72.21442919	-17.44595626	72.7095	53868.5425	2006-05-13 13:01:12	53868.6085532407	2006-05-13 14:36:19	500013070	3.0624	20	3.0624	3.0624	3.0624	3.0624	1	1	1	1	1	0	0	2.088	2.088	5.688	1	PROCESSED	57534.3049074074	2016-05-26 07:19:04	54256	2007-06-05 00:00:00	54042.3037268518	2006-11-03 07:17:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013070/	Quick Look
116	73P/SW3	17.8447	-9.1515	17.217751	-9.416998	12.842123	-15.443966	138.54867442	-71.41609802	59.3994	53893.7363888889	2006-06-07 17:40:24	53893.8023032407	2006-06-07 19:15:19	500014020	3.2369	35	3.2369	3.2369	3.2369	3.2369	1	1	1	1	1	0	0	2.478	2.478	5.6879	0	PROCESSED	57534.5816435185	2016-05-26 13:57:34	54267	2007-06-16 00:00:00	54052.5079861111	2006-11-13 12:11:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014020/	Quick Look
117	73P/SW3	18.0085	-9.2093	17.381763	-9.474557	12.972897	-15.560645	139.0853548	-71.43220951	59.4015	53893.9358333333	2006-06-07 22:27:36	53894.0023032407	2006-06-08 00:03:19	500014050	3.235	35	3.235	3.235	3.235	3.235	1	1	1	1	1	0	0	2.5041	2.5041	5.7359	0	PROCESSED	57534.5878125	2016-05-26 14:06:27	54267	2007-06-16 00:00:00	54052.5317361111	2006-11-13 12:45:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014050/	Quick Look
118	73P/SW3	18.1094	-9.2436	17.482792	-9.508708	13.054019	-15.631304	139.41528011	-71.44015907	59.3996	53894.0691666667	2006-06-08 01:39:36	53894.1356365741	2006-06-08 03:15:19	500014070	2.2209	35	2.2209	2.2209	2.2209	2.2209	1	1	1	1	1	0	0	1.939	1.939	5.7359	1	PROCESSED	57534.589849537	2016-05-26 14:09:23	54267	2007-06-16 00:00:00	54052.5472800926	2006-11-13 13:08:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014070/	Quick Look
119	73P/SW3	18.2503	-9.299	17.623885	-9.563897	13.164284	-15.736856	139.88257526	-71.45759255	59.3985	53894.2691435185	2006-06-08 06:27:34	53894.3356134259	2006-06-08 08:03:17	500014100	1.3121	35	1.3121	1.3121	1.3121	1.3121	1	1	1	1	1	0	0	1.322	1.322	5.742	0	PROCESSED	57534.5960185185	2016-05-26 14:18:16	54267	2007-06-16 00:00:00	54052.5405324074	2006-11-13 12:58:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014100/	Quick Look
120	73P/SW3	18.435	-9.3697	17.808837	-9.63432	13.309685	-15.873419	140.49459076	-71.47695116	59.4003	53894.5358333333	2006-06-08 12:51:36	53894.6016087963	2006-06-08 14:26:19	500014140	1.977	35	1.977	1.977	1.977	1.977	1	1	1	1	1	0	0	1.951	1.951	5.6719	0	PROCESSED	57534.60375	2016-05-26 14:29:24	54267	2007-06-16 00:00:00	54052.5450231482	2006-11-13 13:04:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014140/	Quick Look
121	MBM12	44.0042	19.487	43.295962	19.285573	47.250431	2.610049	159.18888296	-34.46916863	253.4644	53769.9600578704	2006-02-03 23:02:29	53772.6460416667	2006-02-06 15:30:18	500015010	102.9371	100	102.9371	102.9371	102.9371	102.9371	2	2	2	2	1	0	0	93.6709	93.6709	232.0499	1	PROCESSED	57532.9850694444	2016-05-24 23:38:30	54247	2007-05-27 00:00:00	54041.1327662037	2006-11-02 03:11:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001059	Suzaku can potentially determine the time since the nearby supernova that created (or reheated) the Local Hot Bubble (LHB) by measuring the ratio of the O VII/O VIII lines emitted by the LHB. The LHB temperature is ~10^6 K, and in equilibrium we would expect no O VIII emission. However, the LHB is almost certainly not in equilibrium, and it is quite possible that significant O^{+7} is still recombining (and emitting O VIII) following its creation in the most recent local supernova 2-4 Myr ago. We propose to measure these lines from the LHB using the nearby molecular cloud MBM12 as a curtain to shadow more distant emission. Even if O VIII is not detected, the O VII measurement will be the first unambiguous measurement of a line from the LHB.	GALACTIC DIFFUSE EMISSION	5	A	RANDALL SMITH		JAP	0	SWG	DATING THE LOCAL HOT BUBBLE WITH SUZAKU	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500015010/	Quick Look
122	CYGNUS LOOP NE4	313.5005	32.369	312.987812	32.178281	329.006135	47.302265	75.72495347	-7.98937114	221.2023	53704.2368287037	2005-11-30 05:41:02	53704.7661342593	2005-11-30 18:23:14	500023010	25.0049	20	25.0049	25.2689	25.0067	25.0689	2	2	2	2	1	0	0	25.1249	25.1249	45.726	1	PROCESSED	57532.3510763889	2016-05-24 08:25:33	54247	2007-05-27 00:00:00	54038.67625	2006-10-30 16:13:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001093	We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	0	SWG	CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500023010/	Quick Look
123	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
124	X1630-472	248.5405	-47.3458	247.619879	-47.241836	254.106265	-25.080324	336.96147829	0.2654214	120.3	53817.4260300926	2006-03-23 10:13:29	53817.9313425926	2006-03-23 22:21:08	400010060	21.6541	200	21.6621	21.6541	21.6541	21.6541	2	1	2	2	1	0	0	22.7619	22.7619	43.6559	1	PROCESSED	57533.3033796296	2016-05-25 07:16:52	54247	2007-05-27 00:00:00	54042.1043287037	2006-11-03 02:30:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001058	We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		JAP	0	SWG-TOO	FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010060/	Quick Look
125	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
126	3C120	68.2993	5.3535	67.634764	5.249056	67.434072	-16.404208	190.3755878	-27.39480435	262.4873	53789.4598726852	2006-02-23 11:02:13	53790.8748958333	2006-02-24 20:59:51	700001030	40.9073	160	40.9073	40.9073	40.9073	40.9073	2	2	2	2	1	0	0	38.4817	38.4817	77.876	2	PROCESSED	57533.073900463	2016-05-25 01:46:25	54247	2007-05-27 00:00:00	54041.5149189815	2006-11-02 12:21:29	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001003	Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	0	SWG	BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001030/	Quick Look
127	MCG-6-30-15	203.9713	-34.2978	203.254904	-34.042659	215.172989	-22.546967	313.28925681	27.67845448	102.4359	53762.928275463	2006-01-27 22:16:43	53765.368275463	2006-01-30 08:50:19	700007030	96.6919	300	96.6919	96.6919	96.6999	96.6999	2	2	2	2	1	0	0	89.8194	89.8194	210.8019	5	PROCESSED	57532.8529861111	2016-05-24 20:28:18	54247	2007-05-27 00:00:00	54040.8156828704	2006-11-01 19:34:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001035	The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales .	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREW FABIAN		JAP	0	SWG	REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007030/	Quick Look
128	0836+714	130.267	70.829	129.006808	71.006559	109.318804	50.076677	143.62710847	34.4182022	294.8268	53809.7578125	2006-03-15 18:11:15	53810.5836111111	2006-03-16 14:00:24	700010010	55.6261	50	55.6341	55.6341	55.6261	55.6341	2	2	2	2	1	0	0	47.4058	47.4058	71.3419	1	PROCESSED	57533.2238541667	2016-05-25 05:22:21	54247	2007-05-27 00:00:00	54041.9651851852	2006-11-02 23:09:52	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001061	We propose two 50 ks observations, one for each of two EGRET blazars, 1510-089 (OR -017) and 0836+710 (4C +71.07). Both objects show extremely hard X-ray spectra, with photon indices about 1.3. The blazar 1510-089 ($z = 0.361$) is among a few OVV quasars showing prominent soft X-ray excess. The blazar 0836+710 ($z = 2.172)$ is the brightest X-ray source among the high redshift ($z>2$) quasars, and its very hard X-ray spectrum extends down to soft X-rays. Studying spectral shape and variability in the soft X-ray band relative to variability in the mid X-ray and optical bands can help to reveal nature of the soft X-ray excess of unknown origin, and multifrequency variability studies can provide constraints on the structure of jets on subparsec scales.	EXTRAGALACTIC COMPACT SOURCES	7	A	GREG MADEJSKI		JAP	0	SWG	TESTING THE SHOCK-IN-JET MODEL FOR NONTHERMAL FLARES IN BLAZARS VIA SUZAKU OBSERVATIONS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700010010/	Quick Look
129	SWIFT J0746.3+2548	116.6142	25.8792	115.852151	26.002245	113.853224	4.615293	194.5201067	22.91801121	97.0095	53678.357974537	2005-11-04 08:35:29	53680.5862847222	2005-11-06 14:04:15	700011010	99.4284	100	99.5235	100.4524	99.4284	99.7235	2	2	2	2	1	0	0	87.6995	87.6995	192.472	4	PROCESSED	57527.9575694445	2016-05-19 22:58:54	54247	2007-05-27 00:00:00	54037.5799074074	2006-10-29 13:55:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001087	Recently the BAT gamma-ray detector onboard Swift satellite has discovered very flat hard X-ray sources with photon index ~ 1.5 above 100 keV. The x-ray spectrum obtained with the XRT on Swiftis highly variable on time scales < 90 minutes. This variability and flat continuum spectrum suggests that this source is classified as a blazar. If this association is real, we have a precious chance to obtain spectrum upto several hundred keV in the source frame of the source. This wide range is of particularly importanceto study the blazar spectrum, or the electron distribution.	EXTRAGALACTIC COMPACT SOURCES	7	A	TADAYUKI TAKAHASHI		JAP	0	SWG	SUZAKU OBSERVATION OF A HIGH REDSHIFT BLAZAR RECENTLY DISCOVERED BY THE BAT ON SWIFT		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700011010/	Quick Look
