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 337

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	THE CRAB OFFSETS	83.536	22.0119	82.783772	21.978746	84.009124	-1.294644	184.51119717	-5.8617583	85.703	53984.8198263889	2006-09-06 19:40:33	53984.8891666667	2006-09-06 21:20:24	101011150	3.37	2	3.37	3.37	3.37	3.37	1	1	1	1	1	0	0	3.3472	3.3472	5.9839	0	PROCESSED	57535.4824189815	2016-05-27 11:34:41	53826	2006-04-01 00:00:00	54104.9730439815	2007-01-04 23:21:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011150/	Quick Look
2	E0102.2-7219	16.0278	-72.0394	15.623254	-72.307346	314.607654	-65.046746	301.54948943	-45.0548182	34.4136	53876.719525463	2006-05-21 17:16:07	53877.1793287037	2006-05-22 04:18:14	101005020	18.1619	20	18.1619	18.1939	18.1619	18.1939	2	1	2	1	1	0	0	17.7633	17.7633	39.7199	0	PROCESSED	57534.3838425926	2016-05-26 09:12:44	53826	2006-04-01 00:00:00	53926.1422222222	2006-07-10 03:24:48	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005020/	Quick Look
3	E0102.2-7219	15.9978	-72.0424	15.592857	-72.310386	314.59194	-65.039632	301.56284618	-45.05246644	92.9794	53933.2656597222	2006-07-17 06:22:33	53933.9030439815	2006-07-17 21:40:23	101005040	22.0634	20	22.0634	22.1034	22.0634	22.0954	4	2	4	2	1	0	0	20.9823	20.9823	55.0479	1	PROCESSED	57534.9613888889	2016-05-26 23:04:24	53826	2006-04-01 00:00:00	53942.4630092593	2006-07-26 11:06:44	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005040/	Quick Look
4	E0102.2-7219	15.9812	-72.0315	15.575859	-72.299509	314.610205	-65.030381	301.5690149	-45.06369281	159.2453	53997.2263425926	2006-09-19 05:25:56	53997.562662037	2006-09-19 13:30:14	101005060	10.7907	40	10.8067	10.8067	10.7907	10.7987	2	2	2	2	1	0	0	10.3223	10.3223	29.05	0	PROCESSED	57535.6263541667	2016-05-27 15:01:57	53826	2006-04-01 00:00:00	54021.1325115741	2006-10-13 03:10:49	3.0.22.43	3	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005060/	Quick Look
5	E0102.2-7219	15.9801	-72.0277	15.574689	-72.29571	314.618019	-65.028464	301.56912514	-45.06750714	192.8855	54029.650625	2006-10-21 15:36:54	54030.2265625	2006-10-22 05:26:15	101005070	37.1305	40	37.1705	37.1305	37.1705	37.1625	3	3	3	3	1	0	0	36.4716	36.4716	49.76	0	PROCESSED	57535.9063425926	2016-05-27 21:45:08	53826	2006-04-01 00:00:00	54055.5631828704	2006-11-16 13:30:59	3.0.22.43	3	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005070/	Quick Look
6	E0102.2-7219	16.0137	-72.0201	15.608673	-72.288065	314.644734	-65.034638	301.5537348	-45.07437383	265.9905	54115.1395023148	2007-01-15 03:20:53	54115.6655555556	2007-01-15 15:58:24	101005100	22.614	20	22.614	22.614	0	22.614	1	1	0	1	1	0	0	19.1496	19.1496	45.424	1	PROCESSED	57536.8323263889	2016-05-28 19:58:33	53826	2006-04-01 00:00:00	54132.8509490741	2007-02-01 20:25:22	3.0.22.43	3	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005100/	Quick Look
7	PKS2155-304	329.7138	-30.2259	328.989973	-30.465459	321.184272	-16.770452	17.72949775	-52.24318888	57.9013	53856.2600925926	2006-05-01 06:14:32	53857.2501041667	2006-05-02 06:00:09	101006010	38.5515	30	38.5515	38.5515	38.5515	38.5515	2	2	2	2	1	0	0	23.9476	23.9476	85.5141	2	PROCESSED	57533.6080787037	2016-05-25 14:35:38	53826	2006-04-01 00:00:00	53913.2773842593	2006-06-27 06:39:26	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101006010/	Quick Look
8	RXJ1856.5-3754	284.1489	-37.9077	283.297255	-37.973755	281.50944	-15.030994	358.6011477	-17.21474589	254.2953	54028.5128472222	2006-10-20 12:18:30	54029.6405208333	2006-10-21 15:22:21	101009010	40.7841	40	40.7841	40.7841	40.7841	40.7841	2	2	2	2	1	0	0	35.1699	35.1699	97.4039	1	PROCESSED	57535.9219675926	2016-05-27 22:07:38	53826	2006-04-01 00:00:00	54055.4732523148	2006-11-16 11:21:29	3.0.22.43	3	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101009010/	Quick Look
9	CRAB	83.6301	22.0172	82.877819	21.9845	84.096537	-1.293228	184.55366892	-5.78525038	85.7026	53983.2227430556	2006-09-05 05:20:45	53983.8196643518	2006-09-05 19:40:19	101010010	20.7175	20	20.8775	20.7175	20.8935	20.8855	3	2	3	3	1	0	0	19.6071	19.6071	51.5699	1	PROCESSED	57535.464224537	2016-05-27 11:08:29	53826	2006-04-01 00:00:00	54024.6695833333	2006-10-16 16:04:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015014	HXD cal.	CALIBRATION	1	A	KAZUHIRO NAKAZAWA		JAP	1	AO1	CRAB CAL FOR HXD ON 2006 AUTUMN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101010010/	Quick Look
10	THE CRAB OFFSETS	83.6209	22.1323	82.867975	22.099554	84.093103	-1.177861	184.45137768	-5.73082135	85.7132	53983.8199537037	2006-09-05 19:40:44	53983.8891087963	2006-09-05 21:20:19	101011010	3.348	2	3.348	3.348	3.348	3.348	1	1	1	1	1	0	0	3.676	3.676	5.9679	0	PROCESSED	57535.4548263889	2016-05-27 10:54:57	53826	2006-04-01 00:00:00	54104.4418287037	2007-01-04 10:36:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011010/	Quick Look
11	THE CRAB OFFSETS	83.6254	22.076	82.87279	22.043276	84.094781	-1.234292	184.50140903	-5.75744861	85.7164	53983.951712963	2006-09-05 22:50:28	53984.0904976852	2006-09-06 02:10:19	101011030	6.703	2	6.703	6.703	6.703	6.703	1	1	1	1	1	0	0	5.4458	5.4458	11.9839	0	PROCESSED	57535.4650462963	2016-05-27 11:09:40	53826	2006-04-01 00:00:00	54104.972650463	2007-01-04 23:20:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011030/	Quick Look
12	THE CRAB OFFSETS	83.6338	21.931	82.882001	21.898319	84.09616	-1.379498	184.62870178	-5.82849289	87.5103	53996.9516550926	2006-09-18 22:50:23	53997.0140509259	2006-09-19 00:20:14	101011070	2.636	2	2.636	2.636	2.636	2.636	1	1	1	1	1	0	0	2.157	2.157	5.3839	0	PROCESSED	57535.6130092593	2016-05-27 14:42:44	53826	2006-04-01 00:00:00	54104.4160069444	2007-01-04 09:59:03	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011070/	Quick Look
13	THE CRAB OFFSETS	83.7555	22.0251	83.003144	21.993005	84.213055	-1.290417	184.60946275	-5.68280554	87.8963	53997.0840625	2006-09-19 02:01:03	53997.1529282407	2006-09-19 03:40:13	101011090	1.895	2	1.895	1.895	1.895	1.895	2	2	2	2	1	0	0	2.0815	2.0815	5.9459	0	PROCESSED	57535.6191435185	2016-05-27 14:51:34	53826	2006-04-01 00:00:00	54104.4517708333	2007-01-04 10:50:33	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011090/	Quick Look
14	THE CRAB OFFSETS	83.6927	22.0229	82.940372	21.990502	84.154781	-1.290083	184.58004352	-5.7331758	85.756	53984.5680092593	2006-09-06 13:37:56	53984.6252199074	2006-09-06 15:00:19	101011110	2.6354	2	2.6354	2.6354	2.6354	2.6354	1	1	1	1	1	0	0	2.4573	2.4573	4.942	0	PROCESSED	57535.4715046296	2016-05-27 11:18:58	53826	2006-04-01 00:00:00	54104.4321527778	2007-01-04 10:22:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011110/	Quick Look
15	THE CRAB OFFSETS	83.6616	22.0194	82.909299	21.986852	84.125816	-1.292316	184.56751127	-5.75940556	85.7473	53984.6253703704	2006-09-06 15:00:32	53984.6876967593	2006-09-06 16:30:17	101011120	2.9761	2	2.9761	2.9761	2.9761	2.9761	2	2	2	2	1	0	0	2.802	2.802	5.38	0	PROCESSED	57535.4738425926	2016-05-27 11:22:20	53826	2006-04-01 00:00:00	54104.4254513889	2007-01-04 10:12:39	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011120/	Quick Look
16	THE CRAB OFFSETS	83.5991	22.0137	82.846846	21.98085	84.067662	-1.295453	184.54117278	-5.81139714	85.7249	53984.6879398148	2006-09-06 16:30:38	53984.7572222222	2006-09-06 18:10:24	101011130	3.3661	2	3.3661	3.3661	3.3661	3.3661	1	1	1	1	1	0	0	3.19	3.19	5.9839	0	PROCESSED	57535.4770486111	2016-05-27 11:26:57	53826	2006-04-01 00:00:00	54104.4575	2007-01-04 10:58:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011130/	Quick Look
17	PERSEUS CLUSTER	49.9542	41.5047	49.126761	41.324082	58.607992	22.330697	150.58204074	-13.26559499	258.6515	54136.6651388889	2007-02-05 15:57:48	54137.6043287037	2007-02-06 14:30:14	101012020	43.8714	40	43.8954	43.8794	0	43.8714	2	2	0	2	1	0	0	41.5732	41.5732	81.1379	1	PROCESSED	57537.3356944444	2016-05-29 08:03:24	53826	2006-04-01 00:00:00	54151.6542361111	2007-02-20 15:42:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015017	we propose observations for the XIS flight calibrations during the left term of AO-1.	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	1	AO1	XIS CALIBRATIONS FOR AO1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101012020/	Quick Look
18	JUPITER	226.5694	-16.1887	225.870685	-15.99606	228.664382	1.239883	343.96536778	35.7224308	118.4901	53790.7643402778	2006-02-24 18:20:39	53791.7940277778	2006-02-25 19:03:24	401001010	37.7594	36	37.7674	37.7594	37.7674	37.7674	2	2	2	2	1	0	0	32.8361	32.8361	88.9361	1	PROCESSED	57533.0781597222	2016-05-25 01:52:33	54401	2007-10-28 00:00:00	53905.533900463	2006-06-19 12:48:49	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011003	We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure.	GALACTIC POINT SOURCES	4	C	RONALD ELSNER		USA	1	AO1	JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001010/	Quick Look
19	COMA CLUSTER OFFSET	194.6939	27.9466	194.090146	28.216217	181.281218	31.269541	60.06105128	88.1791818	318.0815	53885.0996412037	2006-05-30 02:23:29	53886.8384722222	2006-05-31 20:07:24	801044010	79.172	80	79.172	79.172	79.172	79.172	2	2	2	2	1	0	0	75.2282	75.2282	150.2049	2	PROCESSED	57534.5195949074	2016-05-26 12:28:13	54394	2007-10-21 00:00:00	53926.7587384259	2006-07-10 18:12:35	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010091	In order to determine the distribution of O of the intracluster medium of the Coma cluster, we propose to observe the central region with a 40ks exposure and the offset region with a 80ks exposure. The most important in studying the history of nucleosynthesis by SN II is the O mass in the intracluster medium. Especially, the hot cluster contains most of the metals synthesized in the past.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	1	AO1	THE DETERMINATION OF O ABUNDANCE OF THE INTRACLUSTER MEDIUM OF THE COMA CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801044010/	Quick Look
20	SS 433	287.9527	4.99	287.334904	4.905608	290.182673	27.181461	39.69879316	-2.23786427	78.6446	53833.4611458333	2006-04-08 11:04:03	53834.4579166667	2006-04-09 10:59:24	401004010	40.1976	40	40.2216	40.1976	40.2296	40.2136	2	2	2	2	1	0	0	30.4749	30.4749	86.11	2	PROCESSED	57533.4357638889	2016-05-25 10:27:30	54400	2007-10-27 00:00:00	53906.5501736111	2006-06-20 13:12:15	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010031	SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber.	GALACTIC POINT SOURCES	4	A	NOBUYUKI KAWAI		JAP	1	AO1	SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401004010/	Quick Look
21	MRK 1073	48.7759	41.9723	47.948749	41.787366	57.835678	23.02641	149.56255257	-13.3516285	258.3737	54135.7651851852	2007-02-04 18:21:52	54136.6641087963	2007-02-05 15:56:19	701007020	39.5111	40	39.5191	39.5111	0	39.5191	2	2	0	2	1	0	0	37.1814	37.1814	77.6519	0	PROCESSED	57537.3263657407	2016-05-29 07:49:58	54735	2008-09-26 00:00:00	54151.4969444445	2007-02-20 11:55:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010037	We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	1	AO1	COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701007020/	Quick Look
22	1E1207.4-5209	182.4916	-52.442	181.83735	-52.163724	209.144209	-45.784625	296.53791481	9.91413144	148.6893	54146.2087384259	2007-02-15 05:00:35	54147.6390509259	2007-02-16 15:20:14	401030020	49.8266	50	50.0734	49.8266	0	50.0894	1	2	0	1	1	0	0	44.4468	44.4468	123.576	2	PROCESSED	57537.4372337963	2016-05-29 10:29:37	54750	2008-10-11 00:00:00	54153.9886458333	2007-02-22 23:43:39	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010152	1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object.	GALACTIC POINT SOURCES	4	B	ATSUMASA YOSHIDA		JAP	1	AO1	A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401030020/	Quick Look
23	HR 9024	357.4125	36.4308	356.782155	36.152799	14.165064	34.009987	109.27773456	-24.79729068	49.8624	53939.0616782407	2006-07-23 01:28:49	53940.6016087963	2006-07-24 14:26:19	401032010	58.7757	60	58.7997	58.7757	58.7837	58.7917	2	2	2	2	1	0	0	56.0116	56.0116	133.0398	1	PROCESSED	57535.042025463	2016-05-27 01:00:31	54401	2007-10-28 00:00:00	53950.2624074074	2006-08-03 06:17:52	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011022	Suzaku-XIS is the best available instrument to study the Fe fluorescence emission from late-type evolved stars. Fe fluorescence is produced by illumination of the photosphere by ionizing coronal X-rays and its intensity depends on the height of the X-ray source. We propose to observe Fe fluorescence in the single G-type giant HR 9024 and in the active RS CVn system II Peg to obtain a direct geometrical constraint on the scale height of their coronal structures. These two stars have the brightest Fe fluorescence features of all the late-type stars observed by the Chandra-HETGS and their different stellar parameters (stellar radius, gravity, multiplicity,..) and evolutionary stage will allow us to probe the typical coronal scale for significantly different conditions.	GALACTIC POINT SOURCES	4	B	PAOLA TESTA		USA	1	AO1	GEOMETRY DIAGNOSTICS FROM FE FLUORESCENT EMISSION IN LATE-TYPE EVOLVED STARS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401032010/	Quick Look
24	BETA LYR	282.5098	33.3716	282.047998	33.312385	288.857806	55.996493	63.19266924	14.79477853	53.4974	53867.1260185185	2006-05-12 03:01:28	53867.6252199074	2006-05-12 15:00:19	401036020	21.4962	20	21.4962	21.4962	21.4962	21.4962	1	1	1	1	1	0	0	19.1642	19.1642	43.1199	2	PROCESSED	57534.2764814815	2016-05-26 06:38:08	54401	2007-10-28 00:00:00	53914.2784143518	2006-06-28 06:40:55	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011031	The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse.	GALACTIC POINT SOURCES	4	A	RICHARD IGNACE		USA	1	AO1	AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036020/	Quick Look
25	4U 1705-44	257.2295	-44.1004	256.326357	-44.0367	260.194477	-21.092135	343.32321952	-2.34240238	264.0794	53976.2429166667	2006-08-29 05:49:48	53976.7731712963	2006-08-29 18:33:22	401046010	18.3155	20	18.3155	18.3155	18.3155	18.3155	2	2	2	2	1	0	0	15.3715	15.3715	45.8099	0	PROCESSED	57535.3889236111	2016-05-27 09:20:03	54526	2008-03-01 00:00:00	54021.306087963	2006-10-13 07:20:46	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011112	We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state.	GALACTIC POINT SOURCES	4	A	ANDREW YOUNG		USA	1	AO1	REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046010/	Quick Look
26	4U 1636-536	250.2262	-53.7541	249.22979	-53.657603	256.460667	-31.236861	332.91086545	-4.81751491	91.2457	54140.3877546296	2007-02-09 09:18:22	54140.99125	2007-02-09 23:47:24	401050010	24.232	19	24.232	24.232	0	24.232	2	1	0	2	1	0	0	21.6895	21.6895	52.136	0	PROCESSED	57537.3410069445	2016-05-29 08:11:03	54525	2008-02-29 00:00:00	54151.5052893518	2007-02-20 12:07:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011117	Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.	GALACTIC POINT SOURCES	4	A	JEROEN HOMAN		USA	1	AO1	THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050010/	Quick Look
27	IGRJ16195-4945	244.8541	-49.816	243.916706	-49.695602	251.909406	-27.940354	333.49117084	0.29973526	284.0301	53998.8508333333	2006-09-20 20:25:12	53999.7231481482	2006-09-21 17:21:20	401056010	39.1486	40	39.1486	39.1486	39.1486	39.1486	2	2	2	2	1	0	0	42.2652	42.2652	75.3579	1	PROCESSED	57535.652662037	2016-05-27 15:39:50	54526	2008-03-01 00:00:00	54020.9227199074	2006-10-12 22:08:43	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011132	INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	1	AO1	HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401056010/	Quick Look
28	CYGNUS X-1	299.6124	35.133	299.141904	34.996436	313.652571	54.178807	71.28577556	3.01567368	256.2202	54038.1501273148	2006-10-30 03:36:11	54038.8225	2006-10-30 19:44:24	401059010	27.7068	30	27.7068	27.7378	27.7068	27.7068	2	1	2	2	1	0	0	27.6892	27.6892	58.0839	0	PROCESSED	57535.9949768518	2016-05-27 23:52:46	54526	2008-03-01 00:00:00	54063.4924884259	2006-11-24 11:49:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011141	We request three, 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history.	GALACTIC POINT SOURCES	4	B	MICHAEL NOWAK		USA	1	AO1	ENHANCING THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401059010/	Quick Look
29	CYGNUS LOOP	314.0133	31.992	313.497685	31.799479	329.365567	46.782128	75.70987313	-8.56406979	213.2117	54090.6869791667	2006-12-21 16:29:15	54091.1175231482	2006-12-22 02:49:14	101013020	21.004	20	21.004	21.004	0	21.004	1	1	0	1	1	0	0	18.8719	18.8719	37.168	1	PROCESSED	57536.3885185185	2016-05-28 09:19:28	53826	2006-04-01 00:00:00	54132.7085763889	2007-02-01 17:00:21	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015017	we propose observations for the XIS flight calibrations during the left term of AO-1.	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	1	AO1	XIS CALIBRATIONS FOR AO1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101013020/	Quick Look
30	LOCKMAN HOLE	162.9366	57.2557	162.165538	57.521221	137.120397	45.113941	149.70344314	53.20093146	281.8721	53872.7389583333	2006-05-17 17:44:06	53874.7939583333	2006-05-19 19:03:18	101002010	80.3982	80	80.3982	80.4062	80.4062	80.4062	3	3	3	3	1	0	0	88.854	88.854	177.5138	4	PROCESSED	57534.3694212963	2016-05-26 08:51:58	53826	2006-04-01 00:00:00	53927.7689814815	2006-07-11 18:27:20	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015003	We propose an additional observation of the Lockman Hole for a purpose of the verification of the background (CXB+NXB) modeling of HXD.	CALIBRATION	1	A	MOTOHIDE KOKUBUN		JAP	1	AO1	SUZAKU OBSERVATION OF LOCKMANHOLE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101002010/	Quick Look
31	E0102.2-7219	15.9824	-72.0369	15.577154	-72.304907	314.598987	-65.033002	301.56901677	-45.05828014	133.8232	53972.2052662037	2006-08-25 04:55:35	53973.3933333333	2006-08-26 09:26:24	101005050	68.3632	20	68.9872	68.3632	68.9872	68.9712	5	5	5	6	1	0	0	68.0024	68.0024	102.6339	1	PROCESSED	57535.3618402778	2016-05-27 08:41:03	53826	2006-04-01 00:00:00	54020.9929050926	2006-10-12 23:49:47	3.0.22.43	3	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005050/	Quick Look
32	E0102.2-7219	16.0273	-72.0256	15.62255	-72.293547	314.637137	-65.04077	301.54834682	-45.06859544	302.8131	54141.9262384259	2007-02-10 22:13:47	54142.812662037	2007-02-11 19:30:14	101005110	36.0938	20	36.1018	36.0938	0	36.1018	1	1	0	1	1	0	0	52.7038	52.7038	76.5759	1	PROCESSED	57537.3567592593	2016-05-29 08:33:44	53826	2006-04-01 00:00:00	54153.2227430556	2007-02-22 05:20:45	3.0.22.43	3	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005110/	Quick Look
33	THE CRAB OFFSETS	83.7241	22.023	82.971763	21.990753	84.183875	-1.291252	184.59560566	-5.70852703	87.5484	53997.1534490741	2006-09-19 03:40:58	53997.2154513889	2006-09-19 05:10:15	101011100	1.545	2	1.545	1.545	1.545	1.545	1	1	1	1	1	0	0	1.806	1.806	5.356	0	PROCESSED	57535.619537037	2016-05-27 14:52:08	53826	2006-04-01 00:00:00	54104.4337731482	2007-01-04 10:24:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011100/	Quick Look