130	ABELL2801	9.6433	-29.1188	9.027926	-29.393572	356.054774	-30.312746	357.12193154	-86.53506096	232.0377	53701.3547106482	2005-11-27 08:30:47	53702.1668865741	2005-11-28 04:00:19	800008010	34.89	25	34.89	34.89	34.89	34.89	2	2	2	2	1	0	0	30.1636	30.1636	70.1639	1	PROCESSED	57528.0891898148	2016-05-20 02:08:26	54247	2007-05-27 00:00:00	54038.3717361111	2006-10-30 08:55:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001025	We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYUKI TAMURA		JAP	0	SWG	THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800008010/	Quick Look
131	ABELL 1795 Near North	207.2221	26.7993	206.645445	27.047459	193.815884	35.172187	34.737463	77.20142043	130.7334	53714.7756481482	2005-12-10 18:36:56	53715.3203587963	2005-12-11 07:41:19	800012020	24.4106	25	24.4266	24.4106	24.4426	24.4346	1	1	1	1	1	0	0	25.1798	25.1798	47.0559	2	PROCESSED	57532.404375	2016-05-24 09:42:18	54247	2007-05-27 00:00:00	54038.8804166667	2006-10-30 21:07:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012020/	Quick Look
132	ABELL 1795 Near South	207.2228	26.4007	206.645046	26.648859	194.026663	34.812966	32.94964182	77.16185549	129.833	53715.9739467593	2005-12-11 23:22:29	53716.5355787037	2005-12-12 12:51:14	800012040	26.074	25	26.098	26.0919	26.074	26.086	2	2	2	2	1	0	0	25.7986	25.7986	48.522	1	PROCESSED	57532.4329282407	2016-05-24 10:23:25	54247	2007-05-27 00:00:00	54039.0706018518	2006-10-31 01:41:40	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012040/	Quick Look
133	NGC4388	186.4461	12.6674	185.812197	12.944186	180.780806	14.166666	279.11809751	74.34084148	119.622	53728.3779976852	2005-12-24 09:04:19	53731.250162037	2005-12-27 06:00:14	800017010	123.6341	100	123.9249	125.8143	123.6341	124.1523	2	2	2	2	1	0	0	111.8209	111.8209	248.128	3	PROCESSED	57532.5484143518	2016-05-24 13:09:43	54247	2007-05-27 00:00:00	54039.5984375	2006-10-31 14:21:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001077	Large-scale X-ray nebulae up to a few tens of kpc have been often found in starburst galaxies, which is thermally heated up by the superwind from the starburst nucleus. Iwasawa et al. (2003) found a large X-ray nebula up to 16kpc around NGC4388, which is photoiionized by Seyfert nucleus. Thus, this result suggests that the hard X-ray emission from active galactic nucleus could be a prime heat source of nebula. The goals of this observation are (1) to see how far the X-ray nebula is extended, (2) to obtain its precise X-ray spectrum, (3) to determine what is the X-ray emission mechanism, and (4) to exam if the photoionization by AGN could be a prime heat source of the galactic halo. We determine the photon index and the high energy cut-off of the power-law component from the HXD spectrum.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKESHI TSURU		JAP	0	SWG	VERY EXTENDED PHOTOIONIZED X-RAY NEBULA AROUND THE SEYFERT GALAXY NGC4388	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800017010/	Quick Look
134	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
135	AE AQUARII	310.0457	-0.9355	309.401118	-1.113434	312.219972	16.829528	45.22275468	-24.45710482	264.8759	53673.9022685185	2005-10-30 21:39:16	53676.043275463	2005-11-02 01:02:19	400001010	70.5289	100	70.5289	70.6169	70.5689	70.5449	3	3	3	3	1	0	0	59.4538	59.4538	184.9569	2	PROCESSED	57527.7308217593	2016-05-19 17:32:23	54247	2007-05-27 00:00:00	54036.9851388889	2006-10-28 23:38:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001004	We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku.	GALACTIC POINT SOURCES	4	A	YUKIKATSU TERADA		JAP	0	SWG	SEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKU		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400001010/	Quick Look
136	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
137	A1413	178.8303	23.6485	178.18646	23.926767	169.076487	21.133974	225.18767075	76.86550896	123.0348	53689.8362847222	2005-11-15 20:04:15	53692.5939699074	2005-11-18 14:15:19	800001010	107.8672	100	107.8672	108.0032	107.9472	107.9103	2	2	2	2	1	0	0	102.4315	102.4315	238.2397	7	PROCESSED	57528.0427546296	2016-05-20 01:01:34	54247	2007-05-27 00:00:00	54038.1136689815	2006-10-30 02:43:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001010	No cluster has had its X-ray temperature measured out to the virial radius. Hence no cluster has had it total mass measured using X-ray methods. Typically these measurements extend only to 60% of the virial radius. We propose to perform these measurements for the first time and with high accuracy for the relaxed cluster A1413. The low Suzaku background permits us to make this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	J. HENRY		JAP	0	SWG	CLUSTER TEMPERATURE AND MASS MEASUREMENT TO THE VIRIAL RADIUS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800001010/	Quick Look
138	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
139	X1630-472	248.5414	-47.3441	247.620794	-47.24014	254.106628	-25.078548	336.96314137	0.26612574	120.5775	53802.0758796296	2006-03-08 01:49:16	53802.7300231482	2006-03-08 17:31:14	400010040	21.2481	200	21.2481	21.2499	21.2499	21.2499	3	3	3	3	1	0	0	20.4778	20.4778	56.512	0	PROCESSED	57533.1620486111	2016-05-25 03:53:21	54247	2007-05-27 00:00:00	54041.7698726852	2006-11-02 18:28:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001058	We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		JAP	0	SWG-TOO	FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010040/	Quick Look
140	SGR C BGD	265.7856	-29.8854	264.98542	-29.862996	266.313646	-6.498142	358.90876565	-0.03691694	81.9998	53789.4522106482	2006-02-23 10:51:11	53789.8349421296	2006-02-23 20:02:19	500019010	13.3073	10	13.3153	13.3153	13.3153	13.3073	2	2	2	2	1	0	0	12.2404	12.2404	33.0639	0	PROCESSED	57533.050462963	2016-05-25 01:12:40	54247	2007-05-27 00:00:00	54041.3629166667	2006-11-02 08:42:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001079	We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI MURAKAMI		JAP	0	SWG	FOSSILS OF THE GALACTIC CENTER ACTIVITY	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500019010/	Quick Look
141	1H 0707-495	107.1586	-49.5558	106.829982	-49.474426	125.752559	-70.871973	260.16951247	-17.68246857	144.7199	53707.1759143518	2005-12-03 04:13:19	53710.0974537037	2005-12-06 02:20:20	700008010	97.2291	100	97.8529	100.3891	97.2291	97.8149	4	2	4	4	1	0	0	91.8008	91.8008	252.3688	4	PROCESSED	57532.4288194444	2016-05-24 10:17:30	54247	2007-05-27 00:00:00	54059.7078472222	2006-11-20 16:59:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001040	We propose a 100 ks observation of the NLS1 1H 0707--495 in order to understand its remarkable and puzzling spectral and variability properties. The Suzaku data will help us to disentangle between the two interpretations adopted so far, namely partial covering and relativistically blurred reflection.	EXTRAGALACTIC COMPACT SOURCES	7	A	GIOVANNI MINIUTTI		JAP	0	SWG	THE EXTREME PROPERTIES OF THE NLS1 GALAXY 1H 0707-495	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700008010/	Quick Look
142	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
143	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
144	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
145	SS CYG	325.6842	43.5739	325.1931	43.344666	350.456739	52.648094	90.55430501	-7.12254626	256.8767	53692.6066203704	2005-11-18 14:33:32	53693.8646759259	2005-11-19 20:45:08	400007010	56.043	60	56.059	56.179	56.043	56.059	2	2	2	2	1	0	0	54.3572	54.3572	108.6658	2	PROCESSED	57528.0435763889	2016-05-20 01:02:45	54247	2007-05-27 00:00:00	54037.9128472222	2006-10-29 21:54:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001044	Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst.	GALACTIC POINT SOURCES	4	A	MANABU ISHIDA		JAP	0	SWG-TOO	SS CYG OBSERVATION IN OUTBURST	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400007010/	Quick Look
146	73P/SW3	17.9545	-9.1915	17.327695	-9.456837	12.929266	-15.523337	138.90931762	-71.42827213	59.4015	53893.8691666667	2006-06-07 20:51:36	53893.9356365741	2006-06-07 22:27:19	500014040	3.236	35	3.236	3.236	3.236	3.236	1	1	1	1	1	0	0	2.4909	2.4909	5.7359	0	PROCESSED	57534.5832407407	2016-05-26 13:59:52	54267	2007-06-16 00:00:00	54052.5308912037	2006-11-13 12:44:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014040/	Quick Look