34	NGC 5044 OFFSET1	198.8505	-16.143	198.184446	-15.87899	203.499232	-7.562902	311.28196707	46.33985641	290.0004	53919.3604398148	2006-07-03 08:39:02	53920.9599305556	2006-07-04 23:02:18	801047010	54.6204	60	54.6204	54.6204	54.6204	54.6204	2	2	2	2	1	0	0	45.8033	45.8033	138.1899	1	PROCESSED	57534.8941203704	2016-05-26 21:27:32	54394	2007-10-21 00:00:00	53942.4615740741	2006-07-26 11:04:40	3.0.22.43	6	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010092	We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	1	AO1	THE METAL DISTRIBUTION OF THE NGC 5044 GROUP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801047010/	Quick Look
35	GRB070328	65.0965	-34.1127	64.627027	-34.231006	53.193977	-54.420072	235.19366633	-44.98909931	291.3415	54187.3163773148	2007-03-28 07:35:35	54188.4585416667	2007-03-29 11:00:18	901005010	52.5653	40	52.5653	52.5653	0	52.5653	2	2	0	2	1	0	0	48.2428	48.2428	98.6819	2	PROCESSED	57538.0113888889	2016-05-30 00:16:24	54187	2007-03-28 00:00:00	54209.5955324074	2007-04-19 14:17:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	017004	TOO Observation of GRB 070328, REPORTED BY GCN 6224	EXTRAGALACTIC COMPACT SOURCES	9	A	SUZAKU GRB TEAM		JAP	1	TOO	TOO OBSERVATION OF GRB 070328	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/901005010/	Quick Look
36	A1831	209.8007	27.9693	209.233208	28.211522	195.74505	37.218341	40.05378223	74.96810077	288.1207	53937.1181828704	2006-07-21 02:50:11	53937.5106481482	2006-07-21 12:15:20	801077010	18.0796	18	18.0796	18.0796	18.0796	18.0796	2	2	2	2	1	0	0	17.0891	17.0891	33.8979	1	PROCESSED	57535.0011805556	2016-05-27 00:01:42	54401	2007-10-28 00:00:00	53943.553599537	2006-07-27 13:17:11	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801077010/	Quick Look
37	A1674	195.9676	67.5471	195.510877	67.814977	143.551001	62.83408	121.10331631	49.53698634	114.9985	54085.1434837963	2006-12-16 03:26:37	54087.0426388889	2006-12-18 01:01:24	801062010	68.4138	100	68.4218	68.4218	0	68.4138	2	2	0	2	1	0	0	109.0131	109.0131	164.064	2	PROCESSED	57536.3777546296	2016-05-28 09:03:58	54750	2008-10-11 00:00:00	54094.6003935185	2006-12-25 14:24:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010156	A1674 is a nearby (z=0.106) richness class 3 clsuter with Abell galaxy count of 165, while its X-ray luminsity is as low as 6e43erg/s. We have observed this cluster with ASCA and XMM-Newton, and found iregular extended X-ray emission. The X-ray spectrum can be fitted with a thin thermal model of kT ~ 3keV, but the metal abundance is 0.07 with upper limit of 0.2. We assume this cluster may be a cluster under construction. Utilizing the low background level and high sensitivity of Suzaku XIS, we aim to obtain accurate X-ray spectrum of this cluster to constrain the metal abndance of each species. We also examine possible contribution of diffuse non-thermal emission in cluster scale.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KIYOSHI HAYASHIDA		JAP	1	AO1	METAL DEFICIENT GAS OR NON THERMAL EMISSION? DIFFUSE X-RAYS IN A1674	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801062010/	Quick Look
38	CYGNUS_LOOP_P8	313.9965	31.4722	313.478406	31.279742	329.042886	46.311836	75.29540263	-8.88432445	62.5181	53868.0059837963	2006-05-13 00:08:37	53868.1717476852	2006-05-13 04:07:19	501028010	4.8706	6	4.8706	4.8706	4.8706	4.8706	2	2	2	2	1	0	0	2.328	2.328	14.316	0	PROCESSED	57534.2851736111	2016-05-26 06:50:39	54394	2007-10-21 00:00:00	53914.3326157407	2006-06-28 07:58:58	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501028010/	Quick Look
39	A1800	207.3618	28.0973	206.789109	28.345144	193.256107	36.394356	40.59651819	77.12066844	302.3644	53936.635625	2006-07-20 15:15:18	53937.1140509259	2006-07-21 02:44:14	801078010	20.0437	17	20.0473	20.0553	20.0553	20.0437	2	2	2	2	1	0	0	19.0003	19.0003	41.3319	0	PROCESSED	57535.0036458333	2016-05-27 00:05:15	54401	2007-10-28 00:00:00	53943.5299652778	2006-07-27 12:43:09	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801078010/	Quick Look
40	GC_SGR_B_EAST	267.0203	-28.3518	266.229607	-28.335406	267.358668	-4.938031	0.77973231	-0.1584432	71.8708	54162.5141203704	2007-03-03 12:20:20	54164.5273726852	2007-03-05 12:39:25	501039010	96.4018	100	96.4018	96.4018	0	96.4018	2	2	0	2	1	0	0	91.0829	91.0829	173.9318	3	PROCESSED	57537.6522800926	2016-05-29 15:39:17	54736	2008-09-27 00:00:00	54171.4429050926	2007-03-12 10:37:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010060	We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	1	AO1	OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501039010/	Quick Look
41	CYGNUS X-3	308.2593	40.981	307.808438	40.809488	328.80084	56.880196	79.93230299	0.62160244	252.424	54052.0902893518	2006-11-13 02:10:01	54054.3676388889	2006-11-15 08:49:24	401011010	99.7445	100	99.7462	99.7462	0	99.7445	2	2	0	2	1	0	0	95.3893	95.3893	196.745	1	PROCESSED	57536.1520717593	2016-05-28 03:38:59	54456	2007-12-22 00:00:00	54088.9545023148	2006-12-19 22:54:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010058	We propose an observation of the unusual X-ray binary Cygnus X-3. Cyg X-3 is a final stage of the massive binary stars consisting of a WR(N) star and a compact star. However the nature of the compact star is not well understood. We have fore scientific objective. (A)Determine the Doppler modulation of iron K lines and discuss the binary nature. (2) Determine the iron abundance in the WR wind. (3) Search for the high energy cut off about 100keV of the power law component. (4) Search for the X-ray emission from radio knots. For these four sciences, we propose 100ksec observation of Cyg X-3.	GALACTIC POINT SOURCES	4	C	SHUNJI KITAMOTO		JAP	1	AO1	WIDE BAND OBSERVATION OF CYGNUS X-3 WITH SUZAKU	SPE	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401011010/	Quick Look
42	A2665	357.7161	6.1352	357.076736	5.857083	0.350497	6.536022	96.94047732	-53.65177278	245.9817	54078.2252893518	2006-12-09 05:24:25	54078.562037037	2006-12-09 13:29:20	801076010	13.944	15	13.944	13.944	0	13.944	2	2	0	2	1	0	0	11.6073	11.6073	29.0879	0	PROCESSED	57536.2715393518	2016-05-28 06:31:01	54695	2008-08-17 00:00:00	54089.271412037	2006-12-20 06:30:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801076010/	Quick Look
43	DRACO HVC REGION B	243.9603	59.1738	243.739297	59.296448	199.753416	76.165002	90.07720195	42.68363475	80.282	53816.0059953704	2006-03-22 00:08:38	53817.4148611111	2006-03-23 09:57:24	501005010	61.632	60	61.6447	61.644	61.632	61.636	2	2	2	2	1	0	0	60.6865	60.6865	121.7099	2	PROCESSED	57533.3166319444	2016-05-25 07:35:57	54400	2007-10-27 00:00:00	53906.4964583333	2006-06-20 11:54:54	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010069	High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	1	AO1	SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE -	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501005010/	Quick Look
44	CYGNUS_LOOP_P9	311.8173	30.594	311.299257	30.409327	326.059392	46.235255	73.41991066	-7.98099126	239.9998	54416.7228935185	2007-11-12 17:20:58	54417.2502199074	2007-11-13 06:00:19	501019010	19.5656	15	19.5656	19.5656	0	19.5656	2	2	0	2	1	0	0	17.3446	17.3446	45.5379	0	PROCESSED	57540.4965393518	2016-06-01 11:55:01	54798	2008-11-28 00:00:00	54430.2327546296	2007-11-26 05:35:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501019010/	Quick Look
45	THE CRAB OFFSETS	83.5056	22.0085	82.753398	21.975199	83.980807	-1.296775	184.49889553	-5.88737418	85.6939	53984.8892708333	2006-09-06 21:20:33	53984.935	2006-09-06 22:26:24	101011160	2.7651	2	2.7651	2.7651	2.7651	2.7651	1	1	1	1	1	0	0	2.152	2.152	3.9439	0	PROCESSED	57535.4827083333	2016-05-27 11:35:06	53826	2006-04-01 00:00:00	54104.4508449074	2007-01-04 10:49:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011160/	Quick Look
46	PKS 2356-61	359.7661	-60.908	359.120501	-61.186478	324.284485	-53.222548	314.02525269	-55.07790138	249.6445	54075.7140740741	2006-12-06 17:08:16	54078.21625	2006-12-09 05:11:24	801016010	100.8372	100	100.8452	100.8372	0	100.8532	2	2	0	2	1	0	0	92.1255	92.1255	216.1579	3	PROCESSED	57536.3143171296	2016-05-28 07:32:37	54456	2007-12-22 00:00:00	54088.6546759259	2006-12-19 15:42:44	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010059	We propose a 100 ksec Suzaku observation of the radio galaxy PKS 2356-61. PKS 2356-61 is reported to reside in a group of galaxies, and a sign of a diffuse X-ray emission with a possibly high temperature surrounding PKS 2356-61 was suggested with ASCA. Our objective is the determination of the origin of the diffuse emission to evaluate AGN heating of the intragroup gas by PKS 2356-61.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	SOOJING HONG		JAP	1	AO1	HIGH TEMPERATURE GROUP OF GALAXIES SURROUNDING THE RADIO GALAXY PKS 2356-61	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801016010/	Quick Look
47	CRAB	83.6569	21.9577	82.904946	21.92513	84.118749	-1.353767	184.61755594	-5.79610428	250.9424	53830.5463425926	2006-04-05 13:06:44	53831.5925115741	2006-04-06 14:13:13	101003010	37.8323	40	37.8323	37.8533	37.8323	37.8323	1	1	1	1	1	0	0	30.989	30.989	90.3799	1	PROCESSED	57533.4323726852	2016-05-25 10:22:37	53826	2006-04-01 00:00:00	53907.1306944445	2006-06-21 03:08:12	3.0.22.43	6	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015004	Crab cal at the XIS and HXD nominal positions.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101003010/	Quick Look
48	CRAB	83.6371	22.0108	82.884853	21.978134	84.10274	-1.299909	184.56259415	-5.78319491	253.3318	53824.652650463	2006-03-30 15:39:49	53825.1668865741	2006-03-31 04:00:19	101004010	16.3632	20	16.3632	16.3728	16.365	16.365	1	1	1	1	1	0	0	9.7616	9.7616	44.426	0	PROCESSED	57533.3378009259	2016-05-25 08:06:26	53826	2006-04-01 00:00:00	53906.0621875	2006-06-20 01:29:33	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015004	Crab cal at the XIS and HXD nominal positions.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101004010/	Quick Look
49	GALACTIC CENTER	265.3803	-29.7558	264.581055	-29.731436	265.955939	-6.379444	358.83357751	0.33021849	269	54016.4324074074	2006-10-08 10:22:40	54017.0968055556	2006-10-09 02:19:24	501049010	19.5627	20	19.5627	19.5627	19.5627	19.5627	2	2	2	2	1	0	0	17.6336	17.6336	57.3959	1	PROCESSED	57535.7944675926	2016-05-27 19:04:02	54735	2008-09-26 00:00:00	54053.4403356482	2006-11-14 10:34:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501049010/	Quick Look
50	HER X-1	254.4224	35.4083	253.972328	35.484085	245.910127	57.551397	58.22535664	37.56185232	67.8783	53823.7669907407	2006-03-29 18:24:28	53824.640462963	2006-03-30 15:22:16	101001010	33.0621	40	33.0621	38.8045	33.0621	33.0701	4	3	4	4	1	0	0	26.2228	26.2228	75.4379	0	PROCESSED	57526.8178703704	2016-05-18 19:37:44	53826	2006-04-01 00:00:00	53906.9875925926	2006-06-20 23:42:08	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015002	The main purpose of this observation is to calibrate the enery scale of HXD-GSO, which show a long-term decreasing trend. Another objective is to cross-calibrate the effective area between PIN and GSO.	CALIBRATION	1	A	MOTOHIDE KOKUBUN		JAP	1	AO1	SUZAKU OBSERVATION OF HER X-1 FOR HXD CALIBRATION	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101001010/	Quick Look
51	RCW 86	221.2555	-62.3618	220.269135	-62.150858	241.140538	-43.714444	315.68741681	-2.33681001	278.3377	53959.4574652778	2006-08-12 10:58:45	53961.1294907407	2006-08-14 03:06:28	501037010	59.8054	60	59.8294	59.8054	59.8294	59.8214	2	2	2	2	1	0	0	54.405	54.405	144.42	1	PROCESSED	57535.2984259259	2016-05-27 07:09:44	54394	2007-10-21 00:00:00	54021.0740972222	2006-10-13 01:46:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010054	We propose an observation of the Northwest region of RCW 86, one of Galactic supernova remnants (SNRs). Hard X-ray continuum of RCW 86 is accompanied by Fe K line emission at 6.4keV. There is strong possibility that the origin of this line is electrons and protons accelerated in the shell of the SNR. In PV phase, the Southeast region of RCW 86 will be observed, and the density of this region is much larger than that of the Northwest region. Therefore we must compare the fluxes of Fe line and hard continuum of both regions, and discuss the correlation between the flux and the density of emitting region. Such comparative study is very useful for understanding the particle acceleration in the shell-like SNRs.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		JAP	1	AO1	RCW 86:PECULIAR SNR WITH NEUTRAL FE K LINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501037010/	Quick Look
52	E0102.2-7219	16.0029	-72.0223	15.597746	-72.29028	314.636668	-65.03255	301.55865958	-45.07240987	252.2709	54082.7869907407	2006-12-13 18:53:16	54083.1279976852	2006-12-14 03:04:19	101005090	28.226	20	28.226	28.226	0	28.226	1	1	0	1	1	0	0	23.0546	23.0546	29.4559	0	PROCESSED	57536.3258101852	2016-05-28 07:49:10	53826	2006-04-01 00:00:00	54094.5930324074	2006-12-25 14:13:58	3.0.22.43	3	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005090/	Quick Look
53	CYGNUS LOOP	314.0118	31.9912	313.496184	31.798684	329.363396	46.781909	75.70842949	-8.56360013	217.4642	54090.3953935185	2006-12-21 09:29:22	54090.6848842593	2006-12-21 16:26:14	101013010	9.102	10	9.102	9.102	0	9.102	2	2	0	2	1	0	0	9.2126	9.2126	25.006	1	PROCESSED	57536.373275463	2016-05-28 08:57:31	53826	2006-04-01 00:00:00	54108.4571990741	2007-01-08 10:58:22	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015017	we propose observations for the XIS flight calibrations during the left term of AO-1.	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	1	AO1	XIS CALIBRATIONS FOR AO1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101013010/	Quick Look
54	1E1207.4-5209	182.5062	-52.436	181.851861	-52.157726	209.149793	-45.774623	296.5458403	9.92149786	302.4939	53946.5682060185	2006-07-30 13:38:13	53948.2603587963	2006-08-01 06:14:55	401030010	96.3519	120	96.3519	102.2784	96.3679	96.3519	3	2	3	3	1	0	0	94.0498	94.0498	135.3799	1	PROCESSED	57535.1230787037	2016-05-27 02:57:14	54750	2008-10-11 00:00:00	54132.8187268518	2007-02-01 19:38:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010152	1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object.	GALACTIC POINT SOURCES	4	B	ATSUMASA YOSHIDA		JAP	1	AO1	A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401030010/	Quick Look
55	AB DOR	82.2835	-65.427	82.246883	-65.464502	16.282788	-86.671062	275.26967334	-33.00819219	154.6774	54060.0265277778	2006-11-21 00:38:12	54061.4586111111	2006-11-22 11:00:24	401031010	53.4517	80	53.4517	53.4597	0	53.4614	2	2	0	2	1	0	0	48.0334	48.0334	123.708	1	PROCESSED	57536.170462963	2016-05-28 04:05:28	54502	2008-02-06 00:00:00	54133.0222916667	2007-02-02 00:32:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011021	We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku.	GALACTIC POINT SOURCES	4	B	MARC AUDARD		USA	1	AO1	NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401031010/	Quick Look
56	RXJ1713-3946	258.1672	-39.4231	257.303004	-39.36394	260.487659	-16.371231	347.50735004	-0.13585591	267.9988	53989.9221643518	2006-09-11 22:07:55	53990.3106712963	2006-09-12 07:27:22	501065010	22.011	20	22.011	22.011	22.011	22.011	2	2	2	2	1	0	0	20.7973	20.7973	33.5579	0	PROCESSED	57535.5534606482	2016-05-27 13:16:59	54526	2008-03-01 00:00:00	54020.8390162037	2006-10-12 20:08:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501065010/	Quick Look
57	GC SGR D	267.0913	-27.9356	266.303192	-27.919557	267.412914	-4.520645	1.16847417	0.00287016	108.7996	54174.7887847222	2007-03-15 18:55:51	54176.2127199074	2007-03-17 05:06:19	501059010	62.2372	63	62.2372	62.2452	0	62.2452	2	2	0	2	1	0	0	54.3697	54.3697	123.028	0	PROCESSED	57537.7233912037	2016-05-29 17:21:41	54736	2008-09-27 00:00:00	54185.4865740741	2007-03-26 11:40:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501059010/	Quick Look
58	M106	184.7117	47.2376	184.094273	47.515109	160.404745	44.085185	138.43381178	68.89762168	287.1938	53896.5413078704	2006-06-10 12:59:29	53898.7113425926	2006-06-12 17:04:20	701095010	99.8175	100	99.8815	99.8175	99.8815	99.8815	2	2	2	2	1	0	0	97.5229	97.5229	187.4839	1	PROCESSED	57534.6515393518	2016-05-26 15:38:13	54401	2007-10-28 00:00:00	53927.2308449074	2006-07-11 05:32:25	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	013151	We propose observations of the nearby Low Luminosity AGN, M81 and M106, for 100 ks for each target. We aim to detect both targets up to ~200 keV for the first time. We will determine the photon indices of the hard X-ray power-law continuum, with searching for other possible characteristics such as Compton hump around 10-20 keV and cutoff around 100-200 keV which would lead major discoveries. We will study the shape of Fe-K line(s) around 6-7 keV and their time variances. Our goal is to compare their hard X-ray spectra with those of SWG seyfert galaxies, with unprecedented accuracy, to study the accresion mechanism of LLAGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	TAKESHI ITOH	CHRISTOPHER REYNOLDS	JUS	1	AO1	OBSERVATIONS OF HARD X-RAYS FROM LOW LUMINOSITY ACTIVE GALACTIC NUCLEI	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701095010/	Quick Look
59	CYGNUS_LOOP_P17	312.199	30.014	311.677424	29.82795	326.178147	45.573278	73.16561663	-8.59879153	61.9999	53877.7613657407	2006-05-22 18:16:22	53878.0446064815	2006-05-23 01:04:14	501034010	14.1953	14	14.1993	14.2033	14.1993	14.1953	2	2	2	2	1	0	0	14.8231	14.8231	24.464	0	PROCESSED	57534.3944328704	2016-05-26 09:27:59	54394	2007-10-21 00:00:00	53926.1395833333	2006-07-10 03:21:00	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501034010/	Quick Look
60	NGC 5044 OFFSET2	199.1117	-16.388	198.444886	-16.124395	203.827071	-7.694393	311.59229028	46.06278821	290.7836	53920.9609143518	2006-07-04 23:03:43	53922.7598842593	2006-07-06 18:14:14	801048010	62.451	60	62.451	62.451	62.451	62.451	2	2	2	2	1	0	0	57.1102	57.1102	155.3149	2	PROCESSED	57534.8962615741	2016-05-26 21:30:37	54422	2007-11-18 00:00:00	54034.2926736111	2006-10-26 07:01:27	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010092	We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	1	AO1	THE METAL DISTRIBUTION OF THE NGC 5044 GROUP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801048010/	Quick Look
61	CYGNUS LOOP	314.0129	31.9925	313.497288	31.79998	329.365408	46.782722	75.71004378	-8.56348961	212.8468	54091.1180439815	2006-12-22 02:49:59	54091.6036342593	2006-12-22 14:29:14	101013030	19.7295	20	19.7295	19.7295	0	19.7295	2	2	0	2	1	0	0	20.1005	20.1005	41.9279	1	PROCESSED	57536.3931134259	2016-05-28 09:26:05	53826	2006-04-01 00:00:00	54132.7375694444	2007-02-01 17:42:06	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015017	we propose observations for the XIS flight calibrations during the left term of AO-1.	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	1	AO1	XIS CALIBRATIONS FOR AO1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101013030/	Quick Look
62	A2495	342.5777	10.9124	341.95313	10.647232	348.269753	16.897696	81.20126485	-41.9387619	237.1467	54061.4694097222	2006-11-22 11:15:57	54062.0787037037	2006-11-23 01:53:20	801080010	18.0313	18	18.0313	18.3673	0	18.1193	2	2	0	2	1	0	0	16.3891	16.3891	52.6339	3	PROCESSED	57536.1381365741	2016-05-28 03:18:55	54695	2008-08-17 00:00:00	54088.9563194444	2006-12-19 22:57:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080010/	Quick Look
63	E0102.2-7219	16.0331	-72.0338	15.628552	-72.301739	314.621321	-65.04586	301.54662861	-45.06029066	8.2024	53841.404212963	2006-04-16 09:42:04	53841.9793865741	2006-04-16 23:30:19	101005010	21.324	40	21.34	21.324	21.332	21.34	1	1	1	1	1	0	0	16.6831	16.6831	49.6639	0	PROCESSED	57533.4651273148	2016-05-25 11:09:47	53826	2006-04-01 00:00:00	53905.6938425926	2006-06-19 16:39:08	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005010/	Quick Look
64	E0102.2-7219	16.0373	-72.0314	15.632779	-72.299334	314.627775	-65.046019	301.54456169	-45.06259438	341.0006	54177.8828587963	2007-03-18 21:11:19	54178.2994675926	2007-03-19 07:11:14	101005120	18.242	20	18.242	18.25	0	18.258	1	1	0	1	1	0	0	14.7551	14.7551	35.9839	0	PROCESSED	57537.6970601852	2016-05-29 16:43:46	53826	2006-04-01 00:00:00	54185.4459027778	2007-03-26 10:42:06	3.0.22.43	3	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005120/	Quick Look
65	FORNAX A HOST GALAXY	50.6684	-37.2029	50.191244	-37.380302	32.749558	-53.117138	240.15407206	-56.69497357	218.3809	54091.6179976852	2006-12-22 14:49:55	54092.8689699074	2006-12-23 20:51:19	801015010	48.7217	50	48.7217	48.7217	0	48.7217	2	2	0	2	1	0	0	48.3987	48.3987	108.0839	1	PROCESSED	57536.4184837963	2016-05-28 10:02:37	54735	2008-09-26 00:00:00	54132.9200347222	2007-02-01 22:04:51	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010029	We propose Suzaku observations of the Fornax A west radio lobe and the host galaxy. By measuring the inverse-Compton X-ray spectrum from the radio lobe precisely up to 20 keV and comparing with radio observation results, we are able to determine the electron energy spectrum and to derive magnetic field without any assumptions. This will be an important sample to measure the kinetic energy outflow from an active galactic nucleus.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO TASHIRO		JAP	1	AO1	RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801015010/	Quick Look
66	LMC X-2	80.025	-71.9941	80.229686	-72.041872	298.35324	-83.539153	283.14092563	-32.7117801	313.3022	53849.381712963	2006-04-24 09:09:40	53850.7731365741	2006-04-25 18:33:19	401012010	56.152	60	56.1657	56.1657	56.152	56.16	2	2	2	2	1	0	0	73.408	73.408	120.1938	1	PROCESSED	57533.5735300926	2016-05-25 13:45:53	54394	2007-10-21 00:00:00	53907.6288078704	2006-06-21 15:05:29	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010090	We propose the Suzaku observation of LMC X-2, to detect the slim disk structure in its flaring branch. The luminosity of LMC X-2 is always as luminous as the Eddington limit, and the absorption is so low that the energy spectrum can be observed over the 0.2-30 keV energy range. Then, LMC X-2 is the best target to study whether the disk structure becomes the slim disk or not.	GALACTIC POINT SOURCES	4	B	HIROMITSU TAKAHASHI		JAP	1	AO1	DETECTION OF SLIM-DISK STRUCTURE FROM LOW-MASS X-RAY BINARY LMC X-2	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401012010/	Quick Look
67	MRK 766	184.6154	29.8184	183.986779	30.095968	171.206094	28.943476	190.63186084	82.27243688	133.2599	54055.0242361111	2006-11-16 00:34:54	54057.363900463	2006-11-18 08:44:01	701035010	97.8693	150	98.1756	97.8693	0	98.1676	2	2	0	2	1	0	0	96.8931	96.8931	202.1299	2	PROCESSED	57536.189525463	2016-05-28 04:32:55	54800	2008-11-30 00:00:00	54132.8396990741	2007-02-01 20:09:10	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011328	X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components	EXTRAGALACTIC COMPACT SOURCES	7	B	TRACEY TURNER		USA	1	AO1	DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701035010/	Quick Look
68	MRK 1	19.06	33.0289	18.361574	32.765252	30.564721	23.029207	128.90716196	-29.55492804	249.7486	54111.5318171296	2007-01-11 12:45:49	54114.5836111111	2007-01-14 14:00:24	701047010	126.4441	120	126.4441	126.4441	0	126.4441	2	2	0	2	1	0	0	126.0122	126.0122	263.6237	2	PROCESSED	57637.5831944445	2016-09-06 13:59:48	54702	2008-08-24 00:00:00	54133.1552314815	2007-02-02 03:43:32	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011336	The supermassive black holes of active galactic nuclei (AGN) are fundamentally connected to the stars of their host galaxies, but it is not clear whether this relationship is evident at X-ray energies. We will test the prediction that prolific star formation is responsible for the soft X-ray emission from a Compton thick AGN that also contains a powerful circumnuclear starburst. The AGN's deep obscuration facilitates the soft X-ray measurements, and Compton thick AGN are generally significant, both as a large fraction of the local AGN population and for their contribution to the X-ray background. Furthermore, we will use the direct measurement of the intrinsic AGN luminosity to test unified AGN models and the validity of indirect luminosity indicators.	EXTRAGALACTIC COMPACT SOURCES	7	B	NANCY LEVENSON		USA	1	AO1	TESTING THE STARBURST-AGN CONNECTION AND MEASURING DEEPLY OBSCURED AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701047010/	Quick Look
69	CYGNUS_LOOP_P10	311.5744	30.3992	311.055864	30.215413	325.67249	46.135207	73.13474548	-7.93635975	240.0007	54417.2506944444	2007-11-13 06:01:00	54417.6043402778	2007-11-13 14:30:15	501020010	16.7958	10	16.7958	16.8198	0	16.8038	2	2	0	2	1	0	0	12.6729	12.6729	30.5499	0	PROCESSED	57540.5008333333	2016-06-01 12:01:12	54798	2008-11-28 00:00:00	54430.1578472222	2007-11-26 03:47:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501020010/	Quick Look
70	PUP A : INTERIOR	125.5916	-42.8951	125.161363	-42.733897	147.106586	-59.478577	260.333956	-3.34905821	276.8883	53842.5813541667	2006-04-17 13:57:09	53842.9127199074	2006-04-17 21:54:19	501088010	20.2709	20	20.2924	20.2949	20.2789	20.2709	1	1	1	1	1	0	0	19.9519	19.9519	28.6239	0	PROCESSED	57533.5042476852	2016-05-25 12:06:07	54401	2007-10-28 00:00:00	53906.8948611111	2006-06-20 21:28:36	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501088010/	Quick Look
71	NGC 4968	196.7464	-23.7282	196.071371	-23.461103	204.633939	-15.321329	307.51234678	39.00523278	298.8345	53954.7307523148	2006-08-07 17:32:17	53955.6822222222	2006-08-08 16:22:24	701005010	39.0508	40	39.0508	39.0508	39.0508	39.0508	2	2	2	2	1	0	0	35.617	35.617	82.1979	1	PROCESSED	57535.2527546296	2016-05-27 06:03:58	54408	2007-11-04 00:00:00	54020.7898148148	2006-10-12 18:57:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010037	We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	1	AO1	COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701005010/	Quick Look
72	Z235	10.9622	24.4059	10.298374	24.132304	19.875378	18.073678	120.72614401	-38.43334342	59.0539	53944.0060185185	2006-07-28 00:08:40	53944.6148032407	2006-07-28 14:45:19	801083010	20.0335	20	20.0415	20.0415	20.0415	20.0335	2	2	2	2	1	0	0	19.5263	19.5263	52.5899	1	PROCESSED	57535.0666782407	2016-05-27 01:36:01	54401	2007-10-28 00:00:00	53955.6800925926	2006-08-08 16:19:20	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801083010/	Quick Look
73	GRB060904A	237.7429	44.914	237.336952	45.063372	215.38839	62.37112	71.57699476	50.22047754	264.197	53982.4478935185	2006-09-04 10:44:58	53983.2113888889	2006-09-05 05:04:24	901001010	30.3363	30	30.3443	30.3363	30.3443	30.3443	2	2	2	2	1	0	0	28.347	28.347	65.966	0	PROCESSED	57535.45125	2016-05-27 10:49:48	53982	2006-09-04 00:00:00	54026.4650462963	2006-10-18 11:09:40	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	017001	N/A	EXTRAGALACTIC COMPACT SOURCES	9	A	SWG GRB TEAM		JAP	1	TOO	TOO OBSERVATION OF GRB060904A	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/901001010/	Quick Look
74	SWIFTJ1010.1-5747	152.7309	-57.8539	152.293849	-57.606865	193.450641	-60.897616	282.8705066	-1.37559689	290.7012	53891.2175	2006-06-05 05:13:12	53891.5544560185	2006-06-05 13:18:25	401055010	19.1717	20	19.1717	19.1717	19.1717	19.1717	2	2	2	2	1	0	0	17.8778	17.8778	29.0879	0	PROCESSED	57534.4906944444	2016-05-26 11:46:36	54401	2007-10-28 00:00:00	53926.1075347222	2006-07-10 02:34:51	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011132	INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	1	AO1	HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401055010/	Quick Look
75	JUPITER	226.5948	-16.1928	225.896045	-16.000249	228.688969	1.24261	343.98613419	35.70433361	118.4906	53791.7941319445	2006-02-25 19:03:33	53792.7940277778	2006-02-26 19:03:24	401001020	37.704	36	37.704	37.704	37.704	37.704	1	1	1	1	1	0	0	32.7781	32.7781	86.36	1	PROCESSED	57533.0943981482	2016-05-25 02:15:56	54401	2007-10-28 00:00:00	53905.5035416667	2006-06-19 12:05:06	3.0.22.43	6	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011003	We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure.	GALACTIC POINT SOURCES	4	C	RONALD ELSNER		USA	1	AO1	JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001020/	Quick Look
76	G11.2-0.3	272.8676	19.433	272.324919	19.420376	273.677117	42.836704	46.34586116	17.29738119	77.6432	53834.4626041667	2006-04-09 11:06:09	53835.6634143518	2006-04-10 15:55:19	401010010	43.9846	50	43.9926	43.9846	43.9926	43.9926	2	2	2	2	1	0	0	37.3879	37.3879	83.6799	1	PROCESSED	57533.4279166667	2016-05-25 10:16:12	54397	2007-10-24 00:00:00	53905.4671875	2006-06-19 11:12:45	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010049	The PSR 1811-1925 in a historical supernova remnant G11.2-0.3 has its characteristic age as 10 times longer than the age of the remnant. The pulsar has its period 64 ms and the hard spectrum. We suggest that the pulsar shows the signs of having the small magnetic field. The SUZAKU observation must give the answer for this hypothesis. First, HXD allows us to observe the spectrum in the high energy range, and if the cut-off would be observed, the magnetic fields of pulsar will be estimate. Seconds, XIS has the great energy resolution to determine the abundance of the shell. This would let us estimate the mass of the progenitor. Third, HXD provides the new spin down rate observation. Then, we can make sure the constancy of the spin down rate. The pulsar age mystery must be solved by SUZAKU.	GALACTIC POINT SOURCES	4	C	ASAMI HAYATO		JAP	1	AO1	CLEARING UP THE MECHANISM OF THE PSR J1811-1925 IN SNR G11.2-0.3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401010010/	Quick Look
77	SIGMA^2 CRB	243.6552	33.7881	243.181435	33.91264	231.394365	53.752123	54.56402364	46.14689859	281.1207	53969.4764467593	2006-08-22 11:26:05	53972.1925231482	2006-08-25 04:37:14	401034010	109.1604	110	109.1904	109.1604	109.1684	109.1764	2	2	2	2	1	0	0	98.8376	98.8376	234.6539	3	PROCESSED	57535.3877777778	2016-05-27 09:18:24	54526	2008-03-01 00:00:00	54021.2578587963	2006-10-13 06:11:19	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011025	Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission from RS CVn binaries. We propose to obtain 110 ksec (3 day elapsed time) observations of the RS CVn systems Sigma^2 CrB (F6V + G0V) and Sigma Gem (K0III +?). Our goals are i) to better characterize their hard (> 10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, and iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability in the 10-25 keV region provided by HXD.	GALACTIC POINT SOURCES	4	B	ALEXANDER BROWN		USA	1	AO1	SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL EMISSION ON THE RS CVN BINARIES SIGMA^2 CRB AND SIGMA GEM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401034010/	Quick Look
78	4U 1820-30	275.9207	-30.3623	275.117497	-30.389079	275.135384	-7.027059	2.78792233	-7.91550172	265.9754	53992.9234606482	2006-09-14 22:09:47	53993.6605902778	2006-09-15 15:51:15	401047010	25.7008	37	25.7008	25.8109	25.7239	25.7148	2	1	2	2	1	0	0	31.8782	31.8782	63.6339	1	PROCESSED	57535.6012962963	2016-05-27 14:25:52	54526	2008-03-01 00:00:00	54021.2227083333	2006-10-13 05:20:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011113	The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme.	GALACTIC POINT SOURCES	4	B	JON MILLER		USA	1	AO1	A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401047010/	Quick Look
79	4U 1636-536	250.2259	-53.7533	249.229501	-53.656802	256.460315	-31.236099	332.911352	-4.8168543	100.7755	54188.4720717593	2007-03-29 11:19:47	54188.7856944445	2007-03-29 18:51:24	401050050	12.2418	38	12.2498	12.2418	0	12.2498	2	1	0	2	1	0	0	11.804	11.804	27.088	0	PROCESSED	57537.9973148148	2016-05-29 23:56:08	54695	2008-08-17 00:00:00	54200.4687731482	2007-04-10 11:15:02	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011117	Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.	GALACTIC POINT SOURCES	4	A	JEROEN HOMAN		USA	1	AO1	THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050050/	Quick Look
80	4U1907+09	287.4013	9.8378	286.806482	9.755913	290.334973	32.058259	43.74739314	0.48531727	60.2599	53857.2580324074	2006-05-02 06:11:34	53858.7322222222	2006-05-03 17:34:24	401057010	58.4403	60	58.4403	58.4563	58.4483	58.4563	2	2	2	2	1	0	0	38.8215	38.8215	127.3539	1	PROCESSED	57533.6690509259	2016-05-25 16:03:26	54401	2007-10-28 00:00:00	53913.4367476852	2006-06-27 10:28:55	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011133	We propose 60ksec of Suzaku observations of the high mass X-ray binary 4U1907+09, to study the little known spectrum of the source below 2keV and to measure its behavior during its frequent dips, where matter ceases to accrete onto the magnetic poles of the neutron star. Making use of Suzaku's unique broad band capabilities, we will also perform pulse phase spectroscopy of the cyclotron line and study the parameters of the fundamental and first harmonic cyclotron lines, as 4U1907+09 is one of the few accreting neutron stars where two cyclotron lines lie within the energy range of the XIS and HXD-PIN detectors. The scientific aims of this proposal address questions within NASA's Goals and Research Focus Area ``Structure and Evolution of the Universe''.	GALACTIC POINT SOURCES	4	A	KATJA POTTSCHMIDT		USA	1	AO1	THE BROAD BAND SPECTRUM OF 4U1907+09	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401057010/	Quick Look
81	HESS J1731-347	263.0179	-34.7706	262.185573	-34.73474	264.142481	-11.47104	353.53173388	-0.68198005	79.8005	54154.7807060185	2007-02-23 18:44:13	54155.7432291667	2007-02-24 17:50:15	401099010	40.6189	38	40.6269	40.6189	0	40.6269	2	2	0	2	1	0	0	34.6479	34.6479	83.1559	0	PROCESSED	57537.4739351852	2016-05-29 11:22:28	54528	2008-03-03 00:00:00	54160.3931944444	2007-03-01 09:26:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012042	The hard (Gamma=2.0) TeV source HESS J1731-347 discovered in the H.E.S.S. Galactic plane survey has an intriguing possible counterpart seen in ROSAT survey data. The X-ray data show an unidentified, extended nebular structure with a hard spectrum, in close coincidence to the TeV source. It is plausible to assume that the same energetic particle population is responsible for the emission in both bands. Suzaku is optimally suited to establish the likely non-thermal nature of the X-ray spectrum and to search for the high-energy end of the emitting particle spectrum, which is likely visible in the HXD domain. The observations will help to clarify the nature of HESS J1731-347, which may be a new type of Galactic particle accelerator.	GALACTIC POINT SOURCES	4	A	GERD PUEHLHOFER		EUR	1	AO1	THE HIGH ENERGY PARTICLE SPECTRUM OF THE TEV/X-RAY NEBULA HESS J1731-347	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401099010/	Quick Look
82	A2572B	349.6066	18.7294	348.98329	18.45586	358.210513	21.259827	94.21850787	-38.90117923	59.1565	53922.7742939815	2006-07-06 18:34:59	53923.3002199074	2006-07-07 07:12:19	801073010	24.0595	21	24.0755	24.0595	24.0675	24.0755	2	2	2	2	1	0	0	21.4951	21.4951	45.3979	1	PROCESSED	57534.8583912037	2016-05-26 20:36:05	54401	2007-10-28 00:00:00	53930.6043055556	2006-07-14 14:30:12	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801073010/	Quick Look
83	IC 443	94.2972	22.4797	93.541644	22.498727	93.972502	-0.901975	189.13057055	2.97563306	274.0001	54166.5158680556	2007-03-07 12:22:51	54167.612025463	2007-03-08 14:41:19	501006020	44.0135	40	44.0135	44.0375	0	44.0215	2	2	0	2	1	0	0	36.3209	36.3209	94.6999	1	PROCESSED	57537.6255324074	2016-05-29 15:00:46	54736	2008-09-27 00:00:00	54172.2247800926	2007-03-13 05:23:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010040	IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution.	GALACTIC DIFFUSE EMISSION	5	B	MASANOBU OZAKI		JAP	1	AO1	UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501006020/	Quick Look
84	THE CRAB OFFSETS	83.6274	22.0499	82.874936	22.017186	84.09548	-1.260449	184.52456216	-5.76985767	85.719	53984.0906018518	2006-09-06 02:10:28	53984.1529976852	2006-09-06 03:40:19	101011040	3.353	2	3.353	3.353	3.353	3.353	1	1	1	1	1	0	0	2.414	2.414	5.3839	0	PROCESSED	57535.4661921296	2016-05-27 11:11:19	53826	2006-04-01 00:00:00	54104.4143518518	2007-01-04 09:56:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011040/	Quick Look
85	IC 443	94.2975	22.7757	93.54026	22.794725	93.963954	-0.606095	188.8694635	3.11574616	274.0004	54165.4446643518	2007-03-06 10:40:19	54166.5154398148	2007-03-07 12:22:14	501006010	42.0113	40	42.0113	42.0129	0	42.0209	2	2	0	2	1	0	0	34.6934	34.6934	92.5099	2	PROCESSED	57537.6197337963	2016-05-29 14:52:25	54736	2008-09-27 00:00:00	54174.6613541667	2007-03-15 15:52:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010040	IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution.	GALACTIC DIFFUSE EMISSION	5	B	MASANOBU OZAKI		JAP	1	AO1	UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501006010/	Quick Look
86	CYGNUS_LOOP_P1	313.519	31.9657	313.004288	31.774919	328.788742	46.92673	75.41990185	-8.25713566	240	54417.6059259259	2007-11-13 14:32:32	54418.0904976852	2007-11-14 02:10:19	501012010	16.7385	10	16.7385	16.7489	0	16.7425	2	2	0	2	1	0	0	15.7758	15.7758	41.86	1	PROCESSED	57540.5110648148	2016-06-01 12:15:56	54798	2008-11-28 00:00:00	54430.2159375	2007-11-26 05:10:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501012010/	Quick Look
87	CYGNUS_LOOP_P4	312.8083	31.361	312.292075	31.17275	327.627486	46.612051	74.56035476	-8.16867105	239.9997	54418.9382291667	2007-11-14 22:31:03	54419.3196643518	2007-11-15 07:40:19	501015010	18.279	15	18.287	18.279	0	18.287	1	1	0	1	1	0	0	14.286	14.286	32.9439	0	PROCESSED	57540.5253935185	2016-06-01 12:36:34	54798	2008-11-28 00:00:00	54430.2398726852	2007-11-26 05:45:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501015010/	Quick Look
88	CYGNUS_LOOP_P5	312.5567	31.1701	312.040041	30.982753	327.230821	46.520779	74.2739834	-8.12038976	239.9995	54419.3201388889	2007-11-15 07:41:00	54420.0627777778	2007-11-16 01:30:24	501016010	28.4062	22	28.4062	28.4062	0	28.4062	2	2	0	2	1	0	0	25.37	25.37	64.1559	1	PROCESSED	57540.538900463	2016-06-01 12:56:01	54798	2008-11-28 00:00:00	54430.4318865741	2007-11-26 10:21:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501016010/	Quick Look