147	CH CYG	291.1621	50.2424	290.833167	50.142645	313.7082	70.490137	81.86550652	15.56609243	185.7481	53739.5736458333	2006-01-04 13:46:03	53740.2919560185	2006-01-05 07:00:25	400016020	33.3058	25	33.3075	33.3378	33.3155	33.3058	2	2	2	2	1	0	0	28.4615	28.4615	62.056	1	PROCESSED	57532.6355902778	2016-05-24 15:15:15	54247	2007-05-27 00:00:00	54039.6712268518	2006-10-31 16:06:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001082	CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS.	GALACTIC POINT SOURCES	4	A	KOJI MUKAI		JAP	0	SWG	SUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNI	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400016020/	Quick Look
148	HESS J1804-216	271.1693	-21.6722	270.417896	-21.676057	271.077547	1.764239	8.44223916	-0.04647489	89.0483	53831.6120138889	2006-04-06 14:41:18	53832.4919328704	2006-04-07 11:48:23	500007010	37.5222	50	37.5222	37.5222	37.5222	37.5222	2	2	2	2	1	0	0	28.9336	28.9336	75.9901	0	PROCESSED	57533.4045138889	2016-05-25 09:42:30	54247	2007-05-27 00:00:00	54042.288900463	2006-11-03 06:56:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001029	HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	0	SWG	SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS''	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500007010/	Quick Look
149	HESS J1804-216 BGD	270.9564	-22.0176	270.203045	-22.020418	270.877317	1.420312	8.04431311	-0.04388906	89.2004	53832.4925462963	2006-04-07 11:49:16	53833.454375	2006-04-08 10:54:18	500008010	40.7171	50	40.7171	40.7171	40.7171	40.7171	2	2	2	2	1	0	0	30.6429	30.6429	83.0879	1	PROCESSED	57533.4349537037	2016-05-25 10:26:20	54247	2007-05-27 00:00:00	54056.4266666667	2006-11-17 10:14:24	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001029	HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	0	SWG	SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS''	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500008010/	Quick Look
150	RXJ_0852-4622_NW	132.2926	-45.6157	131.862494	-45.429101	157.976747	-59.482382	265.39238743	-1.14402175	137.763	53723.4478240741	2005-12-19 10:44:52	53727.3016666667	2005-12-23 07:14:24	500010010	175.453	150	175.453	175.525	175.4608	175.461	2	2	2	2	1	0	0	230.0025	230.0025	332.9437	7	PROCESSED	57532.5654513889	2016-05-24 13:34:15	54247	2007-05-27 00:00:00	54059.902662037	2006-11-20 21:39:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001048	We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		JAP	0	SWG	HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500010010/	Quick Look
151	SMC DIFFUSE 1	13.0188	-72.8206	12.579325	-73.092182	312.037754	-64.558836	302.86615918	-44.30756989	221.6864	53687.4452893518	2005-11-13 10:41:13	53688.2231944445	2005-11-14 05:21:24	500011010	46.7789	50	46.7789	46.7869	46.7869	46.7869	1	1	1	1	1	0	0	47.8684	47.8684	67.1999	0	PROCESSED	57527.967337963	2016-05-19 23:12:58	54247	2007-05-27 00:00:00	54038.3531712963	2006-10-30 08:28:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001049	We propose to use Suzaku XIS to observe regions of diffuse emission in the Magellanic Clouds. The diffuse component was identified by ROSAT PSPC observations, but has never been studied with a true spectroscopic instrument. Suzaku is well-matched to the angular size and expected temperature of the regions of diffuse emission in the LMC. Not only will such observations give a clear view of the temperature structure of this gas, they will provide a direct measurement of ambient abundances in the Clouds.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		JAP	0	SWG	DIFFUSE EMISSION IN THE MAGELLANIC CLOUDS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500011010/	Quick Look
152	73P/SW3	18.4857	-9.3839	17.859598	-9.648443	13.351737	-15.906108	140.65827116	-71.47693301	59.4008	53893.6903703704	2006-06-07 16:34:08	53893.7356365741	2006-06-07 17:39:19	500014010	3.228	35	3.228	3.228	3.228	3.228	1	1	1	1	1	0	0	3.312	3.312	3.9039	0	PROCESSED	57534.5195486111	2016-05-26 12:28:09	54267	2007-06-16 00:00:00	54052.5070949074	2006-11-13 12:10:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014010/	Quick Look
153	73P/SW3	18.2949	-9.3163	17.668546	-9.581131	13.199293	-15.770045	140.03044964	-71.46265703	59.3979	53894.3358101852	2006-06-08 08:03:34	53894.4022800926	2006-06-08 09:39:17	500014110	1.4249	35	1.4249	1.4249	1.4249	1.4249	1	1	1	1	1	0	0	1.433	1.433	5.742	0	PROCESSED	57534.5994444445	2016-05-26 14:23:12	54267	2007-06-16 00:00:00	54052.5225694444	2006-11-13 12:32:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014110/	Quick Look
154	73P/SW3	18.4874	-9.3902	17.861309	-9.65474	13.350771	-15.912562	140.66879726	-71.4825298	59.4036	53894.6018055556	2006-06-08 14:26:36	53894.680775463	2006-06-08 16:20:19	500014150	3.232	35	3.232	3.232	3.232	3.232	1	1	1	1	1	0	0	3.293	3.293	6.8159	0	PROCESSED	57534.6057638889	2016-05-26 14:32:18	54267	2007-06-16 00:00:00	54052.5265509259	2006-11-13 12:38:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014150/	Quick Look
155	CYGNUS LOOP NE3	313.7583	32.1826	313.244151	31.990973	329.188805	47.043725	75.71932756	-8.27611719	222.9011	53703.7415162037	2005-11-29 17:47:47	53704.2355208333	2005-11-30 05:39:09	500022010	21.1338	20	21.1916	21.7199	21.1338	21.3599	2	2	2	2	1	0	0	20.2445	20.2445	42.6799	1	PROCESSED	57528.1127893518	2016-05-20 02:42:25	54247	2007-05-27 00:00:00	54038.7522106482	2006-10-30 18:03:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001093	We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	0	SWG	CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500022010/	Quick Look
156	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
157	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
158	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
159	E0102-72	16.0206	-72.0231	15.615717	-72.291056	314.640431	-65.037838	301.55102123	-45.07123322	281.396	53752.9742708333	2006-01-17 23:22:57	53755.3752199074	2006-01-20 09:00:19	100044020	41.2605	20	41.268	41.8524	41.2605	41.361	3	4	3	4	1	0	0	99.7935	99.7935	207.4298	3	PROCESSED	57532.7555555556	2016-05-24 18:08:00	54247	2007-05-27 00:00:00	54040.6979513889	2006-11-01 16:45:03	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001097	We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	0	SWG	XIS FLIGHT CAIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100044020/	Quick Look
160	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
161	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
162	GC CENTER #2	266.7693	-28.6295	265.976908	-28.611884	267.143281	-5.22043	0.42794484	-0.11339991	74.7707	53821.958587963	2006-03-27 23:00:22	53823.7585069444	2006-03-29 18:12:15	500005010	88.4247	100	88.4327	88.4247	88.4327	88.4327	2	2	2	2	1	0	0	64.5911	64.5911	155.5019	2	PROCESSED	57533.3630324074	2016-05-25 08:42:46	54247	2007-05-27 00:00:00	54133.0079861111	2007-02-02 00:11:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001020	We propose to obtain high quality spectrum near the GC. The objective is to resolve 6.4, 6.7, and 6.9 keV line and determine the high energy tail and sub-structures, which may be 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.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	0	SWG	SUZAKU GALACTIC CENTER OBSERVATION PROJECT: #2 SGR B1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500005010/	Quick Look
163	4U1626-67	248.0601	-67.4675	246.801189	-67.3606	258.324109	-44.911512	321.78071552	-13.09322804	103.0359	53803.0543518518	2006-03-09 01:18:16	53805.818275463	2006-03-11 19:38:19	400015010	102.6392	100	102.654	102.6392	102.6472	102.654	2	2	2	2	1	0	0	93.3932	93.3932	238.7819	3	PROCESSED	57533.2349652778	2016-05-25 05:38:21	54247	2007-05-27 00:00:00	54042.4663657407	2006-11-03 11:11:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001081	The X-ray spectrum of the 7 second LMXRB pulsar 4U1626-67 is dominated by low energy line emission with little evedence of iron K line in the pulse phase resolved spectra. It showd also cyclotron line at 37 keV that departs from the correlation of energy cutoff cyclotron energy observed in many other X-ray pulsars. This Suzaku observation allow to characterize the overall continuum, the low energy, the iron K alpha and cyclotron lines as function of the pulse phase,	GALACTIC POINT SOURCES	4	A	LORELLA ANGELINI		JAP	0	SWG	4U1626-67: PHASE RESOLVED SPECTRA AND CYCLOTRON LINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400015010/	Quick Look
164	GALACTIC CENTER	266.5135	-28.9269	265.71928	-28.908039	266.925143	-5.522988	0.05735731	-0.07624929	270.2495	53986.0995833333	2006-09-08 02:23:24	53987.3793402778	2006-09-09 09:06:15	100048010	63.0079	50	63.0079	63.0079	63.0079	63.0079	2	2	2	2	1	0	0	60.3228	60.3228	110.5679	2	PROCESSED	57535.5201967593	2016-05-27 12:29:05	54526	2008-03-01 00:00:00	54056.4849189815	2006-11-17 11:38:17	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015007	Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	1	SWG	XIS FLIGHT CALIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100048010/	Quick Look