89	CYGNUS_LOOP_P6	312.3057	30.9823	311.788615	30.795857	326.837045	46.431585	73.99029438	-8.06939848	240.0003	54415.3923032407	2007-11-11 09:24:55	54416.1668287037	2007-11-12 04:00:14	501017010	28.7049	22	28.7049	28.7049	0	28.7049	1	1	0	1	1	0	0	26.8878	26.8878	66.9119	0	PROCESSED	57540.490474537	2016-06-01 11:46:17	54798	2008-11-28 00:00:00	54430.18875	2007-11-26 04:31:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501017010/	Quick Look
90	CYGNUS_LOOP_P16	312.737	30.4592	312.216541	30.271212	327.037451	45.805605	73.81069789	-8.68546284	61.9998	53877.1905439815	2006-05-22 04:34:23	53877.7605671296	2006-05-22 18:15:13	501033010	23.3375	22	23.3695	23.3375	23.3695	23.3695	2	2	2	2	1	0	0	20.1184	20.1184	49.2439	2	PROCESSED	57534.3873611111	2016-05-26 09:17:48	54398	2007-10-25 00:00:00	53926.8416319445	2006-07-10 20:11:57	3.0.22.43	6	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501033010/	Quick Look
91	GC_SGR_B_NORTH	266.6955	-28.3829	265.90467	-28.36493	267.072555	-4.975375	0.60514127	0.06995468	271.4417	54002.2105555556	2006-09-24 05:03:12	54003.2919444444	2006-09-25 07:00:24	501040020	44.8295	38	44.8455	44.8295	44.8375	44.8535	2	2	2	2	1	0	0	39.9705	39.9705	93.4319	1	PROCESSED	57535.678125	2016-05-27 16:16:30	54744	2008-10-05 00:00:00	54021.2868055556	2006-10-13 06:53:00	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010060	We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	1	AO1	OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501040020/	Quick Look
92	HESS J1614-518	243.5851	-51.743	242.630135	-51.617031	251.446035	-29.987821	331.574855	-0.5276897	283.402	53993.6672222222	2006-09-15 16:00:48	53994.4571064815	2006-09-16 10:58:14	501042010	40.1777	50	40.1857	40.1777	40.1857	40.1857	2	2	2	2	1	0	0	43.5607	43.5607	68.2279	0	PROCESSED	57535.5776967593	2016-05-27 13:51:53	54526	2008-03-01 00:00:00	54020.8545833333	2006-10-12 20:30:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010073	We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	1	AO1	SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501042010/	Quick Look
93	HESS J1614-518 BG	242.0174	-52.4329	241.059171	-52.300176	250.522759	-30.865237	330.3996927	-0.37656553	291.2192	53994.4597569444	2006-09-16 11:02:03	53995.3015509259	2006-09-17 07:14:14	501043010	43.5554	50	43.5634	43.5634	43.5554	43.5634	1	1	1	1	1	0	0	50.5922	50.5922	72.7039	1	PROCESSED	57535.5823726852	2016-05-27 13:58:37	54526	2008-03-01 00:00:00	54020.8662268518	2006-10-12 20:47:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010073	We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	1	AO1	SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501043010/	Quick Look
94	GALACTIC CENTER GC3	265.5781	-29.4684	264.780645	-29.444998	266.119721	-6.086772	359.1684549	0.33584661	108.8001	54170.7951273148	2007-03-11 19:04:59	54171.3397453704	2007-03-12 08:09:14	501048010	27.4546	25	27.4786	27.4546	0	27.4786	1	1	0	1	1	0	0	24.0548	24.0548	47.0479	1	PROCESSED	57537.6483333333	2016-05-29 15:33:36	54736	2008-09-27 00:00:00	54182.2788425926	2007-03-23 06:41:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501048010/	Quick Look
95	GALACTIC CENTER	265.9089	-29.649	265.11021	-29.627197	266.414403	-6.258746	359.16615355	-0.00387238	269	54017.0975115741	2006-10-09 02:20:25	54017.5690277778	2006-10-09 13:39:24	501050010	22.0477	20	22.0477	22.0477	22.0477	22.0477	1	1	1	1	1	0	0	18.6256	18.6256	40.7359	0	PROCESSED	57535.8013194445	2016-05-27 19:13:54	54735	2008-09-26 00:00:00	54053.4127777778	2006-11-14 09:54:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501050010/	Quick Look
96	GALACTIC CENTER	265.2994	-30.4982	264.495374	-30.473432	265.90984	-7.123709	358.16648703	-0.00302139	269.0003	54018.8881828704	2006-10-10 21:18:59	54019.4209953704	2006-10-11 10:06:14	501053010	21.9086	20	21.9086	21.9321	21.9166	21.9166	1	1	1	1	1	0	0	19.948	19.948	46.0319	0	PROCESSED	57535.8190393518	2016-05-27 19:39:25	54735	2008-09-26 00:00:00	54053.5019675926	2006-11-14 12:02:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501053010/	Quick Look
97	GC SGR D EAST	267.2856	-27.6502	266.49923	-27.635104	267.579665	-4.231943	1.50163715	0.00269695	108.7997	54176.2132407407	2007-03-17 05:07:04	54177.8737731482	2007-03-18 20:58:14	501060010	64.7953	63	64.7953	64.8267	0	64.8113	2	2	0	2	1	0	0	54.6297	54.6297	143.4659	1	PROCESSED	57537.7151851852	2016-05-29 17:09:52	54736	2008-09-27 00:00:00	54185.4429050926	2007-03-26 10:37:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501060010/	Quick Look
98	RXJ1713-3946	258.5524	-39.4291	257.687827	-39.37177	260.79719	-16.352329	347.6770378	-0.38034705	267.9999	53997.5713773148	2006-09-19 13:42:47	53997.9140509259	2006-09-19 21:56:14	501069010	18.375	20	18.375	18.375	18.375	18.375	1	1	1	1	1	0	0	14.2767	14.2767	29.5999	0	PROCESSED	57535.6332060185	2016-05-27 15:11:49	54526	2008-03-01 00:00:00	54021.1502546296	2006-10-13 03:36:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501069010/	Quick Look
99	RXJ1713-3946	258.9408	-39.7267	258.073523	-39.671212	261.133474	-16.624716	347.60984156	-0.7970823	268.0009	54013.3138541667	2006-10-05 07:31:57	54013.877974537	2006-10-05 21:04:17	501072010	19.9817	20	19.9817	19.9817	19.9817	19.9817	2	2	2	2	1	0	0	16.2997	16.2997	48.718	1	PROCESSED	57535.7676736111	2016-05-27 18:25:27	54526	2008-03-01 00:00:00	54021.6599652778	2006-10-13 15:50:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501072010/	Quick Look
100	G156.2+5.7NW	74.223	52.4174	73.2357	52.339427	79.010107	29.577951	155.48379099	5.80912082	273.883	54147.6530902778	2007-02-16 15:40:27	54148.7558333333	2007-02-17 18:08:24	501075010	50.5468	50	50.5468	50.5468	0	50.5468	2	2	0	2	1	0	0	46.1958	46.1958	95.2599	0	PROCESSED	57537.3885763889	2016-05-29 09:19:33	54695	2008-08-17 00:00:00	54153.2775	2007-02-22 06:39:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011235	G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target.	GALACTIC DIFFUSE EMISSION	5	C	ROBERT PETRE		USA	1	AO1	A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501075010/	Quick Look
101	SNR G93.3+6.9 CENTER	312.9805	55.373	312.634427	55.183848	352.046818	66.979241	93.25121789	6.97467523	40.9208	53905.2215509259	2006-06-19 05:19:02	53905.6480787037	2006-06-19 15:33:14	501079010	20.5372	20	20.5452	20.5452	20.5452	20.5372	2	2	2	2	1	0	0	20.008	20.008	36.8159	0	PROCESSED	57534.7200347222	2016-05-26 17:16:51	54401	2007-10-28 00:00:00	53926.792962963	2006-07-10 19:01:52	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501079010/	Quick Look
102	SNR G93.3+6.9 S1	313.1088	55.5284	312.76382	55.338789	352.457306	67.040407	93.41888838	7.01647125	40.6424	53905.6486458333	2006-06-19 15:34:03	53905.9696064815	2006-06-19 23:16:14	501080010	15.875	15	15.875	15.8902	15.891	15.883	1	1	1	1	1	0	0	12.7588	12.7588	27.7279	1	PROCESSED	57534.7111805556	2016-05-26 17:04:06	54401	2007-10-28 00:00:00	53926.199212963	2006-07-10 04:46:52	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501080010/	Quick Look
103	SNR G93.3+6.9 S4	312.7524	55.2472	312.406034	55.058863	351.58456	66.978212	93.07038921	6.99620044	39.4008	53906.7271296296	2006-06-20 17:27:04	53907.0550347222	2006-06-21 01:19:15	501083010	15.3662	15	15.3662	15.3662	15.3662	15.3662	2	2	2	2	1	0	0	14.4694	14.4694	28.3279	1	PROCESSED	57534.7341550926	2016-05-26 17:37:11	54401	2007-10-28 00:00:00	53926.117662037	2006-07-10 02:49:26	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501083010/	Quick Look
104	HESS J1718-385	259.5512	-38.6075	258.69231	-38.554942	261.534502	-15.472357	348.79652534	-0.53531102	91.2393	54154.3587731482	2007-02-23 08:36:38	54154.7773611111	2007-02-23 18:39:24	501105010	20.744	19	20.744	20.744	0	20.744	1	1	0	1	1	0	0	15.8365	15.8365	36.1519	0	PROCESSED	57537.4491435185	2016-05-29 10:46:46	54527	2008-03-02 00:00:00	54158.2865740741	2007-02-27 06:52:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012044	HESS J1718-385 is a newly discovered TeV gamma-ray source, with an unusually hard energy spectrum, which lies in close proximity to an energetic pulsar. It is likely that this object belongs to the class of offset pulsar wind nebula (PWN), accelerating electrons and positrons up to ~100 TeV. So far no sensitive X-ray observations of this region have taken place. The synchrotron spectrum of the nebula is predicted to peak in the energy range of the Suzaku HXD. The unprecedented high energy sensitivity of this instrument is required to study the highest energy particles accelerated in this object. Spectral measurements by Suzaku would confirm the inverse-Compton origin of the VHE gamma-rays and place tight constraints on the maximum energy of accelerated electrons.	GALACTIC DIFFUSE EMISSION	5	A	JAMES HINTON		EUR	1	AO1	PROBING THE LIMITS OF PARTICLE ACCELERATION IN A NEW HARD SPECTRUM TEV GAMMA-RAY SOURCE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501105010/	Quick Look
105	G156.2+5.7 CENTER	74.723	51.7342	73.743251	51.658579	79.264036	28.862327	156.21466687	5.62934315	273.4473	54148.7568171296	2007-02-17 18:09:49	54149.9169444444	2007-02-18 22:00:24	501106010	51.2142	50	51.2222	51.2302	0	51.2142	1	1	0	1	1	0	0	46.482	46.482	100.1999	0	PROCESSED	57537.3992824074	2016-05-29 09:34:58	54695	2008-08-17 00:00:00	54158.4264351852	2007-02-27 10:14:04	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	013079	Recent observations revealed that about 10 shell-like supernova remnants (SNRs) exhibit power-law X-ray spectra with no emission line which are considered to be synchrotron radiation from high-energy electrons (larger than 1 TeV). However, all those samples are young SNRs (ages about 300-2000 yr). G156.2+5.7 is an old SNR (age about 10^4 year), but emits hard X-rays in addition to usual thin thermal emission (about 0.5 keV temperature). We propose a Suzaku observation on a center region of this SNR, where diffuse hard X-rays were detected with ASCA and XMM. Our primary objective is to determine whether or not the hard tail is synchrotron X-rays, and study cosmic-ray acceleration in this old SNR.	GALACTIC DIFFUSE EMISSION	5	B	MASARU UENO	ROBERT PETRE	JUS	1	AO1	REVEALING THE ORIGIN OF HARD X-RAY EMISSION FROM AN OLD SNR, G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501106010/	Quick Look
106	VELA X (REGION A)	128.7666	-45.458	128.346603	-45.284447	153.579861	-60.62666	263.74862198	-2.99483781	337.7597	53927.7846990741	2006-07-11 18:49:58	53929.4703819444	2006-07-13 11:17:21	501107010	60.7735	60	60.7735	60.7735	60.7735	60.7735	2	2	2	2	1	0	0	54.1611	54.1611	145.6058	3	PROCESSED	57534.9641203704	2016-05-26 23:08:20	54401	2007-10-28 00:00:00	53942.4562037037	2006-07-26 10:56:56	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014211	The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band.	GALACTIC DIFFUSE EMISSION	5	B	OLEG KARGALTSEV	KOJI MORI	USJ	1	AO1	THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501107010/	Quick Look
107	VELA X (REGION C)	127.7806	-46.2716	127.370041	-46.101802	153.218075	-61.676794	263.99736145	-4.03006469	349.189	53933.9133796296	2006-07-17 21:55:16	53934.7730787037	2006-07-18 18:33:14	501108010	29.2028	30	29.2028	29.2028	29.2028	29.2028	2	2	2	2	1	0	0	25.5929	25.5929	74.248	1	PROCESSED	57534.9868055556	2016-05-26 23:41:00	54404	2007-10-31 00:00:00	53943.4988773148	2006-07-27 11:58:23	3.0.22.43	7	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014211	The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band.	GALACTIC DIFFUSE EMISSION	5	B	OLEG KARGALTSEV	KOJI MORI	USJ	1	AO1	THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501108010/	Quick Look
108	XB1323-619	201.6454	-62.1418	200.814994	-61.88221	229.562797	-47.947963	307.02498182	0.45033402	99.5731	54109.4794907407	2007-01-09 11:30:28	54110.9168402778	2007-01-10 22:00:15	401002010	55.9368	50	55.9368	55.9368	0	55.9368	2	2	0	2	1	0	0	81.8173	81.8173	124.1769	1	PROCESSED	57536.8666087963	2016-05-28 20:47:55	54735	2008-09-26 00:00:00	54133.0271759259	2007-02-02 00:39:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010002	XB 1323-619 is a non-transient dipping LMXB and one of the few LMXB with spectrum extending to high energies. Our XMM-Newton observation revealed many lines including Fe XXV and XXVI absorption. Uniquely, the rate of bursting has increased systematically over 18 years by 15 times to every 20 min in 2006/07 making it the best source for study of absorption in bursts. Suzaku allows measurement of ADC temperature via the high energy cut-off and can give the first detection of cooling by soft photons from the neutron star from the change of cut-off energy during bursts. Curve-of-growth analysis gives the absorber temperature and tests our suggestion that absorption lines are formed in the ADC. Detailed comparison with burst theory is possible because of the regular bursting.	GALACTIC POINT SOURCES	4	C	TADAYASU DOTANI		JAP	1	AO1	BORADBAND INVESTIGATIONS OF THE DIPPING, BURSTGING LOW MASS X-RAY BINARY XB1323-619	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401002010/	Quick Look
109	THE CRAB OFFSETS	83.6343	21.9041	82.882652	21.871421	84.095437	-1.406393	184.65179297	-5.84249768	87.5094	53997.0141550926	2006-09-19 00:20:23	53997.0834953704	2006-09-19 02:00:14	101011080	2.251	2	2.251	2.251	2.251	2.251	1	1	1	1	1	0	0	2.275	2.275	5.9839	1	PROCESSED	57535.6182407407	2016-05-27 14:50:16	53826	2006-04-01 00:00:00	54104.4469675926	2007-01-04 10:43:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011080/	Quick Look
110	PKS 0558-504	89.9335	-50.4395	89.62999	-50.44058	89.864093	-73.881363	257.95137808	-28.57681508	212.4401	54121.9091203704	2007-01-21 21:49:08	54122.3529976852	2007-01-22 08:28:19	701011050	19.5154	20	19.5314	19.5154	0	19.5314	1	1	0	1	1	0	0	16.1236	16.1236	38.312	0	PROCESSED	57536.8983217593	2016-05-28 21:33:35	54735	2008-09-26 00:00:00	54137.0453240741	2007-02-06 01:05:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010057	Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	C	YOSHITO HABA		JAP	1	AO1	SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011050/	Quick Look
111	SWIFT J0350.1-5019	57.6662	-50.2998	57.309175	-50.449494	28.967165	-67.019674	259.65657878	-48.95336771	180.7044	54062.0888078704	2006-11-23 02:07:53	54062.5647453704	2006-11-23 13:33:14	701017020	19.271	23	19.271	19.271	0	19.271	1	1	0	1	1	0	0	16.74	16.74	41.097	0	PROCESSED	57536.1549768518	2016-05-28 03:43:10	54750	2008-10-11 00:00:00	54088.5939583333	2006-12-19 14:15:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010133	Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background".	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	1	AO1	DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017020/	Quick Look
112	BO 375	11.4476	41.6573	10.75946	41.384162	28.671168	33.427051	121.80050832	-21.20204189	232.9596	54135.3691666667	2007-02-04 08:51:36	54135.7592476852	2007-02-04 18:13:19	701028010	12.7798	13	12.7798	12.7798	0	12.7798	1	1	0	1	1	0	0	12.8386	12.8386	33.664	1	PROCESSED	57536.9599189815	2016-05-28 23:02:17	54695	2008-08-17 00:00:00	54151.4930324074	2007-02-20 11:49:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011120	There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	A	ALBERT KONG		USA	1	AO1	PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028010/	Quick Look
113	BO 375	11.4497	41.6556	10.761554	41.382464	28.671878	33.424815	121.80214792	-21.2037783	231.6187	54137.6100810185	2007-02-06 14:38:31	54137.9737731482	2007-02-06 23:22:14	701028020	15.5371	13	15.5371	15.5371	0	15.5371	1	1	0	1	1	0	0	14.942	14.942	31.4159	0	PROCESSED	57537.3176967593	2016-05-29 07:37:29	54695	2008-08-17 00:00:00	54151.4987731482	2007-02-20 11:58:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011120	There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	A	ALBERT KONG		USA	1	AO1	PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028020/	Quick Look
114	BO 375	11.4497	41.6556	10.761554	41.382464	28.671878	33.424815	121.80214792	-21.2037783	231.4176	54142.8248032407	2007-02-11 19:47:43	54143.2167824074	2007-02-12 05:12:10	701028030	15.0878	13	15.0878	15.0878	0	15.0878	2	2	0	2	1	0	0	15.7164	15.7164	33.8379	1	PROCESSED	57537.3535069444	2016-05-29 08:29:03	54695	2008-08-17 00:00:00	54153.1806828704	2007-02-22 04:20:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011120	There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	A	ALBERT KONG		USA	1	AO1	PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028030/	Quick Look
115	NGC 3783	174.7611	-37.7364	174.141196	-37.45925	192.677729	-36.170962	287.45850943	22.95048745	293.6402	53910.7726388889	2006-06-24 18:32:36	53912.8571412037	2006-06-26 20:34:17	701033010	75.7193	75	75.7193	75.7193	75.7193	75.7193	2	2	2	2	1	0	0	68.2993	68.2993	180.0237	0	PROCESSED	57534.7899652778	2016-05-26 18:57:33	54401	2007-10-28 00:00:00	53926.8847453704	2006-07-10 21:14:02	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011325	We propose a 75 ksec Suzaku observation of the bright Seyfert 1 NGC 3783. Absorption due to photo-ionized material in the line of sight is well-established in this source, but can lead to degeneracy during modeling: is 3-6 keV continuum curvature due to photo-ionized absorption or a relativistically broad Fe K component? The simultaneous broadband XIS/HXD coverage is needed to define the continuum emission over a wide bandpass and disentangle the various emitting and absorbing components. We can then study the ionized absorber components, establish whether or not broad Fe K emission exists, and constrain reflection components, including the Compton shoulder.	EXTRAGALACTIC COMPACT SOURCES	7	B	ALEX MARKOWITZ		USA	1	AO1	PROBING FE K EMISSION AND IONIZED ABSORPTION IN NGC 3783	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701033010/	Quick Look
116	MRK 273	206.1319	55.8192	205.671114	56.069559	168.560084	59.024421	108.09580624	59.75355315	290.8776	53923.3108333333	2006-07-07 07:27:36	53925.3356481482	2006-07-09 08:03:20	701050010	79.9046	80	79.9126	79.9046	79.9206	79.9206	2	2	2	2	1	0	0	82.8076	82.8076	174.9059	3	PROCESSED	57534.931400463	2016-05-26 22:21:13	54401	2007-10-28 00:00:00	53930.7076851852	2006-07-14 16:59:04	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011341	We wish to take advantage of the unprecedented sensitivity of Suzaku Observatory to very hard X-rays (> 10 keV) to constrain the energy source -- starburst or black-hole driven activity -- in two of the nearest and brightest ultraluminous infrared galaxies, Mrk 273 and F05189-2524. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short timescale variability, another signature of black-hole driven activity. These data will be part of S. Teng's PhD thesis at Maryland.	EXTRAGALACTIC COMPACT SOURCES	7	A	SYLVAIN VEILLEUX		USA	1	AO1	THE DOMINANT ENERGY SOURCE OF ULTRALUMINOUS INFRARED GALAXIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701050010/	Quick Look
117	APM 08279+5255	127.9265	52.7635	126.994318	52.932793	116.239859	32.72128	165.74397918	36.24189551	118.0523	54020.1580902778	2006-10-12 03:47:39	54022.3134143518	2006-10-14 07:31:19	701057010	102.3328	100	102.3408	102.3408	102.3328	102.3408	2	2	2	2	1	0	0	96.0187	96.0187	186.1858	3	PROCESSED	57535.8953125	2016-05-27 21:29:15	54702	2008-08-24 00:00:00	54053.9467013889	2006-11-14 22:43:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011353	Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	1	AO1	VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057010/	Quick Look
118	1ES 1101-232	165.8976	-23.5471	165.286971	-23.277424	177.035323	-27.087344	273.21266184	33.02701002	279.8544	53880.6859606482	2006-05-25 16:27:47	53882.2161921296	2006-05-27 05:11:19	701071010	62.4327	55	62.4407	62.4407	62.4407	62.4327	2	2	2	2	1	0	0	50.1033	50.1033	132.1939	0	PROCESSED	57534.4584027778	2016-05-26 11:00:06	54401	2007-10-28 00:00:00	53927.4165393518	2006-07-11 09:59:49	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011376	Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra.	EXTRAGALACTIC COMPACT SOURCES	7	A	ANITA REIMER		USA	1	AO1	CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701071010/	Quick Look
119	NGC 4992	197.2442	11.5776	196.620329	11.84391	191.275652	17.435393	318.61367169	73.91298788	297.9177	53904.2287615741	2006-06-18 05:29:25	53905.2112615741	2006-06-19 05:04:13	701080010	38.7886	40	38.7886	38.7886	38.7886	38.7886	2	2	2	2	1	0	0	33.6179	33.6179	84.8819	1	PROCESSED	57534.7313657407	2016-05-26 17:33:10	54422	2007-11-18 00:00:00	53926.1865856482	2006-07-10 04:28:41	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012016	The high-energy detectors onboard Swift and INTEGRAL have started to survey the hard X-ray sky above 10 keV. Although limited to bright X-ray fluxes (~10^-11 cgs), the large area surveyed so far has allowed to build up sizable sa mples of hard X-ray selected AGN almost unbiased against X-ray absorption. The AGN content of these surveys is dominated by obscured AGN. We have identified 3 objects which are most likely obscured by Compton-thick matter and very bright above 10 keV. We propose to observe them with Suzaku for 40 ks each to study their broad-band X-ray spectra and unveil previously unknown nearby heavily obscured AGN, with important consequences for the study of the AGN evolution and the synthesis of the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREA COMASTRI		EUR	1	AO1	BRIGHT COMPTON THICK GALAXIES IN THE BACKYARD	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701080010/	Quick Look
120	MKN 841	226.022	10.498	225.418561	10.69235	220.178743	26.653826	11.31218444	54.65057921	105.7688	54122.3650925926	2007-01-22 08:45:44	54123.6063541667	2007-01-23 14:33:09	701084010	51.7528	50	51.7928	51.7528	0	51.7928	2	2	0	2	1	0	0	43.7077	43.7077	107.2379	1	PROCESSED	57536.9356481482	2016-05-28 22:27:20	54777	2008-11-07 00:00:00	54139.3030208333	2007-02-08 07:16:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012028	We propose to perform two 50 ks Suzaku observations of Mkn 841, at an interval of a few months, in order to elucidate the origin of its different X-ray components. Strong soft excess and complex iron line profile are known to be present in this source and recent XMM observations reveal their extreme and puzzling spectral and temporal behaviors. Nevertheless, while the XMM observations help to better constrain their natures, their physical interpretation strongly suffer from the lack of data above 10 keV. Two dedicated Suzaku observations will provide crucial information for our understanding of these components, allowing 1) to obtain high S/N and striclty simultaneous broad band X-ray spectra from the soft X-ray up to the reflection bump and 2) to study their spectral variability behaviors	EXTRAGALACTIC COMPACT SOURCES	7	B	PIERRE-OLIVIER PETRUCCI		EUR	1	AO1	PROBING THE ORIGIN OF THE STRONG SOFT EXCESS AND PUZZLING REFLECTION COMPONENTS IN MKN 841	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701084010/	Quick Look
121	GB1428+4217	217.5879	42.0673	217.100189	42.288572	194.201902	52.635769	75.8575282	64.90635728	315.7011	53898.716400463	2006-06-12 17:11:37	53899.8336111111	2006-06-13 20:00:24	701092010	48.6956	50	48.6956	48.6956	48.6956	48.6956	2	2	2	2	1	0	0	43.4943	43.4943	96.5159	1	PROCESSED	57534.6334259259	2016-05-26 15:12:08	54394	2007-10-21 00:00:00	53926.3635069444	2006-07-10 08:43:27	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012043	We propose to observe GB1428+4217 at z=4.72 for 50ks with Suzaku in order to determine its spectrum up to 45 keV, corresponding to a rest-frame energy of ~250 keV. This will allow to robustly model the spectrum in terms of a hard power-law and a Comptonization component from the scattering of `cold' electrons in the jet onto the soft nuclear photon field, as qualitatively hinted by XMM-Newton available data. This would be the first detection of such a feature in blazars and would directly and uniquely give information on the power of the relativistic jets in this source.	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREW FABIAN		EUR	1	AO1	JET POWER OF THE DISTANT EXTREME LUMINOSITY BLAZAR GB1428+4217	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701092010/	Quick Look
122	F05189-2524	80.2383	-25.4117	79.728122	-25.460147	76.667297	-48.403351	227.93752087	-30.32292957	290.8212	53835.6784259259	2006-04-10 16:16:56	53837.6467708333	2006-04-12 15:31:21	701097010	78.1555	80	78.1555	78.1635	78.1555	78.1555	2	2	2	2	1	0	0	51.7402	51.7402	169.9899	2	PROCESSED	57533.4937268518	2016-05-25 11:50:58	54401	2007-10-28 00:00:00	53906.8811689815	2006-06-20 21:08:53	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014341	We wish to take advantage of the unprecedented sensitivity of Suzaku Observatory to very hard X-rays (> 10 keV) to constrain the energy source -- starburst or black-hole driven activity -- in two of the nearest and brightest ultraluminous infrared galaxies, Mrk 273 and F05189-2524. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short timescale variability, another signature of black-hole driven activity. These data will be part of S. Teng's PhD thesis at Maryland.	EXTRAGALACTIC COMPACT SOURCES	7	A	SYLVAIN VEILLEUX	NAOHISA ANABUKI	USJ	1	AO1	THE DOMINANT ENERGY SOURCE OF ULTRALUMINOUS INFRARED GALAXIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701097010/	Quick Look
123	A2104W	234.9146	-3.2969	234.261116	-3.135581	233.381893	15.795133	2.73337641	39.30878407	117.9077	54121.3401388889	2007-01-21 08:09:48	54121.8960532407	2007-01-21 21:30:19	801001010	19.9269	20	19.9269	19.9269	0	19.9269	1	1	0	1	1	0	0	17.2001	17.2001	48.0079	2	PROCESSED	57536.8971875	2016-05-28 21:31:57	54735	2008-09-26 00:00:00	54137.0936805556	2007-02-06 02:14:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010012	We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO HATTORI		JAP	1	AO1	TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801001010/	Quick Look
124	RX J1347.5-1145	206.8558	-11.8095	206.189394	-11.560383	209.147012	-0.679812	323.97878779	48.76095676	291.7151	53931.2858333333	2006-07-15 06:51:36	53933.2551388889	2006-07-17 06:07:24	801013020	79.1105	75	79.1265	79.1105	79.1265	79.1345	2	2	2	2	1	0	0	69.567	69.567	170.1098	2	PROCESSED	57534.9865393518	2016-05-26 23:40:37	54394	2007-10-21 00:00:00	53942.463587963	2006-07-26 11:07:34	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010014	We propose to obtain broad-band spectra of the most X-ray luminous cluster of galaxies RXJ1347.5-1145 at z=0.45. Our previous high-resolution Sunyaev-Zel'dovich obvervations of this cluster revealed that it exhibits an unusually violent merger activity. Its high X-ray luminosity ensures the unprecedented high-quality spectra with Suzaku. It is indeed a unique target to probe gas physics and particle acceleration mechanism associated with the violent mergers at high redshift. The continuum observations with HXD and XIS as well as the iron line spectroscopy will specify the physical states of both thermal and non-thermal components of the ICM. Combined with the Chandra and our SZ data, the Suzaku data will accomplish the first comprehensive modeling of a violent merger in distant clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	NAOMI OTA		JAP	1	AO1	BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801013020/	Quick Look
125	OPHIUCHUS CLUSTER 0	258.0174	-23.3865	257.259196	-23.326891	259.005066	-0.401441	0.50702706	9.33401192	88.8366	54183.0313078704	2007-03-24 00:45:05	54183.5648726852	2007-03-24 13:33:25	801021010	16.6411	15	16.6411	16.6411	0	16.6411	2	2	0	2	1	0	0	13.5209	13.5209	46.0959	0	PROCESSED	57537.9746643518	2016-05-29 23:23:31	54736	2008-09-27 00:00:00	54209.5175462963	2007-04-19 12:25:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010065	The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUTAKA FUJITA		JAP	1	AO1	PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801021010/	Quick Look
126	OPHIUCHUS CLUSTER 8	258.0175	-23.6665	257.257716	-23.606887	259.028283	-0.680466	0.2749393	9.17298979	88.8988	54182.4897337963	2007-03-23 11:45:13	54183.0308333333	2007-03-24 00:44:24	801029010	23.7389	15	23.7469	23.7389	0	23.7469	2	2	0	2	1	0	0	21.678	21.678	46.746	0	PROCESSED	57537.9753240741	2016-05-29 23:24:28	54736	2008-09-27 00:00:00	54209.5725231482	2007-04-19 13:44:26	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010065	The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUTAKA FUJITA		JAP	1	AO1	PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801029010/	Quick Look
127	M87 50' SE	188.2678	11.8367	187.635305	12.112401	182.806232	14.132107	286.30035277	74.11241529	119.899	54071.127650463	2006-12-02 03:03:49	54072.312037037	2006-12-03 07:29:20	801039010	53.6374	50	53.6374	53.6581	0	53.6454	2	2	0	2	1	0	0	46.1394	46.1394	102.309	1	PROCESSED	57536.2354861111	2016-05-28 05:39:06	54735	2008-09-26 00:00:00	54088.5776736111	2006-12-19 13:51:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010084	The black hole at the center of M87 is one of the most heaviest in the universe. Recently TeV-gamma ray emission from M87 was found. M87 is thus a very strong candidate for an accelerator of ultra-high energy cosmic rays. We aim at the detection of non-thermal hard X-rays from M87 to clarify the mechanism of the particle acceleration. The giant elliptical galaxy M87 is at the center of the Virgo cluster of galaxies, which is the nearest cluster. We can investigate the distribution of various metal elements. We will clarify how the metals, especially oxygen, diffuse to the intracluster space from the galaxy M87.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	HIRONORI MATSUMOTO		JAP	1	AO1	NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801039010/	Quick Look
128	PERSEUS CL OFFSET	49.2788	41.3719	48.454118	41.188803	58.04223	22.344257	150.2212005	-13.65398882	65.9966	53980.7676273148	2006-09-02 18:25:23	53981.4543287037	2006-09-03 10:54:14	801049020	32.4646	30	32.4806	32.4646	32.4966	32.4886	1	1	1	1	1	0	0	28.2912	28.2912	59.3199	1	PROCESSED	57535.422025463	2016-05-27 10:07:43	54526	2008-03-01 00:00:00	54021.2712731482	2006-10-13 06:30:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010097	We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	1	AO1	MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049020/	Quick Look
129	ABELL 2199 OFFSET 4	247.0296	39.3161	246.598828	39.425672	233.044127	59.841273	62.60481799	43.78660639	250.4756	54012.6800462963	2006-10-04 16:19:16	54013.3044444444	2006-10-05 07:18:24	801060010	24.4546	25	24.4706	24.4626	24.4546	24.4775	2	2	2	2	1	0	0	25.811	25.811	53.9399	0	PROCESSED	57535.7612615741	2016-05-27 18:16:13	54735	2008-09-26 00:00:00	54024.6738888889	2006-10-16 16:10:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010138	Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	1	AO1	PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801060010/	Quick Look
130	Z8276	266.0474	32.9693	265.586798	32.989586	263.998981	56.326696	57.88393681	27.65216461	308.1365	53961.1406134259	2006-08-14 03:22:29	53961.4723958333	2006-08-14 11:20:15	801079010	14.9374	14	14.9374	14.9374	14.9374	14.9374	1	1	1	1	1	0	0	15.462	15.462	28.658	0	PROCESSED	57535.267962963	2016-05-27 06:25:52	54391	2007-10-18 00:00:00	54018.6023842593	2006-10-10 14:27:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801079010/	Quick Look
131	A3667_CENTER	303.141	-56.7974	302.14092	-56.947599	291.656641	-35.82366	340.90266514	-33.39955413	74.263	53861.7363078704	2006-05-06 17:40:17	53862.3843055556	2006-05-07 09:13:24	801096010	20.8805	20	20.8885	20.8885	20.8965	20.8805	1	1	1	1	1	0	0	8.425	8.425	55.9439	1	PROCESSED	57533.6497337963	2016-05-25 15:35:37	54394	2007-10-21 00:00:00	53913.7840509259	2006-06-27 18:49:02	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	013080	We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA	CRAIG SARAZIN	JUS	1	AO1	SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801096010/	Quick Look
132	SGR1806-20	272.1595	-20.349	271.415501	-20.357687	272.017973	3.076639	10.0481975	-0.20823053	88.7483	54189.6305555556	2007-03-30 15:08:00	54190.0627199074	2007-03-31 01:30:19	401021010	19.2889	20	19.2889	19.595	0	19.3563	1	1	0	1	1	0	0	16.5071	16.5071	37.3279	1	PROCESSED	57538.0253587963	2016-05-30 00:36:31	54561	2008-04-05 00:00:00	54209.5169212963	2007-04-19 12:24:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010124	We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs.	GALACTIC POINT SOURCES	4	A	YUJIN NAKAGAWA		JAP	1	AO1-TOO	PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR"	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401021010/	Quick Look
133	T CRB	239.8773	25.9106	239.353591	26.051383	230.095833	45.264151	42.36027985	48.16117824	268.9321	53984.9474652778	2006-09-06 22:44:21	53986.0911921296	2006-09-08 02:11:19	401043010	46.3033	50	46.3113	46.3113	46.3193	46.3033	2	2	2	2	1	0	0	45.4314	45.4314	98.8159	1	PROCESSED	57535.5107175926	2016-05-27 12:15:26	54526	2008-03-01 00:00:00	54053.4340856482	2006-11-14 10:25:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011106	Hard X-ray emission up to ~100 keV has recently been detected with INTEGRAL and Swift from 3 exceptional symbiotic stars. These 3 objects are members of a subclass of symbiotics characterized by rapid optical flickering, and in some cases jets, recurrent nova eruptions, and high-mass white dwarfs possibly headed toward supernova Type Ia explosion. The origin of the hard X-ray emission from these accreting white dwarfs is a mystery. Broad-band X-ray observations, which only Suzaku can provide, are needed to bridge the gap between existing soft and hard X-ray spectra. We propose to perform such Suzaku observations of RT Cru, T CrB, and RS Oph to distinguish among thermal emission from a magnetic accretion column, non-thermal emission from a jet, or some unforeseen emission mechanism.	GALACTIC POINT SOURCES	4	A	JENNIFER SOKOLOSKI		USA	1	AO1	THE NATURE OF HARD X-RAY SYMBIOTIC BINARIES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401043010/	Quick Look
134	GC_SGR_B_NORTH	266.6958	-28.383	265.90497	-28.365031	267.072823	-4.975469	0.60519276	0.06967717	271.4415	53999.7284837963	2006-09-21 17:29:01	54001.2863425926	2006-09-23 06:52:20	501040010	61.3753	62	61.3913	61.3753	61.3833	61.3913	2	2	2	2	1	0	0	53.867	53.867	134.5818	2	PROCESSED	57535.7042361111	2016-05-27 16:54:06	54735	2008-09-26 00:00:00	54021.2828472222	2006-10-13 06:47:18	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010060	We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR.	GALACTIC DIFFUSE EMISSION	5	B	KATSUJI KOYAMA		JAP	1	AO1	OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501040010/	Quick Look
135	IGRJ16465-4507	251.6303	-45.1738	250.724808	-45.083948	256.064043	-22.616175	340.00343338	0.10772124	284.9562	53987.3839814815	2006-09-09 09:12:56	53987.9203009259	2006-09-09 22:05:14	401052010	22.5279	20	22.5359	22.5279	22.5359	22.5359	2	2	2	2	1	0	0	24.6454	24.6454	46.332	0	PROCESSED	57535.4975925926	2016-05-27 11:56:32	54526	2008-03-01 00:00:00	54021.113287037	2006-10-13 02:43:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011132	INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	1	AO1	HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401052010/	Quick Look
136	FORNAX A WEST LOBE	50.4184	-37.1645	49.940428	-37.342839	32.47574	-52.998531	240.1258488	-56.89722719	219.7525	54092.8700462963	2006-12-23 20:52:52	54095.6113888889	2006-12-26 14:40:24	801014010	93.3093	100	93.3093	93.3093	0	93.3093	2	2	0	2	1	0	0	96.3716	96.3716	236.8358	5	PROCESSED	57536.4597569444	2016-05-28 11:02:03	54735	2008-09-26 00:00:00	54111.6821875	2007-01-11 16:22:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010029	We propose Suzaku observations of the Fornax A west radio lobe and the host galaxy. By measuring the inverse-Compton X-ray spectrum from the radio lobe precisely up to 20 keV and comparing with radio observation results, we are able to determine the electron energy spectrum and to derive magnetic field without any assumptions. This will be an important sample to measure the kinetic energy outflow from an active galactic nucleus.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO TASHIRO		JAP	1	AO1	RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801014010/	Quick Look
137	IGR J17497-2821	267.404	-28.4152	266.612848	-28.400666	267.698677	-4.994865	0.89934627	-0.48041902	271.4056	54003.2926967593	2006-09-25 07:01:29	54004.593275463	2006-09-26 14:14:19	901003010	53.3178	60	53.3338	53.3338	53.3338	53.3178	3	2	3	3	1	0	0	47.9476	47.9476	112.3599	1	PROCESSED	57535.7125925926	2016-05-27 17:06:08	54004	2006-09-26 00:00:00	54026.5016898148	2006-10-18 12:02:26	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	017003	N/A	GALACTIC COMPACT OBJECT	9	A	SWG		JAP	1	TOO	OBSERVATION OF IGR J17497-2821	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/901003010/	Quick Look
138	OPHIUCHUS CLUSTER 1	258.2981	-23.3868	257.539766	-23.328523	259.261866	-0.380707	0.65649186	9.12279372	88.7031	54180.6159953704	2007-03-21 14:47:02	54181.1398611111	2007-03-22 03:21:24	801022010	24.067	15	24.075	24.067	0	24.075	2	2	0	2	1	0	0	21.8213	21.8213	45.254	1	PROCESSED	57537.7417476852	2016-05-29 17:48:07	54736	2008-09-27 00:00:00	54186.192650463	2007-03-27 04:37:25	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010065	The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUTAKA FUJITA		JAP	1	AO1	PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801022010/	Quick Look
139	AWM7	43.631	41.5933	42.82175	41.390486	53.723626	23.815753	146.34082925	-15.61629549	90.4997	53954.2348842593	2006-08-07 05:38:14	53954.71625	2006-08-07 17:11:24	801035010	18.9858	20	18.9858	18.9858	18.9858	18.9858	2	2	2	2	1	0	0	17.5542	17.5542	41.588	0	PROCESSED	57535.2434953704	2016-05-27 05:50:38	54422	2007-11-18 00:00:00	54020.7471759259	2006-10-12 17:55:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010076	The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKAYA OHASHI		JAP	1	AO1	SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801035010/	Quick Look
140	NGC 4631	190.5387	32.5478	189.929771	32.821718	174.99352	33.703009	142.74124336	84.2191655	139.0678	54067.1412615741	2006-11-28 03:23:25	54068.9133217593	2006-11-29 21:55:11	801019010	81.0761	80	81.0841	81.0761	0	81.0841	2	2	0	2	1	0	0	74.4358	74.4358	153.07	0	PROCESSED	57536.2568865741	2016-05-28 06:09:55	54735	2008-09-26 00:00:00	54088.6914699074	2006-12-19 16:35:43	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010062	We propose to observe a edge-on nearby starburst galaxy, NGC 4631 for an exposure time of 80 ksec. This observation will give us a ``template'' of ejecta from type II SNe with less than 30% accuracy of abandance of alpha elemements.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORIKO YAMASAKI		JAP	1	AO1	OBSERVATION OF A STARBURST GALAXY NGC 4631 WITH XIS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801019010/	Quick Look