165	Crab nebula	83.8083	22.0272	83.05592	21.995359	84.262061	-1.290429	184.63396429	-5.64031243	86.9342	53604.5844791667	2005-08-22 14:01:39	53604.6479861111	2005-08-22 15:33:06	100007050	3.262	5	3.262	3.262	3.262	3.262	1	1	1	1	1	0	0	3.179	3.179	5.448	0	PROCESSED	57520.7490509259	2016-05-12 17:58:38	54247	2007-05-27 00:00:00	54105.3334143518	2007-01-05 08:00:07	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/ver3.0/100007050/	Quick Look
166	TYCHO SNR	6.3244	64.1507	5.624265	63.873888	42.856632	53.765731	120.08671326	1.42345384	81.1044	53913.439224537	2006-06-27 10:32:29	53915.6530555556	2006-06-29 15:40:24	500024010	101.1274	100	101.1434	101.1274	101.1434	101.1434	2	2	2	2	1	0	0	94.5123	94.5123	191.2068	3	PROCESSED	57534.8252199074	2016-05-26 19:48:19	54289	2007-07-08 00:00:00	54052.7199884259	2006-11-13 17:16:47	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001099	We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		JAP	0	SWG	SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500024010/	Quick Look
167	NEP	272.8227	66.0165	272.806643	66.002812	335.593486	88.746745	95.79277142	28.663354	126.3033	53776.2556944445	2006-02-10 06:08:12	53778.0836111111	2006-02-12 02:00:24	500026010	88.5082	80	88.5322	88.5082	88.5242	88.5322	2	2	2	2	1	0	0	83.6728	83.6728	157.902	0	PROCESSED	57532.9856481482	2016-05-24 23:39:20	54247	2007-05-27 00:00:00	54041.1403703704	2006-11-02 03:22:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000042	We propose a second Suzaku observation of the NEP region in order to constrain the long-term and short-term valiability of OVII and OIVVV emission line intensities.Short-term variability detected in the first Suzaku observation implies existence of a charge-exchange component in oVIII linem suggesting solar wind and geo corona interaction. First purpose is to confirm this with the second observtaion.Secondly, to search a long-term variability. If it is observed, it will place a further constraints on the solar wind and interplanetary medium near the Earth.	GALACTIC DIFFUSE EMISSION	5	A	SWG		JAP	0	SWG	NEP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500026010/	Quick Look
168	73P/SW3	18.0599	-9.2267	17.433228	-9.491881	13.014248	-15.596574	139.25333623	-71.43625621	59.4006	53894.0025	2006-06-08 00:03:36	53894.0689699074	2006-06-08 01:39:19	500014060	3.235	35	3.235	3.235	3.235	3.235	1	1	1	1	1	0	0	2.49	2.49	5.7359	0	PROCESSED	57534.5883796296	2016-05-26 14:07:16	54267	2007-06-16 00:00:00	54052.5346759259	2006-11-13 12:49:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014060/	Quick Look
169	73P/SW3	18.338	-9.3332	17.711705	-9.597966	13.233056	-15.802283	140.17356876	-71.46762322	59.3974	53894.4024768518	2006-06-08 09:39:34	53894.4682986111	2006-06-08 11:14:21	500014120	1.5551	35	1.5551	1.5551	1.5551	1.5551	1	1	1	1	1	0	0	1.566	1.566	5.682	0	PROCESSED	57534.5988773148	2016-05-26 14:22:23	54267	2007-06-16 00:00:00	54052.5441782407	2006-11-13 13:03:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014120/	Quick Look
170	SN1006 SE	225.8656	-42.0517	225.046486	-41.856364	235.600187	-23.734349	327.61589547	14.40537	115.0022	53765.3759259259	2006-01-30 09:01:20	53766.487662037	2006-01-31 11:42:14	500016010	51.6076	50	51.6132	51.6212	51.6212	51.6076	2	2	2	2	1	0	0	55.6704	55.6704	96.0399	2	PROCESSED	57532.8333564815	2016-05-24 20:00:02	54247	2007-05-27 00:00:00	54040.6484259259	2006-11-01 15:33:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001062	We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		JAP	0	SWG	THE EJECTA IN SN1006	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500016010/	Quick Look
171	SGR C	266.1523	-29.4673	265.354719	-29.446679	266.622211	-6.071258	359.43182832	-0.08906822	82.0001	53786.5315393518	2006-02-20 12:45:25	53789.4515509259	2006-02-23 10:50:14	500018010	106.9219	100	106.9219	106.9219	106.9219	106.9219	2	2	2	2	1	0	0	46.6069	46.6069	252.2778	2	PROCESSED	57533.0732175926	2016-05-25 01:45:26	54247	2007-05-27 00:00:00	54041.6109375	2006-11-02 14:39:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001079	We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI MURAKAMI		JAP	0	SWG	FOSSILS OF THE GALACTIC CENTER ACTIVITY	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500018010/	Quick Look
172	NGC 4945	196.3712	-49.4666	195.641165	-49.198921	217.023772	-38.637449	305.27663793	13.34118784	313.9062	53604.7788310185	2005-08-22 18:41:31	53605.1010763889	2005-08-23 02:25:33	100008010	14.338	15	14.338	14.338	14.338	14.338	2	2	2	2	1	0	0	13.8067	13.8067	27.8419	1	PROCESSED	57526.8553819444	2016-05-18 20:31:45	54247	2007-05-27 00:00:00	54035.5212152778	2006-10-27 12:30:33	3.0.22.43	4	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/ver3.0/100008010/	Quick Look
173	3C120	68.2984	5.3555	67.633855	5.251051	67.433469	-16.402094	190.37315865	-27.39441526	237.4585	53775.1527199074	2006-02-09 03:39:55	53776.2433217593	2006-02-10 05:50:23	700001010	41.9321	160	41.9321	41.9321	41.9321	41.9321	2	2	2	2	1	0	0	34.0941	34.0941	94.2219	1	PROCESSED	57532.9769791667	2016-05-24 23:26:51	54247	2007-05-27 00:00:00	53906.2470601852	2006-06-20 05:55:46	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001003	Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	0	SWG	BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001010/	Quick Look
174	PKS2155-304	329.7191	-30.2247	328.99529	-30.464273	321.189186	-16.770975	17.73226544	-52.24760927	254.1358	53704.7749884259	2005-11-30 18:35:59	53706.3613888889	2005-12-02 08:40:24	700012010	63.9114	80	63.9194	63.9114	63.9194	63.9166	2	2	2	2	1	0	0	58.0114	58.0114	137.0498	3	PROCESSED	57532.3797685185	2016-05-24 09:06:52	54247	2007-05-27 00:00:00	54038.8920138889	2006-10-30 21:24:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001100	Jets in blazars are believed to be a powerful site of particle acceleration. TeV emitting blazars are very important, because we can study very end of electron distribution near the maximum energy by using X-ray spectrum, because X-ray emission is believed to be due to synchrotron emission from the higher energy electron. Comparison of spectral index between X-ray and TeV gives us a crucial information on these source, because this is very sensitive to the particle injection and rapid cooling. In order to maximize the capability of sensitive hard X-ray observations of Suzaku, we propose reserved TOO observations for the next six months of PV phase from the TeV emitting blazars established by HESS, selected from five candidates.	EXTRAGALACTIC COMPACT SOURCES	7	A	TADAYUKI TAKAHASHI		JAP	0	SWG-TOO	RESERVED TOO OBSERVATIONS OF SELECTED TEV-BRIGHT BLAZARS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700012010/	Quick Look
175	ABELL 1795	207.2241	26.601	206.646901	26.849155	193.922602	34.994161	33.84733119	77.1817764	130.8638	53714.5034259259	2005-12-10 12:04:56	53714.7752199074	2005-12-10 18:36:19	800012010	13.0982	120	13.1062	13.0982	13.1062	13.1062	1	1	1	1	1	0	0	10.3759	10.3759	23.4639	1	PROCESSED	57532.3922453704	2016-05-24 09:24:50	54247	2007-05-27 00:00:00	54038.7903703704	2006-10-30 18:58:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012010/	Quick Look
176	Cen A	201.3695	-43.0177	200.636124	-42.757733	217.139897	-31.325572	309.51950829	19.41821819	303.9158	53601.1523032407	2005-08-19 03:39:19	53602.4098148148	2005-08-20 09:50:08	100005010	64.6759	40	64.6942	64.7658	64.6759	64.7399	5	2	5	5	1	0	0	66.2582	66.2582	108.6119	0	PROCESSED	57520.7361921296	2016-05-12 17:40:07	53705	2005-12-01 00:00:00	53905.4597106482	2006-06-19 11:01:59	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	000005		CALIBRATION	1	A	SWG		JAP	0	SWG	Cen A		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100005010/	Quick Look
177	Crab Nebula	83.727	22.1071	82.97419	22.074866	84.190219	-1.207347	184.52563634	-5.6612791	84.9996	53615.0424652778	2005-09-02 01:01:09	53615.2432175926	2005-09-02 05:50:14	100015060	6.5256	5	6.5256	6.5256	6.5256	6.5256	1	1	1	1	1	0	0	6.7599	6.7599	17.34	0	PROCESSED	57527.2534490741	2016-05-19 06:04:58	54247	2007-05-27 00:00:00	54109.1715393518	2007-01-09 04:07:01	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/ver3.0/100015060/	Quick Look
178	MCG -5-23-16	146.9445	-30.9023	146.395049	-30.669659	162.619875	-41.096298	262.72964912	17.28396386	118.3849	53711.9526388889	2005-12-07 22:51:48	53714.4939699074	2005-12-10 11:51:19	700002010	95.6774	100	95.6774	95.7174	95.7174	95.6854	2	2	2	2	1	0	0	85.5647	85.5647	219.5251	3	PROCESSED	57532.4508680556	2016-05-24 10:49:15	54247	2007-05-27 00:00:00	54039.1988310185	2006-10-31 04:46:19	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001006	We request a 100ks Suzaku observation of the bright Seyfert galaxy, MCG -5-23-16 simultaneously with approved XMM-Newton and Chandra HETG observations in December 2005. MCG -5-23-16 has one of the best known examples of a relativistically broadened iron K line. With a Swift-BAT flux of 1.6e-10 cgs (15-100 keV), it is one of the brightest AGN above 10 keV. The simultaneous observations will allow us to determine the shape of the broad relativistic Fe line after subtracting the narrow line components measured by HETG. Importantly, Suzaku's wide bandpass will accurately measure the broad-band continuum and reflection component of MCG -5-23-16, essential for constraining the broad iron line. These observations will also allow us to determine the temperature of the high energy cut-off.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		JAP	0	SWG	PROBING THE BROAD IRON LINE AND HIGH ENERGY CONTINUUM OF MCG -5-23-16 SIMULTANEOUSLY WITH SUZAKU, XMM-NEWTON AND CHANDRA	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700002010/	Quick Look
179	PG 1211+143	183.6045	14.1097	182.967898	14.387617	177.569786	14.352789	267.53559231	74.37841457	120.7913	53698.7348263889	2005-11-24 17:38:09	53701.3397453704	2005-11-27 08:09:14	700009010	96.3241	100	96.59	97.5802	96.3241	96.3241	3	2	3	3	1	0	0	84.0087	84.0087	225.0438	2	PROCESSED	57528.1616203704	2016-05-20 03:52:44	54247	2007-05-27 00:00:00	54038.7422106482	2006-10-30 17:48:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001041	A 100ks Suzaku observation of the NLS1, PG 1211+143 is proposed. Previous XMM-Newton and Chandra observation claimed both blue-shifted (0.1c) and redshifted (0.26c-0.40c) iron Kalpha absorption lines. The redshifted iron K lines may originate from matter falling onto the supermassive black hole. The high effective area and low background of Suzaku XIS above 5 keV will enable us to measure these relativistically shifted iron lines in PG 1211+143 with great accuracy. Constraining the time variability of the lines will allow us to determine the physical origins of the absorption, e.g. failed jet/outflow or gravitational redshift from a Kerr black hole. The excellent broadband capabilities of Suzaku will accurately determine the continuum, essential for modeling the iron K band.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		JAP	0	SWG	EXPLORING THE RELATIVISTICALLY SHIFTED IRON LINES IN PG 1211+143	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700009010/	Quick Look
180	CENTAURUS CLUSTER	192.2012	-41.3132	191.510497	-41.040677	209.072585	-32.853902	302.40029759	21.55583076	106.2442	53731.2579050926	2005-12-27 06:11:23	53732.1808333333	2005-12-28 04:20:24	800014010	36.5192	30	36.5192	36.5464	36.5464	36.5224	2	2	2	2	1	0	0	32.1498	32.1498	79.7399	0	PROCESSED	57532.5349652778	2016-05-24 12:50:21	54247	2007-05-27 00:00:00	54039.373900463	2006-10-31 08:58:25	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001070	A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	0	SWG	OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800014010/	Quick Look
181	A1060	159.1744	-27.531	158.58579	-27.271265	172.752913	-33.32931	269.60056717	26.48279097	103.6438	53696.6258796296	2005-11-22 15:01:16	53697.7211111111	2005-11-23 17:18:24	800003010	39.139	40	39.139	39.147	39.155	39.155	2	2	2	2	1	0	0	34.6024	34.6024	94.6259	1	PROCESSED	57528.0675462963	2016-05-20 01:37:16	54247	2007-05-27 00:00:00	54037.8583449074	2006-10-29 20:36:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001021	A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI		JAP	0	SWG	OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800003010/	Quick Look
182	NGC720	28.2529	-13.7362	27.644452	-13.982164	20.9363	-23.62893	173.01572713	-70.35499124	242.5294	53734.3673611111	2005-12-30 08:49:00	53739.5627546296	2006-01-04 13:30:22	800009010	177.1929	100	177.1929	177.1929	177.1929	177.1929	2	2	2	2	1	0	0	9.6621	9.6621	47.5408	0	PROCESSED	57532.602962963	2016-05-24 14:28:16	54247	2007-05-27 00:00:00	54039.6651736111	2006-10-31 15:57:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001031	We propose to observe an isolated elliptical galaxy NGC720 with Suzaku. Isolated elliptical galaxies are important to probe the ISM metal abundance, since their hot gas is not affected by the amibient bright intracluster medium which often exists around X-ray bright elliptical galaxies. Suzaku is expected to measure the Oxygen abundance in the ISM bettern than XMM-Newton and constrain the origin of metals in the ISM and also ICM. Dark matter content around elliptical galaxies can also be constrained better than XMM-Newton. Such a measurement is difficult for X-ray bright galaxies due to the superposition of the cluster potential.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	0	SWG	OXYGEN ABUNDANCE AND DARK MATTER CONTENT AROUDN AN ISOLATED ELLIPTICAL GALAXY NGC720	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800009010/	Quick Look
183	ABELL 1795 Far South	207.2227	26.2001	206.644395	26.44826	194.131601	34.631873	32.0541753	77.13779505	129.4115	53716.5361921296	2005-12-12 12:52:07	53717.4168865741	2005-12-13 10:00:19	800012050	40.1206	30	40.1366	40.1526	40.1206	40.1366	2	2	2	2	1	0	0	39.4373	39.4373	76.0819	1	PROCESSED	57532.4477314815	2016-05-24 10:44:44	54247	2007-05-27 00:00:00	54039.1460069445	2006-10-31 03:30:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012050/	Quick Look
184	ABELL2811	10.4703	-28.5552	9.856516	-28.82929	357.097887	-30.138768	358.34166022	-87.45073592	232.1065	53702.1678240741	2005-11-28 04:01:40	53702.8814699074	2005-11-28 21:09:19	800005010	30.6546	25	30.6626	30.6826	30.6546	30.6659	2	2	2	2	1	0	0	28.3254	28.3254	61.656	0	PROCESSED	57528.0937268518	2016-05-20 02:14:58	54247	2007-05-27 00:00:00	54038.5109722222	2006-10-30 12:15:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001025	We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYUKI TAMURA		JAP	0	SWG	THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800005010/	Quick Look
185	A426	49.9554	41.5039	49.127963	41.323287	58.608686	22.329679	150.58326426	-13.26576669	260.2176	53767.568900463	2006-02-01 13:39:13	53768.5294560185	2006-02-02 12:42:25	800010010	50.3986	50	50.4066	50.4066	50.3986	50.4066	2	2	2	2	1	0	0	54.4364	54.4364	82.9758	0	PROCESSED	57532.8781365741	2016-05-24 21:04:31	54247	2007-05-27 00:00:00	54041.0862152778	2006-11-02 02:04:09	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001036	A426 is the X-ray brightest cluster in the Sky. The core is X-ray peaked, has a short radiative cooling time, a temperature drop and a central radio source which is blowing bubbles in the intracluster medium. A radio minihalo extends over the central 6 arcmin. A coincident power-law component is seen in deep Chandra data. This is likely to be inverse Compton emission from the electron population responsible for the radio emission. The region is expected to be a luminous, extended, hard X-ray source easily detectable by the Suzaku HXD. Confirmation of this hard X-ray component will enable the magnetic field to be securely determined in the intracluster gas.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ANDREW FABIAN		JAP	0	SWG	THE HARD X-RAY FLUX FROM THE CORE OF THE PERSEUS CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800010010/	Quick Look
186	CENCL OFFSET2	192.2009	-41.1804	191.510431	-40.907877	208.999282	-32.736275	302.39848339	21.68862024	106.52	53733.2507407407	2005-12-29 06:01:04	53734.3543865741	2005-12-30 08:30:19	800016010	43.2773	40	43.2853	43.2853	43.2773	43.2933	2	2	2	2	1	0	0	35.2531	35.2531	95.332	1	PROCESSED	57532.5900578704	2016-05-24 14:09:41	54247	2007-05-27 00:00:00	54039.6041203704	2006-10-31 14:29:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001070	A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	0	SWG	OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800016010/	Quick Look
187	NGC 4636	190.7243	2.7556	190.086173	3.029415	188.766391	6.778722	297.77503713	65.54179663	112.2967	53710.1073726852	2005-12-06 02:34:37	53711.9446643518	2005-12-07 22:40:19	800018010	79.201	80	79.201	79.201	79.201	79.201	2	2	2	2	1	0	0	75.7771	75.7771	158.7278	2	PROCESSED	57532.4099421296	2016-05-24 09:50:19	54247	2007-05-27 00:00:00	54038.9551388889	2006-10-30 22:55:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001083	We propose to observe NGC 4636 for 50~ksec in a single pointing, to determine the chemical evolution of elliptical galaxies via the determination of the spatially resolved abundance of Oxygen and other elements. Being one of the most X-ray luminous ellipticals, and having been observed by both Chandra and XMM, this is also an important target to compare the capabilities of the three observatories and interpret the results of the Suzaku XIS in light of the source spectrum provided by the XMM RGS.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ENECTALI FIGUEROA-FELICIANO		JAP	0	SWG	OBSERVATION OF THE X-RAY LUMINOUS EXTENDED EARLY-TYPE GALAXY NGC 4636	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800018010/	Quick Look