141	MARKARIAN 509	311.0428	-10.7274	310.361715	-10.908973	310.545221	7.124071	35.9681072	-29.85888698	254.2043	54054.375150463	2006-11-15 09:00:13	54055.0113541667	2006-11-16 00:16:21	701093030	24.4466	25	24.4466	24.4466	0	24.4466	2	2	0	2	1	0	0	18.327	18.327	54.9679	1	PROCESSED	57536.1015162037	2016-05-28 02:26:11	54456	2007-12-22 00:00:00	54088.6171875	2006-12-19 14:48:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012050	We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV).	EXTRAGALACTIC COMPACT SOURCES	7	A	GABRIELE PONTI		EUR	1	AO1	SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093030/	Quick Look
142	RXJ1713-3946	257.7765	-39.428	256.912609	-39.366986	260.174712	-16.402181	347.32530765	0.10490445	268.0003	53990.7111689815	2006-09-12 17:04:05	53991.0488888889	2006-09-13 01:10:24	501067010	21.1796	20	21.1876	21.1796	21.1931	21.1956	1	1	1	1	1	0	0	21.9861	21.9861	29.1679	0	PROCESSED	57535.5530902778	2016-05-27 13:16:27	54526	2008-03-01 00:00:00	54020.8250925926	2006-10-12 19:48:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501067010/	Quick Look
143	JUPITER	226.6157	-16.1957	225.916913	-16.003222	228.709072	1.245307	344.00356707	35.68981432	118.4907	53792.7940856482	2006-02-26 19:03:29	53793.8599421296	2006-02-27 20:38:19	401001030	40.7912	36	40.7992	40.7912	40.7992	40.7992	2	2	2	2	1	0	0	35.5363	35.5363	92.0739	0	PROCESSED	57533.1063078704	2016-05-25 02:33:05	54401	2007-10-28 00:00:00	53905.5868055556	2006-06-19 14:05:00	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011003	We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure.	GALACTIC POINT SOURCES	4	C	RONALD ELSNER		USA	1	AO1	JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001030/	Quick Look
144	BETA LYR	282.5094	33.3738	282.047614	33.314587	288.857821	55.998718	63.19462876	14.79594569	59.4704	53862.545474537	2006-05-07 13:05:29	53862.9952083333	2006-05-07 23:53:06	401036010	20.2515	20	20.2675	20.2515	20.2675	20.2675	2	2	2	2	1	0	0	9.8947	9.8947	38.8519	1	PROCESSED	57533.7394212963	2016-05-25 17:44:46	54401	2007-10-28 00:00:00	53913.8191550926	2006-06-27 19:39:35	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011031	The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse.	GALACTIC POINT SOURCES	4	A	RICHARD IGNACE		USA	1	AO1	AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036010/	Quick Look
145	BETA LYR	282.5093	33.3719	282.047501	33.312687	288.85715	55.996853	63.19278609	14.79528012	53.4973	53871.4311226852	2006-05-16 10:20:49	53871.8571875	2006-05-16 20:34:21	401036030	18.1954	20	18.1954	18.1954	18.1954	18.1954	2	2	2	2	1	0	0	19.8421	19.8421	36.8079	0	PROCESSED	57534.3160532407	2016-05-26 07:35:07	54401	2007-10-28 00:00:00	53920.4164351852	2006-07-04 09:59:40	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011031	The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse.	GALACTIC POINT SOURCES	4	A	RICHARD IGNACE		USA	1	AO1	AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036030/	Quick Look
146	SKY_50.0_-62.4	50.0507	-62.4328	49.819854	-62.612067	354.772614	-72.643934	278.67600391	-47.08169247	281.591	53795.7055671296	2006-03-01 16:56:01	53796.9369675926	2006-03-02 22:29:14	501001010	80.145	80	80.153	80.145	80.153	80.145	2	2	2	2	1	0	0	74.0122	74.0122	106.376	0	PROCESSED	57533.1282638889	2016-05-25 03:04:42	54401	2007-10-28 00:00:00	53905.6164930556	2006-06-19 14:47:45	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011252	We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble.	GALACTIC DIFFUSE EMISSION	5	A	ROBIN SHELTON		USA	1	AO1	SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501001010/	Quick Look
147	4U 1636-536	250.2272	-53.754	249.230789	-53.657507	256.461332	-31.236669	332.91133194	-4.81789372	91.2454	54160.0424421296	2007-03-01 01:01:07	54160.8931597222	2007-03-01 21:26:09	401050030	38.7193	38	38.7274	38.7193	0	38.7194	2	1	0	2	1	0	0	48.1459	48.1459	73.498	1	PROCESSED	57537.5161111111	2016-05-29 12:23:12	54695	2008-08-17 00:00:00	54167.6400462963	2007-03-08 15:21:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011117	Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.	GALACTIC POINT SOURCES	4	A	JEROEN HOMAN		USA	1	AO1	THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050030/	Quick Look
148	GC SOUTH	266.5016	-29.1694	265.705845	-29.150477	266.920624	-5.765664	359.84485124	-0.1935349	265.0006	54004.5960185185	2006-09-26 14:18:16	54007.8925231482	2006-09-29 21:25:14	501008010	129.5773	130	129.5773	129.5773	129.5773	129.5773	2	2	2	2	1	0	0	111.2591	111.2591	284.8038	5	PROCESSED	57535.7712731482	2016-05-27 18:30:38	54744	2008-10-05 00:00:00	54021.0929050926	2006-10-13 02:13:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010044	Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	1	AO1	SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501008010/	Quick Look
149	HESS J1745-303	266.2629	-30.3722	265.459457	-30.352101	266.742769	-6.973282	358.71029443	-0.64354718	263.6011	54015.0950462963	2006-10-07 02:16:52	54016.4300810185	2006-10-08 10:19:19	501010010	50.6707	50	50.6707	50.6707	50.6707	50.6707	1	1	1	1	1	0	0	45.6897	45.6897	115.3119	1	PROCESSED	57535.8009837963	2016-05-27 19:13:25	54526	2008-03-01 00:00:00	54021.698587963	2006-10-13 16:45:58	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010046	So far, the evidence for hadron acceleration up to near the knee energy has not yet obtained. Recent galactic plane survey in the TeV gamma-ray band reveals several new unidentified sources like HESS J1745-303. It is extended, hence likely a supernova remnant. Also it coincides with an EGRET unidentified source (3EG J1744-3011), which may suggest that it is a source of accelerated protons. However, HESS J1745-303 shows rather hard spectrum that cannot be explained by the simplest version of the diffusive shock acceleration model. X-ray study on HESS J1745-303 is necessary for further discussions. We might find that observed data requires modification of the common picture that young supernova remnants are the dominant source of high-energy protons.	GALACTIC DIFFUSE EMISSION	5	A	RYO YAMAZAKI		JAP	1	AO1	X-RAY STUDY ON THE TEV UNIDENTIFIED SOURCE HESS J1745-303	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501010010/	Quick Look
150	SWIFTJ2000.6+3210	300.1137	32.1218	299.624092	31.983158	312.678705	51.196511	68.93835501	1.08211502	255.6072	54039.0205671296	2006-10-31 00:29:37	54039.3029976852	2006-10-31 07:16:19	401053020	12.7484	10	12.7564	12.7484	12.7564	12.7564	2	2	2	2	1	0	0	11.727	11.727	24.3939	0	PROCESSED	57535.9859490741	2016-05-27 23:39:46	54775	2008-11-05 00:00:00	54056.1959953704	2006-11-17 04:42:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011132	INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	1	AO1	HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401053020/	Quick Look
151	IGR J16318-4848	247.9691	-48.8061	247.034981	-48.699533	253.953463	-26.583352	335.63186461	-0.44896472	266.5948	53961.4825	2006-08-14 11:34:48	53964.3488310185	2006-08-17 08:22:19	401094010	97.2538	100	97.2698	97.2538	97.2698	97.2698	2	2	2	2	1	0	0	87.1128	87.1128	247.6059	5	PROCESSED	57535.3483564815	2016-05-27 08:21:38	54526	2008-03-01 00:00:00	54020.9181597222	2006-10-12 22:02:09	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012034	We propose a detailed study of Compton thick X-ray absorption in neutral or weakly ionized material by using 100ksec of Suzaku observations of the strongly absorbed (N_H~2E24cm2) Galactic X-ray binary IGR J16318-4848. Measuring a high signal to noise ratio broad band spectrum will allow us to determine the curvature in the >10keV continuum caused by Compton downscattering in the absorber, to deduce its ionization state from observations of the Fe Kalpha line, and to study the variability of the source and the absorber. These observations will also shed more light onto the nature of the compact object in IGR J16318-4848.	GALACTIC POINT SOURCES	4	B	JOERN WILMS		EUR	1	AO1	OBSERVING IGR J16318-4848: PROBING COMPTON-THICK ABSORPTION	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401094010/	Quick Look
152	CYGNUS_LOOP_P7	312.0838	30.7678	311.566097	30.58216	326.462182	46.307536	73.70103145	-8.0534172	239.9966	54416.1673032407	2007-11-12 04:00:55	54416.7223263889	2007-11-12 17:20:09	501018010	24.1545	22	24.1545	24.1545	0	24.1545	2	2	0	2	1	0	0	18.861	18.861	47.92	0	PROCESSED	57540.4878587963	2016-06-01 11:42:31	54798	2008-11-28 00:00:00	54430.1343287037	2007-11-26 03:13:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501018010/	Quick Look
153	HESS J1825-137	276.5031	-13.6997	275.794781	-13.729527	276.397624	9.596588	17.87105596	-0.70261201	269.3213	54025.8175462963	2006-10-17 19:37:16	54027.1682291667	2006-10-19 04:02:15	501044010	50.293	50	50.293	50.293	50.293	50.293	2	2	2	2	1	0	0	42.9557	42.9557	116.694	1	PROCESSED	57535.8789351852	2016-05-27 21:05:40	54526	2008-03-01 00:00:00	54055.4418634259	2006-11-16 10:36:17	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010073	We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	1	AO1	SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501044010/	Quick Look
154	RXJ1713-3946	257.7744	-39.7271	256.908127	-39.666071	260.20044	-16.700257	347.08325974	-0.07081205	268.0001	53990.3113310185	2006-09-12 07:28:19	53990.7106944444	2006-09-12 17:03:24	501066010	20.9207	20	20.9407	20.9207	20.926	20.9447	2	2	2	2	1	0	0	20.699	20.699	34.504	1	PROCESSED	57535.5600347222	2016-05-27 13:26:27	54526	2008-03-01 00:00:00	54020.8077546296	2006-10-12 19:23:10	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501066010/	Quick Look
155	GALACTIC CENTER	265.5037	-30.2156	264.701457	-30.191826	266.078204	-6.8356	358.49956421	-0.00336241	269.0005	54018.2813541667	2006-10-10 06:45:09	54018.887662037	2006-10-10 21:18:14	501052010	19.2451	20	19.2611	19.2611	19.2531	19.2451	2	2	2	2	1	0	0	16.0462	16.0462	52.3799	1	PROCESSED	57535.818275463	2016-05-27 19:38:19	54735	2008-09-26 00:00:00	54053.5074537037	2006-11-14 12:10:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501052010/	Quick Look
156	SNR G93.3+6.9 S2	312.6887	55.4958	312.345372	55.307685	351.959804	67.182569	93.24230604	7.18061007	40.0056	53905.9701736111	2006-06-19 23:17:03	53906.4293865741	2006-06-20 10:18:19	501081010	16.0092	15	16.0352	16.0272	16.0092	16.0352	2	2	2	2	1	0	0	18.3757	18.3757	39.6679	1	PROCESSED	57534.7256134259	2016-05-26 17:24:53	54401	2007-10-28 00:00:00	53927.314537037	2006-07-11 07:32:56	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501081010/	Quick Look
157	SWIFT J0601.9-8636	91.1523	-86.6779	95.292028	-86.662252	269.78546	-69.879444	299.2555588	-27.75439578	292.1727	53838.6834259259	2006-04-13 16:24:08	53839.0779976852	2006-04-14 01:52:19	701018010	19.7657	20	19.7817	19.7817	19.7657	19.7737	2	2	2	2	1	0	0	16.6614	16.6614	34.0599	0	PROCESSED	57533.4511226852	2016-05-25 10:49:37	54397	2007-10-24 00:00:00	53905.4682060185	2006-06-19 11:14:13	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010133	Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background".	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	1	AO1	DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701018010/	Quick Look
158	PUP A : SE	126.0128	-43.1802	125.58355	-43.01733	147.904142	-59.590498	260.74447692	-3.25911558	277.1832	53843.3098842593	2006-04-18 07:26:14	53843.8328009259	2006-04-18 19:59:14	501089010	29.7493	30	29.7493	29.8172	29.7652	29.7612	4	2	4	4	1	0	0	22.8867	22.8867	45.174	0	PROCESSED	57533.5119675926	2016-05-25 12:17:14	54401	2007-10-28 00:00:00	53907.001412037	2006-06-21 00:02:02	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501089010/	Quick Look
159	NGC 5506	213.3121	-3.2119	212.6632	-2.97838	212.190756	9.596557	339.14659218	53.80640928	287.3747	53958.1015972222	2006-08-11 02:26:18	53959.4488425926	2006-08-12 10:46:20	701030020	53.2962	63	53.3042	53.2962	53.3042	53.3042	2	2	2	2	1	0	0	47.9832	47.9832	116.386	1	PROCESSED	57535.2817476852	2016-05-27 06:45:43	54695	2008-08-17 00:00:00	54116.3307291667	2007-01-16 07:56:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011312	NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	A	TRACEY TURNER		USA	1	AO1	SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030020/	Quick Look
160	MBM12 OFF-CLOUD	41.3205	18.3346	40.61976	18.124407	44.482795	2.251416	157.33933963	-36.81758445	247.4802	53772.648599537	2006-02-06 15:33:59	53774.618275463	2006-02-08 14:50:19	501104010	75.3292	70	75.3372	75.3292	75.3372	75.3372	2	2	2	2	1	0	0	67.769	67.769	170.1159	1	PROCESSED	57532.9691550926	2016-05-24 23:15:35	54401	2007-10-28 00:00:00	53905.9757523148	2006-06-19 23:25:05	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011262	Suzaku will observe MBM 12, a nearby molecular cloud which shadows all but the most local soft X-ray emission. The goal of that observation is to measure the O VII and O VIII emission from the Local Hot Bubble, taking advantage of Suzaku's low energy sensitivity and low background. In light of this, we propose to observe the diffuse background near the MBM 12 position. This will: (1) Measure the O VII and O VIII emission from the Galactic disk and halo, after subtracting the local emission, and (2) confirm that this background emission does not contaminate the initial observation. The absolute measure of the strength of the O VII line, as well as the O VIII/O VII ratio, is essential to understanding the origin of the Galactic component to the 3/4 keV diffuse emission.	GALACTIC DIFFUSE EMISSION	5	B	RANDALL SMITH		USA	1	AO1	THE ORIGIN OF THE GALACTIC DIFFUSE 3/4 KEV X-RAY BACKGROUND	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501104010/	Quick Look
161	MRK 766	184.6147	29.8197	183.986078	30.097268	171.204802	28.944359	190.62410896	82.27145087	134.9989	54421.893287037	2007-11-17 21:26:20	54423.2363310185	2007-11-19 05:40:19	701035020	59.3635	50	59.3635	59.3635	0	59.3635	1	1	0	1	1	0	0	51.1517	51.1517	116.0238	1	PROCESSED	57540.5762384259	2016-06-01 13:49:47	54800	2008-11-30 00:00:00	54433.2716666667	2007-11-29 06:31:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011328	X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components	EXTRAGALACTIC COMPACT SOURCES	7	B	TRACEY TURNER		USA	1	AO1	DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701035020/	Quick Look
162	E0102.2-7219	16.0175	-72.0405	15.612819	-72.30846	314.602108	-65.044333	301.55408267	-45.05394165	60.6353	53912.8662731482	2006-06-26 20:47:26	53913.4245833333	2006-06-27 10:11:24	101005030	21.6758	20	21.7158	21.6838	21.7158	21.6758	2	4	2	4	1	0	0	35.0626	35.0626	48.2039	0	PROCESSED	57534.7584837963	2016-05-26 18:12:13	53826	2006-04-01 00:00:00	53928.4586458333	2006-07-12 11:00:27	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	AO1	XIS FLIGHT CALIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005030/	Quick Look
163	RBS 315	36.2519	18.8398	35.555924	18.614311	40.065414	4.223463	151.73247281	-38.74296898	76.7825	53941.8167013889	2006-07-25 19:36:03	53943.0404976852	2006-07-27 00:58:19	701077010	47.8309	50	47.8309	47.8309	47.8309	47.8309	2	2	2	2	1	0	0	43.425	43.425	105.7299	1	PROCESSED	57535.0495023148	2016-05-27 01:11:17	54400	2007-10-27 00:00:00	53955.7322106482	2006-08-08 17:34:23	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012008	We propose to observe with Suzaku the X-ray bright blazar RBS 315, showing a very hard spectrum (Gamma<1.2) in the 2-10 keV range as determined by XMM. The requested observation will allow us to measure the continuum in the full Suzaku range (0.3-200 keV), fully exploiting the unique capabilities of the satellite. With its wide energy coverage and good response at soft energies, Suzaku will allow to determine with precision the spectral properties of the source in the hard medium and soft X-ray ranges, providing important clues on the physics and the environment of relativistic jets. A good measurement of the continuum will allow us to determine the luminosity emitted via the IC mechanism which usually dominates the radiative output and the total kinetic power carried by the outflow.	EXTRAGALACTIC COMPACT SOURCES	7	B	FABRIZIO TAVECCHIO		EUR	1	AO1	SUZAKU OBSERVATION OF THE HARD BROAD BAND CONTINUUM OF THE POWERFUL BLAZAR RBS 315	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701077010/	Quick Look
164	GALACTIC CENTER	266.0341	-30.1068	265.232432	-30.085596	266.53657	-6.713302	358.83318764	-0.33628911	269.0002	54019.4218402778	2006-10-11 10:07:27	54020.1446064815	2006-10-12 03:28:14	501057010	20.4884	20	20.4884	20.4964	20.4964	20.4964	2	2	2	2	1	0	0	19.086	19.086	62.4379	0	PROCESSED	57535.8262037037	2016-05-27 19:49:44	54735	2008-09-26 00:00:00	54053.6059837963	2006-11-14 14:32:37	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501057010/	Quick Look
165	THE CRAB OFFSETS	83.6229	22.105	82.870128	22.072264	84.093748	-1.205217	184.47554642	-5.74387633	85.7146	53983.889212963	2006-09-05 21:20:28	53983.9516087963	2006-09-05 22:50:19	101011020	3.35	2	3.35	3.35	3.35	3.35	1	1	1	1	1	0	0	3.004	3.004	5.3839	0	PROCESSED	57535.4600694444	2016-05-27 11:02:30	53826	2006-04-01 00:00:00	54104.4374189815	2007-01-04 10:29:53	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011020/	Quick Look
166	SKY_53.3_-63.4	53.24	-63.4549	53.047022	-63.62196	354.144887	-74.40934	278.62179386	-45.30780651	286.1724	53797.8694444444	2006-03-03 20:52:00	53800.3342476852	2006-03-06 08:01:19	501002010	101.4752	100	101.4752	101.4752	101.4752	101.4752	2	2	2	2	1	0	0	145.4318	145.4318	212.8539	4	PROCESSED	57533.1863425926	2016-05-25 04:28:20	54401	2007-10-28 00:00:00	53906.7729282407	2006-06-20 18:33:01	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011252	We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble.	GALACTIC DIFFUSE EMISSION	5	A	ROBIN SHELTON		USA	1	AO1	SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501002010/	Quick Look
167	GC SOUTH BGD	266.1893	-28.9082	265.395265	-28.887768	266.639666	-5.511508	359.92534776	0.17564926	265.0003	54007.8931365741	2006-09-29 21:26:07	54009.2884143518	2006-10-01 06:55:19	501009010	51.19	50	51.198	51.206	51.19	51.198	2	2	2	2	1	0	0	47.7157	47.7157	120.5479	0	PROCESSED	57535.7087847222	2016-05-27 17:00:39	54735	2008-09-26 00:00:00	54020.9371064815	2006-10-12 22:29:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010044	Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	1	AO1	SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501009010/	Quick Look
168	G344.7-0.1	255.9588	-41.7032	255.078113	-41.633558	258.959028	-18.797881	344.67682908	-0.15577285	89.2821	54152.1890393518	2007-02-21 04:32:13	54153.2919097222	2007-02-22 07:00:21	501011010	42.1336	40	42.1336	42.1336	0	42.1336	2	2	0	2	1	0	0	34.2016	34.2016	95.28	1	PROCESSED	57537.4329050926	2016-05-29 10:23:23	54777	2008-11-07 00:00:00	54158.2352662037	2007-02-27 05:38:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010050	We propose an observation of a supernova remnant (SNR) G344.7-0.1 with Suzaku. In addition to emission lines from highly ionized ions (Si, S, and so on), we found a strong emission line at 6.4 keV in the spectra obtained with ASCA and XMM-Newton. This line is thought to be a K-line from the low-ionized Fe, but the origin is still unknown. Precise measurements of the line energy and the spectral parameters with the XIS will provide us with understanding the origin of the Fe-K line and the physical process in the SNR.	GALACTIC DIFFUSE EMISSION	5	C	SHIGEO YAMAUCHI		JAP	1	AO1	SUZAKU OBSERVATION OF G344.7-0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501011010/	Quick Look
169	CYGNUS_LOOP_P13	313.4901	31.0708	312.971102	30.880128	328.238327	46.115492	74.70349314	-8.80441033	68.2467	53865.1416666667	2006-05-10 03:24:00	53865.5321643518	2006-05-10 12:46:19	501030010	17.073	17	17.073	17.081	17.089	17.089	1	1	1	1	1	0	0	14.269	14.269	33.7279	0	PROCESSED	57534.2605092593	2016-05-26 06:15:08	54394	2007-10-21 00:00:00	53914.0847569444	2006-06-28 02:02:03	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501030010/	Quick Look
170	G156.2+5.7E	75.8128	51.6405	74.832405	51.569986	80.017374	28.69124	156.70319129	6.10796494	274.6638	54149.9177893518	2007-02-18 22:01:37	54151.1750231482	2007-02-20 04:12:02	501074010	53.3331	50	53.3494	53.3491	0	53.3331	2	2	0	2	1	0	0	50.8218	50.8218	108.6199	2	PROCESSED	57537.4302893518	2016-05-29 10:19:37	54773	2008-11-03 00:00:00	54158.2839583333	2007-02-27 06:48:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011235	G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target.	GALACTIC DIFFUSE EMISSION	5	C	ROBERT PETRE		USA	1	AO1	A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501074010/	Quick Look
171	SNR G93.3+6.9 S3	313.171	55.2801	312.823004	55.090273	352.082126	66.837166	93.24775568	6.83197363	40.0152	53906.4300462963	2006-06-20 10:19:16	53906.7266087963	2006-06-20 17:26:19	501082010	16.3347	15	16.3347	16.3587	16.3507	16.3427	1	1	1	1	1	0	0	13.9186	13.9186	25.6159	0	PROCESSED	57534.7339814815	2016-05-26 17:36:56	54401	2007-10-28 00:00:00	53926.2481365741	2006-07-10 05:57:19	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501082010/	Quick Look
172	PUP A : NE	125.7583	-42.7117	125.326284	-42.549841	147.156331	-59.259606	260.25284038	-3.14403225	277.1213	53842.913287037	2006-04-17 21:55:08	53843.3091319445	2006-04-18 07:25:09	501087010	20.7109	20	20.7336	20.7349	20.7189	20.7109	1	1	1	1	1	0	0	19.7443	19.7443	34.1899	1	PROCESSED	57533.5127083333	2016-05-25 12:18:18	54401	2007-10-28 00:00:00	53906.9450231482	2006-06-20 22:40:50	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501087010/	Quick Look
173	N11 SB	74.1823	-66.412	74.156384	-66.487992	354.048784	-83.709745	277.1886014	-36.07081942	146.432	54046.4407291667	2006-11-07 10:34:39	54047.232037037	2006-11-08 05:34:08	501091010	30.452	30	30.452	30.452	30.452	30.452	2	2	2	2	1	0	0	26.405	26.405	68.3659	0	PROCESSED	57536.0384953704	2016-05-28 00:55:26	54455	2007-12-21 00:00:00	54088.5643287037	2006-12-19 13:32:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011251	Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 2 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 4 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission.	GALACTIC DIFFUSE EMISSION	5	C	ROSA WILLIAMS		USA	1	AO1	A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501091010/	Quick Look
174	VELA PULSAR/PWN 3	128.6368	-45.8007	128.219858	-45.627635	153.778024	-60.967724	263.96966687	-3.27226783	344.1164	53925.347974537	2006-07-09 08:21:05	53926.0467476852	2006-07-10 01:07:19	501110010	17.5886	20	17.6046	17.5886	17.5886	17.6046	1	1	1	1	1	0	0	17.2252	17.2252	60.3519	0	PROCESSED	57534.8715509259	2016-05-26 20:55:02	54401	2007-10-28 00:00:00	53930.634224537	2006-07-14 15:13:17	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014211	The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band.	GALACTIC DIFFUSE EMISSION	5	B	OLEG KARGALTSEV	KOJI MORI	USJ	1	AO1	THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501110010/	Quick Look
175	THE CRAB OFFSETS	83.6323	21.9916	82.880162	21.958911	84.097445	-1.318894	184.57650041	-5.79723168	85.7244	53984.1531944445	2006-09-06 03:40:36	53984.2224421296	2006-09-06 05:20:19	101011050	3.355	2	3.355	3.355	3.355	3.355	1	1	1	1	1	0	0	2.187	2.187	5.9759	0	PROCESSED	57535.4744907407	2016-05-27 11:23:16	53826	2006-04-01 00:00:00	54104.4478587963	2007-01-04 10:44:55	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011050/	Quick Look
176	RXJ1713-3946	258.1633	-39.7281	257.296672	-39.668915	260.511599	-16.675371	347.25895477	-0.31287235	268.0002	53989.5311574074	2006-09-11 12:44:52	53989.9216898148	2006-09-11 22:07:14	501064010	21.322	20	21.322	21.322	21.322	21.322	2	2	2	2	1	0	0	23.0306	23.0306	33.7279	0	PROCESSED	57535.5353356482	2016-05-27 12:50:53	54526	2008-03-01 00:00:00	54020.8109027778	2006-10-12 19:27:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501064010/	Quick Look
177	CYGNUS_LOOP_P2	313.2729	31.7708	312.75774	31.580892	328.394465	46.831624	75.13379207	-8.21853117	240.0005	54418.0909722222	2007-11-14 02:11:00	54418.4168865741	2007-11-14 10:00:19	501013010	16.3799	10	16.3879	16.3879	0	16.3799	1	1	0	1	1	0	0	10.9786	10.9786	28.1519	0	PROCESSED	57540.5114351852	2016-06-01 12:16:28	54798	2008-11-28 00:00:00	54430.1915972222	2007-11-26 04:35:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501013010/	Quick Look
178	CYGNUS_LOOP_P14	313.2365	30.8681	312.717032	30.678328	327.835222	46.014729	74.40554659	-8.76356285	62.362	53867.6311111111	2006-05-12 15:08:48	53868.0050462963	2006-05-13 00:07:16	501031010	18.5809	18	18.5809	18.5809	18.5809	18.5809	2	2	2	2	1	0	0	12.7378	12.7378	32.2979	0	PROCESSED	57534.275775463	2016-05-26 06:37:07	54394	2007-10-21 00:00:00	53914.3142476852	2006-06-28 07:32:31	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501031010/	Quick Look
179	CYGNUS_LOOP_P18	312.0547	29.7111	311.531939	29.525574	325.8489	45.340722	72.84665082	-8.68804998	237.4994	54087.0528819444	2006-12-18 01:16:09	54087.3405208333	2006-12-18 08:10:21	501035010	12.011	13	12.915	12.011	0	12.907	2	2	0	2	1	0	0	11.4394	11.4394	24.8359	3	PROCESSED	57536.3543981482	2016-05-28 08:30:20	54750	2008-10-11 00:00:00	54096.4390972222	2006-12-27 10:32:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501035010/	Quick Look
180	HESS J1825-137 BG	276.9022	-13.2649	276.196149	-13.29666	276.811822	10.012623	18.4366217	-0.84356166	269.33	54027.1689351852	2006-10-19 04:03:16	54028.5072337963	2006-10-20 12:10:25	501045010	52.1444	50	52.1524	52.1444	52.1524	52.1444	2	2	2	2	1	0	0	42.1974	42.1974	115.6079	2	PROCESSED	57535.8869907407	2016-05-27 21:17:16	54526	2008-03-01 00:00:00	54055.6591550926	2006-11-16 15:49:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010073	We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137.	GALACTIC DIFFUSE EMISSION	5	B	HIRONORI MATSUMOTO		JAP	1	AO1	SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501045010/	Quick Look
181	PUP A : S	125.6829	-43.1445	125.254263	-42.982932	147.449231	-59.669734	260.57740663	-3.43620983	277.8865	53843.8334606482	2006-04-18 20:00:11	53844.4397569444	2006-04-19 10:33:15	501090010	31.1445	30	31.1605	31.1525	31.1445	31.1685	2	2	2	2	1	0	0	26.5856	26.5856	52.3719	1	PROCESSED	57533.5191550926	2016-05-25 12:27:35	54401	2007-10-28 00:00:00	53907.0902199074	2006-06-21 02:09:55	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501090010/	Quick Look
182	VELA FRAGMENT B	135.5139	-43.4767	135.058427	-43.278826	159.573758	-56.461444	265.2464603	1.98991007	89.0012	54044.6051388889	2006-11-05 14:31:24	54046.4341898148	2006-11-07 10:25:14	501085010	57.8804	60	57.8964	57.8804	57.8964	57.8964	2	2	2	2	1	0	0	56.9652	56.9652	158.0219	2	PROCESSED	57536.0751157407	2016-05-28 01:48:10	54695	2008-08-17 00:00:00	54091.4107175926	2006-12-22 09:51:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011245	Ejecta fragments from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM-Newton, show strongly enhanced but very different abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe another fragment, "B". The abundances and distribution will provide further evidence about the origin and evolution of these ejecta clumps, In combination with the existing observations of fragments A and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interaction with the remnant shell and the surrounding ISM.	GALACTIC DIFFUSE EMISSION	5	C	TERRANCE GAETZ		USA	1	AO1	SEARCHING FOR EJECTA IN VELA SNR FRAGMENT B	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501085010/	Quick Look
183	VELA PULSAR/PWN 1	128.7701	-45.1981	128.348103	-45.024538	153.316878	-60.401286	263.5414959	-2.83747227	337.9628	53926.0492592593	2006-07-10 01:10:56	53927.7841782407	2006-07-11 18:49:13	501109010	60.2913	60	60.3446	60.2913	60.3313	60.3233	2	2	2	2	1	0	0	52.6899	52.6899	149.8659	1	PROCESSED	57534.9239699074	2016-05-26 22:10:31	54401	2007-10-28 00:00:00	53942.4588078704	2006-07-26 11:00:41	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014211	The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band.	GALACTIC DIFFUSE EMISSION	5	B	OLEG KARGALTSEV	KOJI MORI	USJ	1	AO1	THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501109010/	Quick Look
184	THE CRAB OFFSETS	83.5675	22.0116	82.815266	21.978598	84.038293	-1.296249	184.5271819	-5.8372614	85.7131	53984.7573263889	2006-09-06 18:10:33	53984.8197222222	2006-09-06 19:40:24	101011140	3.369	2	3.369	3.369	3.369	3.369	1	1	1	1	1	0	0	3.632	3.632	5.3839	0	PROCESSED	57535.4802546296	2016-05-27 11:31:34	53826	2006-04-01 00:00:00	54104.4270601852	2007-01-04 10:14:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011140/	Quick Look
185	IRASF11223-1244	171.2239	-12.9662	170.593283	-12.69128	177.194404	-15.365769	272.54538498	44.73919633	107.3062	54064.7275347222	2006-11-25 17:27:39	54065.5709953704	2006-11-26 13:42:14	701008010	40.9415	40	41.1015	40.9415	0	41.1095	1	1	0	1	1	0	0	37.6804	37.6804	72.8639	1	PROCESSED	57536.1775925926	2016-05-28 04:15:44	54735	2008-09-26 00:00:00	54088.8556828704	2006-12-19 20:32:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010038	The source of huge energy output from ultraluminous infrared galaxies (ULIRGs) is still under debate. We propose to search for a hidden QSO as the energy source by observing ULIRGs with high luminosity optical emission lines classified as a Seyfert 2. The data will be used to constrain the power of the central AGN and to study the nature of infrared selected type 2 QSOs.	EXTRAGALACTIC COMPACT SOURCES	7	C	YUICHI TERASHIMA		JAP	1	AO1	A SEARCH FOR HIDDEN QSO IN ULTRALUMINOUS INFRARED GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701008010/	Quick Look
186	MRK 0359	21.8893	19.1757	21.213343	18.916781	27.368924	9.282102	134.6025573	-42.87605962	244.6178	54137.9789699074	2007-02-06 23:29:43	54140.3738078704	2007-02-09 08:58:17	701082010	107.507	100	107.507	107.507	0	107.507	2	2	0	2	1	0	0	102.5761	102.5761	206.8678	2	PROCESSED	57537.3689930556	2016-05-29 08:51:21	54735	2008-09-26 00:00:00	54151.5150925926	2007-02-20 12:21:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012023	Markarian 359 was the first source to be identified as a Narrow Line Seyfert 1 (NLS1) AGN, and its importance as an unusual source has been recognised for a long time. In the optical, it has unusually narrow lines for a NLS1. X-ray observations of the source are rare, but based on an XMM-Newton observation a strong reflection 'hump' is predicted. The source is therefore a critical one in the investigation of relativistically blurred photoionized disc reflection models. A detailed Suzaku observation will provide improved data quality in the XIS waveband, allow investigation of spectral variability in this waveband, and constrain the amount of reflection independently by using the HXD.	EXTRAGALACTIC COMPACT SOURCES	7	C	JAMIE CRUMMY		EUR	1	AO1	NVESTIGATING REFLECTION IN MARKARIAN 359	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701082010/	Quick Look
187	M31	10.6944	41.2627	10.010045	40.988882	27.852586	33.34214	121.18191229	-21.57961988	231.6592	54115.6775578704	2007-01-15 16:15:41	54117.4572222222	2007-01-17 10:58:24	801043010	99.8723	100	99.8723	99.8723	0	99.8723	2	2	0	2	1	0	0	103.9124	103.9124	153.7238	1	PROCESSED	57536.8902777778	2016-05-28 21:22:00	54744	2008-10-05 00:00:00	54132.9457291667	2007-02-01 22:41:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010089	We propose the 100 ks Suzaku observation of the central region of Andromeda Nebula (M31). Our gaol is to detect 3 components (cool, hot and hard) of galactic diffuse X-ray emission (GDXE) with the XIS and HXD. This detection shows the existance of the GDXE hot and hard component in the extragalactic normal spiral galaxy, for the first time.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	HIROMITSU TAKAHASHI		JAP	1	AO1	DETECTION OF GALACTIC DIFFUSE X-RAY EMISSION FROM THE CENTRAL REGION OF THE ANDROMEDA NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801043010/	Quick Look
188	CRAB	83.6368	22.0131	82.88454	21.980432	84.102563	-1.297599	184.56049184	-5.78219867	250.943	53829.1296643518	2006-04-04 03:06:43	53829.5974305556	2006-04-04 14:20:18	101004020	19.1389	20	19.1389	19.1458	19.1389	19.1389	1	1	1	1	1	0	0	13.2831	13.2831	40.4119	1	PROCESSED	57533.3778009259	2016-05-25 09:04:02	53826	2006-04-01 00:00:00	53906.6409375	2006-06-20 15:22:57	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015004	Crab cal at the XIS and HXD nominal positions.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101004020/	Quick Look
189	PKS 0558-504	89.9324	-50.4401	89.628897	-50.441186	89.861567	-73.881962	257.95192858	-28.57760064	211.3321	54120.8400925926	2007-01-20 20:09:44	54121.3279976852	2007-01-21 07:52:19	701011040	19.7381	20	19.7541	19.7381	0	19.7541	1	1	0	1	1	0	0	17.175	17.175	42.1359	0	PROCESSED	57536.8909953704	2016-05-28 21:23:02	54735	2008-09-26 00:00:00	54137.1036921296	2007-02-06 02:29:19	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010057	Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	C	YOSHITO HABA		JAP	1	AO1	SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011040/	Quick Look
190	SWIFT J0255.2-0011	43.8161	-0.2397	43.176621	-0.441669	41.282729	-16.217011	175.95402612	-49.91735431	256.3177	54123.6209490741	2007-01-23 14:54:10	54126.2294560185	2007-01-26 05:30:25	701013010	101.6321	100	101.6321	101.6321	0	101.6321	2	2	0	2	1	0	0	86.2824	86.2824	225.3379	3	PROCESSED	57536.9811342593	2016-05-28 23:32:50	54735	2008-09-26 00:00:00	54137.3009027778	2007-02-06 07:13:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010122	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of type-2 AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new type-2 AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. This proposal is complementary to our separate proposal entitled "direct determination of the fraction of Compton-thick AGNs in the local universe".	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	1	AO1	BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701013010/	Quick Look
191	SWIFT J0505.7-2348	76.4285	-23.9055	75.907939	-23.972083	71.84647	-46.496539	225.00444872	-33.15769393	284.9903	53826.9254166667	2006-04-01 22:12:36	53829.1216898148	2006-04-04 02:55:14	701014010	78.5544	80	78.5544	78.5544	78.5544	78.5544	2	2	2	2	1	0	0	53.4937	53.4937	189.6979	1	PROCESSED	57533.4023726852	2016-05-25 09:39:25	54439	2007-12-05 00:00:00	53945.2822569444	2006-07-29 06:46:27	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010122	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of type-2 AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new type-2 AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. This proposal is complementary to our separate proposal entitled "direct determination of the fraction of Compton-thick AGNs in the local universe".	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	1	AO1	BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701014010/	Quick Look
192	SWIFT J0138.6-4001	24.6022	-39.9757	24.058156	-40.229446	3.045259	-45.758208	268.75310615	-73.8819888	44.7851	53890.7590740741	2006-06-04 18:13:04	53891.2085532407	2006-06-05 05:00:19	701015010	21.1979	20	21.2139	21.1979	21.2139	21.2139	1	1	1	1	1	0	0	17.4771	17.4771	38.8319	1	PROCESSED	57534.4839814815	2016-05-26 11:36:56	54394	2007-10-21 00:00:00	53926.7722337963	2006-07-10 18:32:01	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010133	Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background".	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	1	AO1	DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701015010/	Quick Look
193	SWIFT J0350.1-5019	57.5863	-50.3518	57.229549	-50.501821	28.784936	-67.035424	259.75531799	-48.98660415	277.9348	54162.2927777778	2007-03-03 07:01:36	54162.5036921296	2007-03-03 12:05:19	701017030	8.1487	10	8.1567	8.1487	0	8.1567	1	1	0	1	1	0	0	7.0597	7.0597	18.2159	0	PROCESSED	57537.5866898148	2016-05-29 14:04:50	54750	2008-10-11 00:00:00	54167.6235763889	2007-03-08 14:57:57	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010133	Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background".	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	1	AO1	DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017030/	Quick Look
194	TON S180	14.333	-22.3803	13.720307	-22.650448	3.73482	-26.131336	138.98529016	-85.06726133	237.1425	54078.5680671296	2006-12-09 13:38:01	54081.3584953704	2006-12-12 08:36:14	701021010	120.6609	120	120.6849	120.6609	0	120.6769	2	2	0	2	1	0	0	109.3128	109.3128	241.052	3	PROCESSED	57536.3458680556	2016-05-28 08:18:03	54735	2008-09-26 00:00:00	54094.4773958333	2006-12-25 11:27:27	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010141	TON S180 is a luminous Narrow Line Seyfert 1 galaxy, chracterizing enhanced Soft X-ray emission component without complex absorption/emission structures. The source is considered to be at super Eddington accretion rate. We aim to track change (or no change) in soft X-ray spectrum of this source according to factor of two ,rapid flux variation this source show. We partciularly focus on the slim disk model propsed for super Eddington accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	C	KIYOSHI HAYASHIDA		JAP	1	AO1	SOFT X-RAY EMISSION FROM SUPER-EDDINGTON ACCRETION DISK IN TON S180	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701021010/	Quick Look