188	1A1742-294(GCBGD1)	266.5239	-29.5135	265.725945	-29.49468	266.948574	-6.109181	359.5610912	-0.38914955	264.8673	53643.1880092593	2005-09-30 04:30:44	53643.2536921296	2005-09-30 06:05:19	100037020	3.273	5	3.281	3.273	3.2887	3.281	1	1	1	1	1	0	0	3.0911	3.0911	5.6719	0	PROCESSED	57527.4425347222	2016-05-19 10:37:15	54247	2007-05-27 00:00:00	54035.5547453704	2006-10-27 13:18:50	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/ver3.0/100037020/	Quick Look
189	73P/SW3	18.1606	-9.2654	17.534064	-9.530431	13.093401	-15.671197	139.58635244	-71.44823165	59.3999	53894.1358333333	2006-06-08 03:15:36	53894.2085416667	2006-06-08 05:00:18	500014080	1.8637	35	1.8637	1.8637	1.8637	1.8637	2	2	2	2	1	0	0	1.9212	1.9212	6.2779	0	PROCESSED	57534.5937731482	2016-05-26 14:15:02	54267	2007-06-16 00:00:00	54052.5243171296	2006-11-13 12:35:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014080/	Quick Look
190	73P/SW3	18.3869	-9.3535	17.760674	-9.618192	13.270909	-15.839893	140.33698221	-71.47421859	59.3991	53894.4684490741	2006-06-08 11:14:34	53894.5356365741	2006-06-08 12:51:19	500014130	1.6939	35	1.6939	1.6939	1.6939	1.6939	1	1	1	1	1	0	0	1.694	1.694	5.804	0	PROCESSED	57534.6023611111	2016-05-26 14:27:24	54267	2007-06-16 00:00:00	54052.5234722222	2006-11-13 12:33:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014130/	Quick Look
191	MCG-6-30-15	203.9717	-34.2976	203.255303	-34.04246	215.173232	-22.546653	313.28966663	27.67858669	102.4356	53758.5062962963	2006-01-23 12:09:04	53761.0835648148	2006-01-26 02:00:20	700007020	98.4834	300	98.4834	98.4834	98.4834	98.4834	2	2	2	2	1	0	0	81.8922	81.8922	222.6497	3	PROCESSED	57532.8430902778	2016-05-24 20:14:03	54247	2007-05-27 00:00:00	54059.5463773148	2006-11-20 13:06:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001035	The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales .	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREW FABIAN		JAP	0	SWG	REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007020/	Quick Look
192	N132D	81.4727	-69.6025	81.573639	-69.643574	312.317041	-85.606179	280.24276086	-32.71811202	53.1485	53597.9869444444	2005-08-15 23:41:12	53598.2398958333	2005-08-16 05:45:27	100002050	0	7	0	0	0	0	0	0	0	0	0	0	0	0	0	0	0	PROCESSED	57520.6873263889	2016-05-12 16:29:45	54247	2007-05-27 00:00:00	54230.4157291667	2007-05-10 09:58:39	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/ver3.0/100002050/	Quick Look
193	HCG62	193.274	-9.2022	192.623373	-8.930867	195.778851	-3.241931	303.62256693	53.66732525	113.6407	53755.3883333333	2006-01-20 09:19:12	53758.5002199074	2006-01-23 12:00:19	800013020	114.8488	100	114.8568	114.8488	114.8488	114.8568	2	2	2	2	1	0	0	98.7836	98.7836	268.8498	4	PROCESSED	57532.7777199074	2016-05-24 18:39:55	54247	2007-05-27 00:00:00	54040.4546064815	2006-11-01 10:54:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001057	We propose to obtain high-quality spectra of the X-ray brightest, compact group of galaxies HCG62 with Suzaku. The previous ASCA observation has reported that this group has a hard tail in the spectrum. With 100 ksec exposure, we can constrain the flux of the hard component above ~3 keV with much higher accuracy. This will give a great impact in understanding the origin of the hard emission and non-thermal populations in the IGM. Furhtermore determining the metal abundance, particularly Oxygen, in the central and outer regions will give us new, valuable information on metal enrichment processes in the group that is not dominated by a cD galaxy. Suzaku/XIS is the best-suited for our scientific objectives since it has a low background level and the unprecedented high sensitivity.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	NAOMI OTA		JAP	0	SWG	MEASURING HARD TAILS AND METAL DISTRIBUTIONS IN THE GALAXY GROUP HCG62	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800013020/	Quick Look
194	RXJ_0852-4622_NW_offset	135.1284	-47.9102	134.705364	-47.713589	163.727844	-60.335158	268.39892579	-1.13950817	140.267	53727.3040393518	2005-12-23 07:17:49	53728.368912037	2005-12-24 08:51:14	500010020	59.1784	50	59.1784	59.1925	59.2026	59.1925	2	2	2	2	1	0	0	63.4821	63.4821	91.9959	0	PROCESSED	57532.4967708333	2016-05-24 11:55:21	54247	2007-05-27 00:00:00	54039.2486226852	2006-10-31 05:58:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001048	We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		JAP	0	SWG	HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500010020/	Quick Look
195	NGC 2403	114.2007	65.5918	112.996594	65.703234	103.458828	43.277316	150.58117971	29.1798975	310.3004	53810.5896875	2006-03-16 14:09:09	53811.5884143518	2006-03-17 14:07:19	800021010	72.3687	70	72.3767	72.3687	72.3767	72.3767	2	2	2	2	1	0	0	59.3591	59.3591	86.2779	0	PROCESSED	57533.2480439815	2016-05-25 05:57:11	54247	2007-05-27 00:00:00	54042.0667708333	2006-11-03 01:36:09	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001101	We propose to observe NGC 2403, which is a nearby luminous normal spiral. Our main objective is to search and investigation of diffuse emission components. These include both rather soft (kT = 0.1 - 1 keV) ones already detected from a fair number of spirals, and hot (kT = a few keV) emission which, if established, may become an analogue to the Galactic ridge emission.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUO MAKISHIMA		JAP	0	SWG	A PROPOSAL FOR A 70 KSEC SUZAKU OBSERVATION OF THE NORMAL SPIRAL GALAXY NGC 2403	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800021010/	Quick Look
196	73P/SW3	317.9167	24.1666	317.359719	23.9609	329.535722	38.234901	71.86402338	-16.24383714	72.7109	53868.3425	2006-05-13 08:13:12	53868.4085532407	2006-05-13 09:48:19	500013040	3.225	20	3.225	3.225	3.225	3.225	1	1	1	1	1	0	0	2.677	2.677	5.7039	0	PROCESSED	57534.2934143518	2016-05-26 07:02:31	54256	2007-06-05 00:00:00	54042.2977430556	2006-11-03 07:08:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013040/	Quick Look
197	3C120	68.298	5.3556	67.633455	5.25115	67.433074	-16.401934	190.3728125	-27.39468757	237.4583	53782.5602199074	2006-02-16 13:26:43	53783.5876967593	2006-02-17 14:06:17	700001020	41.5545	160	41.5545	41.5545	41.5545	41.5545	2	2	2	2	1	0	0	36.8461	36.8461	88.772	2	PROCESSED	57533.0172685185	2016-05-25 00:24:52	54247	2007-05-27 00:00:00	54041.2956365741	2006-11-02 07:05:43	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001003	Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	0	SWG	BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001020/	Quick Look
198	3C120	68.2979	5.3541	67.633361	5.249649	67.432732	-16.403401	190.37414386	-27.39561637	262.5053	53796.9456828704	2006-03-02 22:41:47	53797.8606365741	2006-03-03 20:39:19	700001040	40.9051	160	40.9131	40.9211	40.9211	40.9051	2	2	2	2	1	0	0	40.3118	40.3118	79.0459	0	PROCESSED	57533.1408912037	2016-05-25 03:22:53	54247	2007-05-27 00:00:00	54041.627025463	2006-11-02 15:02:55	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001003	Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	0	SWG	BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001040/	Quick Look
199	NGC 2992	146.4352	-14.2714	145.83373	-14.040218	154.019094	-26.058459	249.66741784	28.82528499	102.6298	53680.5956481482	2005-11-06 14:17:44	53681.5850925926	2005-11-07 14:02:32	700005010	37.5029	120	37.5029	38.7568	37.518	37.715	2	2	2	2	1	0	0	32.073	32.073	85.4859	1	PROCESSED	57527.9475231482	2016-05-19 22:44:26	54247	2007-05-27 00:00:00	54037.5593518518	2006-10-29 13:25:28	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001013	NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	0	SWG	THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005010/	Quick Look
200	A 2218	249.0001	66.203	248.949919	66.302836	172.76704	81.613118	97.724401	38.11892096	242.3617	53644.3643402778	2005-10-01 08:44:39	53645.3446643518	2005-10-02 08:16:19	100030010	43.3629	50	43.3629	44.7173	43.4253	43.8248	2	2	2	2	1	0	0	41.4918	41.4918	84.678	1	PROCESSED	57527.4791898148	2016-05-19 11:30:02	54247	2007-05-27 00:00:00	54035.7677314815	2006-10-27 18:25:32	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/ver3.0/100030010/	Quick Look
201	X1630-472	248.5239	-47.3401	247.603368	-47.236061	254.092996	-25.076506	336.95804041	0.27755382	107.6616	53809.226412037	2006-03-15 05:26:02	53809.743912037	2006-03-15 17:51:14	400010050	23.1671	200	23.1751	23.1769	23.1768	23.1671	2	1	2	2	1	0	0	18.8605	18.8605	44.706	0	PROCESSED	57533.2189930556	2016-05-25 05:15:21	54247	2007-05-27 00:00:00	54041.9302662037	2006-11-02 22:19:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001058	We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		JAP	0	SWG-TOO	FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010050/	Quick Look
202	CH CYG	291.1168	50.2494	290.78804	50.14985	313.638835	70.5089	81.85997028	15.59541424	38.1861	53883.3112962963	2006-05-28 07:28:16	53884.1502199074	2006-05-29 03:36:19	400016030	35.144	35	35.152	35.16	35.16	35.144	1	1	1	1	1	0	0	37.459	37.459	72.4479	1	PROCESSED	57534.4573726852	2016-05-26 10:58:37	54258	2007-06-07 00:00:00	54109.7043981482	2007-01-09 16:54:20	3.0.22.43	9	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001082	CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS.	GALACTIC POINT SOURCES	4	A	KOJI MUKAI		JAP	0	SWG	SUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNI	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400016030/	Quick Look
203	FORNAX CLUSTER NORTH	54.7043	-35.2293	54.224181	-35.391159	39.001198	-52.608062	236.34100564	-53.57224957	244.9996	53741.5137847222	2006-01-06 12:19:51	53742.3336111111	2006-01-07 08:00:24	800002020	37.1921	80	37.1921	37.2161	37.2081	37.2001	2	2	2	2	1	0	0	39.2874	39.2874	70.8159	1	PROCESSED	57532.6432291667	2016-05-24 15:26:15	54247	2007-05-27 00:00:00	54039.8151041667	2006-10-31 19:33:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001018	The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	0	SWG	MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800002020/	Quick Look
204	73P/SW3	17.8996	-9.1693	17.272719	-9.434717	12.886588	-15.48163	138.7272506	-71.42013328	59.3998	53893.8025	2006-06-07 19:15:36	53893.8689699074	2006-06-07 20:51:19	500014030	3.2361	35	3.2361	3.2361	3.2361	3.2361	1	1	1	1	1	0	0	2.4331	2.4331	5.7359	0	PROCESSED	57534.5821875	2016-05-26 13:58:21	54267	2007-06-16 00:00:00	54052.5088310185	2006-11-13 12:12:43	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014030/	Quick Look
205	73P/SW3	18.2084	-9.2837	17.581929	-9.54866	13.13101	-15.70655	139.744498	-71.45365551	59.3985	53894.2087384259	2006-06-08 05:00:35	53894.2689467593	2006-06-08 06:27:17	500014090	1.5089	35	1.5089	1.5089	1.5089	1.5089	1	1	1	1	1	0	0	1.6552	1.6552	5.202	0	PROCESSED	57534.5937037037	2016-05-26 14:14:56	54267	2007-06-16 00:00:00	54052.5382986111	2006-11-13 12:55:09	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014090/	Quick Look
206	CYGNUS LOOP NE1	314.1885	31.738	313.671289	31.544868	329.414773	46.489683	75.60815027	-8.84073861	223.0005	53697.7354282407	2005-11-23 17:39:01	53698.2051388889	2005-11-24 04:55:24	500020010	20.3437	20	20.3517	20.3517	20.3517	20.3437	1	1	1	1	1	0	0	17.992	17.992	40.5759	0	PROCESSED	57528.0684837963	2016-05-20 01:38:37	54247	2007-05-27 00:00:00	54037.9167476852	2006-10-29 22:00:07	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001093	We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	0	SWG	CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500020010/	Quick Look
207	CYGNUS LOOP NE2	313.9681	31.9542	313.452396	31.761838	329.292075	46.763002	75.65570239	-8.55863001	223.0005	53698.2056134259	2005-11-24 04:56:05	53698.6766666667	2005-11-24 16:14:24	500021010	21.4135	20	21.4455	21.4375	21.4295	21.4135	2	2	2	2	1	0	0	21.6541	21.6541	40.6939	0	PROCESSED	57528.0693518518	2016-05-20 01:39:52	54247	2007-05-27 00:00:00	54038.4014351852	2006-10-30 09:38:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001093	We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	0	SWG	CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500021010/	Quick Look
208	HIGH LAT. DIFFUSE B	38.7468	-52.2774	38.331334	-52.495237	4.39034	-61.411521	272.40280946	-58.27300774	280.6379	53783.933900463	2006-02-17 22:24:49	53786.5211111111	2006-02-20 12:30:24	500027020	103.553	100	103.553	103.561	103.561	103.561	2	2	2	2	1	0	0	68.6094	68.6094	223.5238	3	PROCESSED	57533.0790972222	2016-05-25 01:53:54	54247	2007-05-27 00:00:00	54041.5670717593	2006-11-02 13:36:35	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/ver3.0/500027020/	Quick Look
209	FORNAX CLUSTER NORTH	54.7043	-35.2294	54.224181	-35.391259	39.001136	-52.608154	236.34117402	-53.57224789	244.9993	53749.1506134259	2006-01-14 03:36:53	53750.3265509259	2006-01-15 07:50:14	800002030	45.575	80	45.583	45.579	45.575	45.587	2	2	2	2	1	0	0	42.5713	42.5713	101.6	1	PROCESSED	57532.6714236111	2016-05-24 16:06:51	54247	2007-05-27 00:00:00	54039.9702777778	2006-10-31 23:17:12	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001018	The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	0	SWG	MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800002030/	Quick Look
210	RCW86 SW	220.2761	-62.6782	219.292066	-62.464185	240.754321	-44.190898	315.14426109	-2.43598628	109.6929	53778.0961689815	2006-02-12 02:18:29	53780.2814699074	2006-02-14 06:45:19	500004010	100.7659	100	100.7819	100.7659	100.7819	100.7819	2	2	2	2	1	0	0	90.6819	90.6819	188.7918	2	PROCESSED	57533.035787037	2016-05-25 00:51:32	54247	2007-05-27 00:00:00	54041.2835648148	2006-11-02 06:48:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001019	The supernova remnants (SNRs) are most convincing candidates for the acceleration of cosmic-rays. Together with the TeV gamma-ray detection by CANGAROO and HESS, it is now confirmed that at least some of the SNRs can actually accelerate electrons up to > 10 TeV. However, such studies have not provided direct information on ``protons'', which is the major component of cosmic-rays. Here we propose to measure spatial distribution of accelerated protons in the shell of RCW 86, and its association with the high energy (>10 TeV) electrons which emit synchrotron X-rays up to 50 keV. Large effective area and the good detection capability of Suzaku will be ideal tools for our scientific goal.	GALACTIC DIFFUSE EMISSION	5	A	JUN KATAOKA		JAP	0	SWG	THE FIRST DIRECT MAPPING OF ACCELERATED PROTONS IN THE SW SHELL OF RCW 86	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500004010/	Quick Look
211	73P/SW3	279.2884	33.5067	278.829487	33.462856	284.096243	56.493773	62.26395264	17.33399104	47.3721	53862.3946875	2006-05-07 09:28:21	53862.4794444444	2006-05-07 11:30:24	500012010	3.25	5	3.25	3.25	3.25	3.25	1	1	1	1	1	0	0	2.3139	2.3139	7.304	0	PROCESSED	57533.6418402778	2016-05-25 15:24:15	54256	2007-06-05 00:00:00	54042.1755671296	2006-11-03 04:12:49	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500012010/	Quick Look
212	N132D	81.1356	-69.5861	81.235257	-69.628797	313.439432	-85.525223	280.24807804	-32.83670135	53.4639	53597.5317361111	2005-08-15 12:45:42	53597.6932291667	2005-08-15 16:38:15	100002020	0	7	0	0	0	0	0	0	0	0	0	0	0	0	0	0	0	PROCESSED	57520.6768865741	2016-05-12 16:14:43	54247	2007-05-27 00:00:00	54230.4131828704	2007-05-10 09:54:59	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/ver3.0/100002020/	Quick Look
213	N132D	81.0865	-69.7023	81.190689	-69.745221	312.425808	-85.439083	280.38777612	-32.83268249	53.5118	53597.8375	2005-08-15 20:06:00	53597.9865625	2005-08-15 23:40:39	100002040	0	7	0	0	0	0	0	0	0	0	0	0	0	0	0	0	0	PROCESSED	57520.6840277778	2016-05-12 16:25:00	54247	2007-05-27 00:00:00	54230.4148726852	2007-05-10 09:57:25	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/ver3.0/100002040/	Quick Look
214	ABELL2811-OFF	10.1781	-28.7333	9.563743	-29.007637	356.740152	-30.181509	358.19144602	-87.13859798	232.6526	53702.8821296296	2005-11-28 21:10:16	53703.731412037	2005-11-29 17:33:14	800006010	33.9494	25	33.9574	33.9654	33.9494	33.9498	2	2	2	2	1	0	0	30.9056	30.9056	73.3659	1	PROCESSED	57528.1125115741	2016-05-20 02:42:01	54247	2007-05-27 00:00:00	54038.6719560185	2006-10-30 16:07:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001025	We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYUKI TAMURA		JAP	0	SWG	THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800006010/	Quick Look
215	NGC 2992	146.4592	-14.2821	145.857736	-14.050853	154.047551	-26.059819	249.69438343	28.83515423	128.4959	53717.4275462963	2005-12-13 10:15:40	53718.506412037	2005-12-14 12:09:14	700005030	46.8361	120	46.8441	46.8681	46.8361	46.8601	2	2	2	2	1	0	0	44.2983	44.2983	93.2079	1	PROCESSED	57532.4690046296	2016-05-24 11:15:22	54247	2007-05-27 00:00:00	54039.2254861111	2006-10-31 05:24:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001013	NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	0	SWG	THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005030/	Quick Look
216	SN 1987A	83.8361	-69.2786	83.928024	-69.308301	307.518784	-86.433209	279.71542477	-31.94667609	132.5904	53677.835775463	2005-11-03 20:03:31	53678.3475	2005-11-04 08:20:24	500006010	36.7863	40	36.7863	36.7863	36.7863	36.7863	2	2	2	2	1	0	0	32.9198	32.9198	44.1661	1	PROCESSED	57527.9193518518	2016-05-19 22:03:52	54247	2007-05-27 00:00:00	54037.1281481482	2006-10-29 03:04:32	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001028	SN1987A is providing us with a unique opportunity to study the supernova explosion itself and the very early phase of the supernova-remnants evolution. The supernova blast wave has started to strike the inner circumstellar ring. The neutrino flash observed at the time of explosion implies the formation of a neutron star, but no evidence of this has been detected yet. We propose to observe SN1987A for 40 ksec with Suzaku HXD and XIS. Our first goal is the search for a periodic hard signal from the putative pulsar. We also want to study the collision of the supernova blast wave with the inner ring. In order to follow the temporal evolution of the shock, we propose to observe the source with Suzaku in the early phase of the SWG PV-phase as a reference for further studies.	GALACTIC DIFFUSE EMISSION	5	A	GUENTHER HASINGER		JAP	0	SWG	SUZAKU OBSERVATION OF SN1987A : SEARCH FOR PULSAR EMISSION AND STUDY OF A NEWBORN SNR		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500006010/	Quick Look
217	GALACTIC RIDGE	281.0049	-4.0776	280.344509	-4.129178	281.602156	18.920781	28.45801897	-0.21166151	265.5297	53671.1112037037	2005-10-28 02:40:08	53673.8960069445	2005-10-30 21:30:15	500009010	93.3276	100	93.3436	93.3596	93.3436	93.3276	2	2	2	2	1	0	0	77.5364	77.5364	240.5759	0	PROCESSED	57527.7330439815	2016-05-19 17:35:35	54247	2007-05-27 00:00:00	54037.6929513889	2006-10-29 16:37:51	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001042	We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field.	GALACTIC DIFFUSE EMISSION	5	A	KEN EBISAWA		JAP	0	SWG	ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500009010/	Quick Look
218	73P/SW3	318.3252	23.9905	317.766876	23.78347	329.890581	37.931404	71.97868305	-16.64134569	72.7093	53868.4091666667	2006-05-13 09:49:12	53868.4752199074	2006-05-13 11:24:19	500013050	3.225	20	3.225	3.225	3.225	3.225	1	1	1	1	1	0	0	2.584	2.584	5.7039	0	PROCESSED	57534.2992476852	2016-05-26 07:10:55	54256	2007-06-05 00:00:00	54089.4348611111	2006-12-20 10:26:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013050/	Quick Look
219	73P/SW3	318.7382	23.8104	318.178519	23.602036	330.247137	37.622205	72.09504522	-17.04458663	72.7096	53868.4758333333	2006-05-13 11:25:12	53868.5418865741	2006-05-13 13:00:19	500013060	3.218	20	3.218	3.218	3.218	3.218	1	1	1	1	1	0	0	2.539	2.539	5.6959	0	PROCESSED	57534.3046759259	2016-05-26 07:18:44	54256	2007-06-05 00:00:00	54042.3000462963	2006-11-03 07:12:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013060/	Quick Look
220	73P/SW3	319.575	23.4516	319.012619	23.240566	330.968775	37.00001	72.3420597	-17.8575616	72.7092	53868.609212963	2006-05-13 14:37:16	53868.6738310185	2006-05-13 16:10:19	500013080	3.1644	20	3.1644	3.1644	3.1644	3.1644	1	1	1	1	1	0	0	2.986	2.986	5.5519	0	PROCESSED	57534.3120601852	2016-05-26 07:29:22	54256	2007-06-05 00:00:00	54042.3213657407	2006-11-03 07:42:46	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013080/	Quick Look
221	MCG-6-30-15	203.9706	-34.2946	203.254215	-34.039458	215.17105	-22.544253	313.28931603	27.68170589	107.0204	53744.9738310185	2006-01-09 23:22:19	53749.1390277778	2006-01-14 03:20:12	700007010	143.1965	300	143.1965	143.3162	143.2685	143.2445	2	2	2	2	1	0	0	126.2903	126.2903	359.8399	4	PROCESSED	57532.7604398148	2016-05-24 18:15:02	54247	2007-05-27 00:00:00	54040.4060416667	2006-11-01 09:44:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001035	The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales .	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREW FABIAN		JAP	0	SWG	REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007010/	Quick Look
222	ARP220	233.7664	23.5658	233.223657	23.731386	223.777121	41.366844	36.73879852	53.01919685	114.8377	53742.3490856482	2006-01-07 08:22:41	53744.9654398148	2006-01-09 23:10:14	700006010	98.5506	100	98.5586	98.5506	98.5586	98.5586	2	2	2	2	1	0	0	93.3623	93.3623	226.0419	2	PROCESSED	57532.6850925926	2016-05-24 16:26:32	54247	2007-05-27 00:00:00	54040.0356597222	2006-11-01 00:51:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001033	We propose a 100 ks observation of the nearest ultraluminous infrared galaxy (ULIG) Arp220. The major objective is to search for evidence of heavily obscured nuclei. First detection of a Compton-thick source may be possible with the HXD's sensitivity, if a powerful nucleus is present, leading to a major discovery. The good quality XIS spectrum can be decisive for the origin of the strong Fe K line, barely detected with the previous XMM-Newton observation.	EXTRAGALACTIC COMPACT SOURCES	7	A	KAZUSHI IWASAWA		JAP	0	SWG	HARD X-RAY EMISSION FROM THE NEAREST ULTRALUMINOUS INFRARED GALAXY ARP220	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700006010/	Quick Look
223	FORNAX CLUSTER NORTH	54.7022	-35.2276	54.222066	-35.389468	38.999643	-52.605839	236.33819165	-53.57399329	245.0013	53740.3046990741	2006-01-05 07:18:46	53740.493275463	2006-01-05 11:50:19	800002010	7.7635	80	7.7635	7.7635	7.7635	7.7635	1	1	1	1	1	0	0	8.2708	8.2708	16.2719	0	PROCESSED	57532.6205324074	2016-05-24 14:53:34	54247	2007-05-27 00:00:00	54039.6718518518	2006-10-31 16:07:28	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001018	The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	0	SWG	MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800002010/	Quick Look
224	A1060 OFFSET	159.5124	-27.532	158.922997	-27.271679	173.074389	-33.196781	269.88117164	26.64663217	96.4857	53694.9817708333	2005-11-20 23:33:45	53696.6231365741	2005-11-22 14:57:19	800004010	52.4025	60	52.4025	53.2025	52.4185	52.5385	2	2	2	2	1	0	0	46.2039	46.2039	141.8018	1	PROCESSED	57528.0764583333	2016-05-20 01:50:06	54247	2007-05-27 00:00:00	54038.1216666667	2006-10-30 02:55:12	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001021	A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI		JAP	0	SWG	OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800004010/	Quick Look
225	CENCL OFFSET1	192.2015	-41.4461	191.510562	-41.173577	209.146138	-32.971575	302.40210867	21.42294125	106.2765	53732.1811689815	2005-12-28 04:20:53	53733.2502199074	2005-12-29 06:00:19	800015010	44.8802	40	44.8962	44.9042	44.8802	44.9196	2	2	2	2	1	0	0	37.2267	37.2267	92.3478	2	PROCESSED	57532.5827893518	2016-05-24 13:59:13	54247	2007-05-27 00:00:00	54039.5403472222	2006-10-31 12:58:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001070	A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	0	SWG	OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800015010/	Quick Look
226	RXJ1713-3946-BKGD1	257.3853	-38.8228	256.526519	-38.759945	259.804008	-15.82642	347.63223985	0.70836337	270.0091	53638.7997685185	2005-09-25 19:11:40	53639.6542708333	2005-09-26 15:42:09	100026020	34.9284	40	34.9284	34.9284	34.9284	34.9284	2	2	2	2	1	0	0	28.3713	28.3713	73.8199	0	PROCESSED	57527.432349537	2016-05-19 10:22:35	54247	2007-05-27 00:00:00	54035.5347453704	2006-10-27 12:50:02	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/ver3.0/100026020/	Quick Look
227	ABELL2804	9.8968	-28.9096	9.281885	-29.184169	356.393467	-30.22696	357.98440451	-86.83577265	234.7036	53706.3688078704	2005-12-02 08:51:05	53707.166875	2005-12-03 04:00:18	800007010	31.6129	25	31.6129	31.6129	31.6129	31.6129	2	2	2	2	1	0	0	26.9145	26.9145	68.95	2	PROCESSED	57532.3559259259	2016-05-24 08:32:32	54247	2007-05-27 00:00:00	54038.8727893518	2006-10-30 20:56:49	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001025	We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYUKI TAMURA		JAP	0	SWG	THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800007010/	Quick Look
228	GALACTIC RIDGE	281.0036	-4.078	280.343207	-4.129572	281.600756	18.920487	28.45707071	-0.21069081	265.5303	54023.0938888889	2006-10-15 02:15:12	54025.8141087963	2006-10-17 19:32:19	500009020	98.8583	100	98.8743	98.8663	98.8583	98.8743	2	2	2	2	1	0	0	81.9519	81.9519	235.0139	1	PROCESSED	57535.9070023148	2016-05-27 21:46:05	54697	2008-08-19 00:00:00	54055.6082407407	2006-11-16 14:35:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001042	We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field.	GALACTIC DIFFUSE EMISSION	5	A	KEN EBISAWA		JAP	0	SWG	ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500009020/	Quick Look
229	73P/SW3	317.5094	24.3437	316.953773	24.139336	329.181406	38.538464	71.75290875	-15.84652301	72.7094	53868.2758333333	2006-05-13 06:37:12	53868.3418865741	2006-05-13 08:12:19	500013030	3.225	20	3.225	3.225	3.225	3.225	1	1	1	1	1	0	0	2.915	2.915	5.7039	0	PROCESSED	57534.2995023148	2016-05-26 07:11:17	54256	2007-06-05 00:00:00	54042.2712731482	2006-11-03 06:30:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013030/	Quick Look

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