195	MARKARIAN 335	1.5539	20.2624	0.911019	19.984083	9.744165	17.917566	108.74842011	-41.36053721	68.4831	53907.0624537037	2006-06-21 01:29:56	53910.7585532407	2006-06-24 18:12:19	701031010	151.2884	150	151.2964	151.2884	151.2964	151.2964	2	2	2	2	1	0	0	140.9812	140.9812	319.3028	4	PROCESSED	57534.8340046296	2016-05-26 20:00:58	54401	2007-10-28 00:00:00	53928.5392361111	2006-07-12 12:56:30	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011323	We propose to observe the two Seyfert 1 galaxies Mrk 335 and ESO198-G024 for a total exposure of 150 ks each with the high sensitivity and broad band coverage of the Suzaku satellite. Both sources show a broad Fe K line and a strong soft excess. One appealing explanation for the nature of the soft excess is reflection. Fundamental to this hypothesis is the assumption that the same self-consistent reflection spectrum explains the Fe K line (including its shape), the soft excess, and also the Compton reflection hump above 20 keV. Suzaku's ability to measure all three reflection components simultaneously enables the different spectral models to be disentangled and reflection to be strongly tested. Understanding black hole accretion is fundamental to NASA's "SEU" theme.	EXTRAGALACTIC COMPACT SOURCES	7	B	JON MILLER		USA	1	AO1	REVEALING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701031010/	Quick Look
196	NGC 1068	40.6928	-0.0667	40.052721	-0.278811	38.248989	-15.097296	172.18986515	-51.95763403	248.588	54141.0038078704	2007-02-10 00:05:29	54141.9168287037	2007-02-10 22:00:14	701039010	41.6229	35	41.6309	41.6309	0	41.6229	2	2	0	2	1	0	0	41.8024	41.8024	78.8839	0	PROCESSED	57537.346875	2016-05-29 08:19:30	54525	2008-02-29 00:00:00	54151.5012962963	2007-02-20 12:01:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011333	The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB.	EXTRAGALACTIC COMPACT SOURCES	7	C	AARON STEFFEN		USA	1	AO1	MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701039010/	Quick Look
197	MARKARIAN 509	311.0427	-10.7271	310.361616	-10.908673	310.545205	7.124386	35.96837179	-29.85867019	254.3019	54022.3263888889	2006-10-14 07:50:00	54023.0856365741	2006-10-15 02:03:19	701093020	25.9298	25	25.9618	25.9298	25.9538	25.9618	2	2	2	2	1	0	0	23.4497	23.4497	65.5899	1	PROCESSED	57535.8399305556	2016-05-27 20:09:30	54526	2008-03-01 00:00:00	54053.6032638889	2006-11-14 14:28:42	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012050	We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV).	EXTRAGALACTIC COMPACT SOURCES	7	A	GABRIELE PONTI		EUR	1	AO1	SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093020/	Quick Look
198	MARKARIAN 509	311.0451	-10.7278	310.364015	-10.909382	310.547312	7.12309	35.96880101	-29.86110163	254.2048	54066.1625810185	2006-11-27 03:54:07	54067.12875	2006-11-28 03:05:24	701093040	33.0944	32	33.0944	33.0944	0	33.0944	2	2	0	2	1	0	0	29.4544	29.4544	83.4659	1	PROCESSED	57536.2044212963	2016-05-28 04:54:22	54456	2007-12-22 00:00:00	54088.5895023148	2006-12-19 14:08:53	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012050	We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV).	EXTRAGALACTIC COMPACT SOURCES	7	A	GABRIELE PONTI		EUR	1	AO1	SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093040/	Quick Look
199	PKS 1510-089	228.2108	-9.1043	227.537329	-8.917552	228.287746	8.492539	351.2856545	40.1353659	286.8003	53949.3968634259	2006-08-02 09:31:29	53952.2544444445	2006-08-05 06:06:24	701094010	119.1577	120	119.1577	119.1577	119.1657	119.1657	2	2	2	2	1	0	0	106.2588	106.2588	246.8638	5	PROCESSED	57535.1605208333	2016-05-27 03:51:09	54394	2007-10-21 00:00:00	54018.7363194444	2006-10-10 17:40:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	013016	It has been a long mystery (i) how the relativistic jets are formed, and (ii) what is the composition of a jet. In the theoretical view, strong magnetic field (u_B >> u_e) is necessary to produce such outflows with baryonic matters, but observations favor opposite scenario, namely particle dominated (u_e >> u_B), leptonic jet. Such discrepancies can be resolved if moderate numbers of protons (n_e/n_p > 50) are mixed in the non-tnermal pair populations. This can be easily tested if we can observe characteristic "soft X-ray bump" produced by the bulk-Comptonization of UV photons emitted from an accretion disk. We propose a deep observation (40ksec x3) of an EGRET quasar PKS 1510-089, which shows a clear sign of soft X-ray bump in BeppoSAX, ROSAT and ASCA observations.	EXTRAGALACTIC COMPACT SOURCES	7	B	JUN KATAOKA	GRZEGORZ MADEJSKI	JUS	1	AO1	DIRECT TESTING THE JET COMPOSITION IN A POWERFUL EGRET QUASAR PKS 1510-089	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701094010/	Quick Look
200	Z8852	347.6318	7.5789	346.999079	7.307292	351.631711	11.858062	84.17423864	-47.55525942	260.3346	54065.5867013889	2006-11-26 14:04:51	54066.1543287037	2006-11-27 03:42:14	801074010	14.8526	15	14.8526	14.8526	0	14.8526	2	2	0	2	1	0	0	13.9834	13.9834	49.0379	0	PROCESSED	57536.1918402778	2016-05-28 04:36:15	54695	2008-08-17 00:00:00	54088.6000694444	2006-12-19 14:24:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801074010/	Quick Look
201	A2495	342.5662	10.9218	341.941655	10.656649	348.262816	16.910805	81.19678392	-41.92445268	65.1354	54260.5857523148	2007-06-09 14:03:29	54261.1668287037	2007-06-10 04:00:14	801080020	25.7806	18	25.7806	25.7806	0	25.7806	2	2	0	2	1	0	0	20.9762	20.9762	50.1959	2	PROCESSED	57538.8757291667	2016-05-30 21:01:03	54695	2008-08-17 00:00:00	54270.430625	2007-06-19 10:20:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080020/	Quick Look
202	NGC 1667	72.1445	-6.2644	71.533156	-6.35119	69.717897	-28.457954	203.99435404	-30.10712566	81.9813	53964.3614814815	2006-08-17 08:40:32	53965.2536805556	2006-08-18 06:05:18	701006010	39.253	40	39.253	39.261	39.261	39.261	2	2	2	2	1	0	0	35.7281	35.7281	77.0759	0	PROCESSED	57535.2875578704	2016-05-27 06:54:05	54526	2008-03-01 00:00:00	54020.7803009259	2006-10-12 18:43:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010037	We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	1	AO1	COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701006010/	Quick Look
203	NGC4418	186.7074	-0.9383	186.066307	-0.661629	186.526079	1.80107	290.03230216	61.31559989	292.8039	53929.4791898148	2006-07-13 11:30:02	53931.280775463	2006-07-15 06:44:19	701001010	68.3485	70	68.3485	68.3485	68.3485	68.3485	2	2	2	2	1	0	0	57.1103	57.1103	155.634	1	PROCESSED	57534.9858564815	2016-05-26 23:39:38	54408	2007-11-04 00:00:00	53942.4601388889	2006-07-26 11:02:36	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010001	We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASATOSHI IMANISHI		JAP	1	AO1	COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701001010/	Quick Look
204	PKS 0558-504	89.9338	-50.4417	89.630316	-50.442779	89.864771	-73.883563	257.95388656	-28.57696937	207.8266	54117.4686226852	2007-01-17 11:14:49	54118.1127777778	2007-01-18 02:42:24	701011010	20.6207	20	20.6207	20.6207	0	20.6207	2	2	0	2	1	0	0	18.914	18.914	55.6479	0	PROCESSED	57536.8527777778	2016-05-28 20:28:00	54735	2008-09-26 00:00:00	54133.0355787037	2007-02-02 00:51:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010057	Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	C	YOSHITO HABA		JAP	1	AO1	SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011010/	Quick Look
205	PKS 0558-504	89.9338	-50.4409	89.630307	-50.441979	89.864775	-73.882763	257.95298672	-28.57684464	209.1054	54118.6998032407	2007-01-18 16:47:43	54119.2654976852	2007-01-19 06:22:19	701011020	18.8753	20	18.8753	18.8753	0	18.8753	2	2	0	2	1	0	0	18.0497	18.0497	48.87	1	PROCESSED	57536.8739814815	2016-05-28 20:58:32	54735	2008-09-26 00:00:00	54133.3967361111	2007-02-02 09:31:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010057	Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	C	YOSHITO HABA		JAP	1	AO1	SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011020/	Quick Look
206	KAZ 102	270.6661	67.6374	270.701804	67.634057	77.059679	88.893324	97.62313354	29.55178422	2.066	53895.6833101852	2006-06-09 16:23:58	53896.5343055556	2006-06-10 12:49:24	701012010	41.454	40	41.454	41.462	41.47	41.47	2	2	2	2	1	0	0	40.9507	40.9507	73.5199	2	PROCESSED	57534.6269328704	2016-05-26 15:02:47	54394	2007-10-21 00:00:00	53928.2501157407	2006-07-12 06:00:10	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010112	We propose to make a detailed broad-band X-ray spectroscopic study of the radio quiet QSO (RQQ) Kaz 102. This RQQ had a power-law spectrum with a photon index ~ 1 with our ASCA observation. We also found a spectral variability over the time scale of years, from ~ 2.2 during the ROSAT All Sky Survey to ~ 1 during the Einstein / ASCA observations. From our ASCA spectra, we couldn't discriminate whether the apparently unusual hard spectrum was caused by warm absorber, Compton reflection, or a simple featureless power-law continuum. High quality and wide-band spectroscopy with Suzaku is essential to unveil the physical nature of the enigmatic hardness and spectral variability of Kaz 102.	EXTRAGALACTIC COMPACT SOURCES	7	B	YOSHITAKA ISHISAKI		JAP	1	AO1	WHAT IS THE PHYSICAL NATURE OF KAZ 102: AN ENIGMATIC X-RAY HARD RADIO QUIET QSO?	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701012010/	Quick Look
207	1ES1218+304	185.3064	30.1169	184.679878	30.394195	171.661841	29.481192	186.88913956	82.72978014	298.9428	53874.8006365741	2006-05-19 19:12:55	53876.706412037	2006-05-21 16:57:14	701025010	79.8692	80	79.8852	79.8692	79.8852	79.8772	2	2	2	2	1	0	0	70.5118	70.5118	164.6379	2	PROCESSED	57534.4292013889	2016-05-26 10:18:03	54398	2007-10-25 00:00:00	53927.8564930556	2006-07-11 20:33:21	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010157	We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV)	EXTRAGALACTIC COMPACT SOURCES	7	A	TADAYUKI TAKAHASHI		JAP	1	AO1	SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701025010/	Quick Look
208	1ES1426+428	217.0716	42.6249	216.585066	42.847682	193.182318	52.911489	77.44668506	64.96380656	316.1862	53902.7388310185	2006-06-16 17:43:55	53904.2225	2006-06-18 05:20:24	701026010	60.9149	60	60.9149	60.9149	60.9149	60.9149	2	2	2	2	1	0	0	54.0911	54.0911	128.16	1	PROCESSED	57534.6747800926	2016-05-26 16:11:41	54400	2007-10-27 00:00:00	53928.3009143518	2006-07-12 07:13:19	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010157	We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV)	EXTRAGALACTIC COMPACT SOURCES	7	A	TADAYUKI TAKAHASHI		JAP	1	AO1	SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701026010/	Quick Look
209	MRK 501	253.4	39.7089	252.98087	39.789378	242.4893	61.571247	63.52834502	38.90621529	316.9908	53934.7872569444	2006-07-18 18:53:39	53935.7272916667	2006-07-19 17:27:18	701027010	42.4271	40	42.4389	42.4389	42.4271	42.4351	2	2	2	2	1	0	0	39.9711	39.9711	81.2099	0	PROCESSED	57534.9978587963	2016-05-26 23:56:55	54408	2007-11-04 00:00:00	53971.6784259259	2006-08-24 16:16:56	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010157	We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV)	EXTRAGALACTIC COMPACT SOURCES	7	A	TADAYUKI TAKAHASHI		JAP	1	AO1	SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701027010/	Quick Look
210	NGC 4552	188.9456	12.612	188.314388	12.887225	183.105993	15.109639	287.9907408	75.02773792	120.0696	54072.312974537	2006-12-03 07:30:41	54072.8405092593	2006-12-03 20:10:20	701037010	20.4398	20	20.4398	20.4398	0	20.4398	1	1	0	1	1	0	0	16.553	16.553	45.5439	0	PROCESSED	57536.226875	2016-05-28 05:26:42	54455	2007-12-21 00:00:00	54088.5410069444	2006-12-19 12:59:03	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011333	The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB.	EXTRAGALACTIC COMPACT SOURCES	7	C	AARON STEFFEN		USA	1	AO1	MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701037010/	Quick Look
211	PDS 456	262.0807	-14.2604	261.370018	-14.220332	262.221238	8.96686	10.39565911	11.16772638	98.239	54155.7486574074	2007-02-24 17:58:04	54160.0355787037	2007-03-01 00:51:14	701056010	190.6002	188	190.6082	190.6002	0	190.6142	2	2	0	2	1	0	0	176.4708	176.4708	370.3428	4	PROCESSED	57537.5850578704	2016-05-29 14:02:29	54757	2008-10-18 00:00:00	54168.6244560185	2007-03-09 14:59:13	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011351	A long 150ks Suzaku observation of the most luminous nearby quasar, PDS 456, is proposed. In the X-ray band, PDS 456 shows a deep iron K absorption trough. One possibility is that the absorption arises from a massive 0.1c outflow, of column density 10^24 cm^-2. Such an outflow would represent a significant fraction of the quasar energy budget. A deep Suzaku observation is proposed to test this outflow model, in particular the high energy bandpass of Suzaku is essential for measuring the profile of the absorption feature and determining the kinematics of the outflow. It is also possible to differentiate between competing models for the iron K feature, most notably between an outflow and a strong reflection component from the innermost radii around a Kerr black hole.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		USA	1	AO1	SOLVING THE ORIGIN OF THE DEEP IRON K ABSORPTION IN PDS 456	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701056010/	Quick Look
212	BL LACERTAE	330.6466	42.3471	330.130697	42.105096	354.282545	49.658149	92.61224541	-10.37092111	71.9797	53882.2303703704	2006-05-27 05:31:44	53883.305775463	2006-05-28 07:20:19	701073010	48.5294	50	48.5454	48.5454	48.5294	48.5374	2	2	2	2	1	0	0	35.5443	35.5443	92.902	1	PROCESSED	57534.4514236111	2016-05-26 10:50:03	54401	2007-10-28 00:00:00	53926.2373032407	2006-07-10 05:41:43	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011377	We propose two 50 ks Suzaku observations, one for each of gamma-ray bright blazars PKS 1510-089 and BL Lacertae, to be coordinated with optical and radio observations. The goal is to obtain broadband spectra and light-curves. The X-ray fluxes are known to be rapidly variable, but there is no information about the correlation between the spectral shape and flux, which is necessary to establish the origin of previously detected prominent soft X-ray excesses. They are crucial to discriminate between different radiation scenarios responsible for production of hard X-rays and gamma-rays, and to constrain the content and by extension, the acceleration process of the jet. These observations will be ingredients of a "pilot" campaigns for the future joint Suzaku-GLAST investigations.	EXTRAGALACTIC COMPACT SOURCES	7	A	GRZEGORZ MADEJSKI		USA	1	AO1	SUZAKU OBSERVATIONS OF GAMMA-RAY BRIGHT BLAZARS BL LACERTAE AND PKS 1510-089	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701073010/	Quick Look
213	MARKARIAN 509	311.0194	-10.6637	310.338544	-10.845188	310.53976	7.19158	36.02321332	-29.81091499	73.1708	53850.7831481482	2006-04-25 18:47:44	53851.5252199074	2006-04-26 12:36:19	701093010	24.5756	25	24.5756	24.5756	24.5916	24.5916	2	2	2	2	1	0	0	15.407	15.407	64.0979	1	PROCESSED	57533.5586342593	2016-05-25 13:24:26	54394	2007-10-21 00:00:00	53907.6894560185	2006-06-21 16:32:49	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012050	We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV).	EXTRAGALACTIC COMPACT SOURCES	7	A	GABRIELE PONTI		EUR	1	AO1	SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093010/	Quick Look
214	A2104N	235.0318	-3.1802	234.37876	-3.019346	233.471257	15.936264	2.94593816	39.29281704	117.689	54119.2779166667	2007-01-19 06:40:12	54119.7522337963	2007-01-19 18:03:13	801002010	18.8424	20	18.8424	18.8424	0	18.8424	2	2	0	2	1	0	0	13.6448	13.6448	40.9779	1	PROCESSED	57536.8705439815	2016-05-28 20:53:35	54735	2008-09-26 00:00:00	54133.3893518518	2007-02-02 09:20:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010012	We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO HATTORI		JAP	1	AO1	TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801002010/	Quick Look
215	NGC 507	20.9105	33.2598	20.206045	32.999169	32.202982	22.611804	130.6367604	-29.12969375	54.0771	53944.6189351852	2006-07-28 14:51:16	53946.5544444444	2006-07-30 13:18:24	801017010	79.5013	80	79.5253	79.5013	79.5253	79.5253	2	2	2	2	1	0	0	80.2867	80.2867	167.17	2	PROCESSED	57535.1047222222	2016-05-27 02:30:48	54394	2007-10-21 00:00:00	53955.7736689815	2006-08-08 18:34:05	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010061	We propose to observe luminous elliptical galaxies NGC 507 and NGC 499 for 80 and 100 ksec, respectively, to study abundance distribution of Fe and O. The good energy resolution and low background of the XIS instrument is crucial for this study, and we can perform the first reliable measurement of O distribution around elliptical galaxies. Comparison of O and Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. Comparison of NGC 507 and NGC 499 will show us how much metal production process differ with galaxy size.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KOSUKE SATO		JAP	1	AO1	CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES IN GROUP OF GALAXIES: NGC 507 AND NGC 499	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801017010/	Quick Look
216	OPHIUCHUS CLUSTER 2	257.7375	-23.3864	256.979428	-23.325463	258.749053	-0.422802	0.3572282	9.54416529	94.9391	54181.1423726852	2007-03-22 03:25:01	54181.825162037	2007-03-22 19:48:14	801023010	24.6782	15	24.7022	24.6942	0	24.6782	2	2	0	2	1	0	0	21.2781	21.2781	58.9879	1	PROCESSED	57537.9744097222	2016-05-29 23:23:09	54736	2008-09-27 00:00:00	54209.5433217593	2007-04-19 13:02:23	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010065	The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUTAKA FUJITA		JAP	1	AO1	PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801023010/	Quick Look
217	A2319CENTER	290.3341	43.878	289.944223	43.782148	306.012819	64.798086	75.63759851	13.45022652	251.6652	54035.9326041667	2006-10-27 22:22:57	54038.1466898148	2006-10-30 03:31:14	801040010	99.5332	100	99.5492	99.5412	99.5332	99.5492	2	2	2	2	1	0	0	93.9548	93.9548	191.268	2	PROCESSED	57535.9905555556	2016-05-27 23:46:24	54735	2008-09-26 00:00:00	54063.5741666667	2006-11-24 13:46:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010085	We propose the observations of the A2319 cluster with the Suzaku HXD and XIS to investigate particle acceleration processes in the intracluster medium(ICM). A2319 is a nearby massive merging cluster whose collision axis is nearly along the line of sight, and has diffuse non-thermal radio emission. We will detect non-thermal hard X-ray with HXD, and determine the velocity difference between the two subclusters with XIS. With these results, we will determine dynamical status of the ICM and get implications on the particle acceleration processes. We will compare the results with theoretical models, numerical simulations, and radio and optical observations to get an overall picture of particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MOTOKAZU TAKIZAWA		JAP	1	AO1	PARTICLE ACCELERATION IN THE A2319 CLUSTER	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801040010/	Quick Look
218	PERSEUS CL OFFSET	50.5735	41.8053	49.742345	41.626976	59.178685	22.492416	150.80595618	-12.75877318	65.9956	53982.1426736111	2006-09-04 03:25:27	53982.4377893518	2006-09-04 10:30:25	801049040	10.4206	30	10.4206	10.4206	10.4206	10.4206	2	2	2	2	1	0	0	7.5402	7.5402	25.4679	1	PROCESSED	57535.4390856482	2016-05-27 10:32:17	54526	2008-03-01 00:00:00	54021.0033680556	2006-10-13 00:04:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010097	We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	1	AO1	MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049040/	Quick Look
219	NGC3923	177.7599	-28.8047	177.126048	-28.526534	190.367331	-27.106442	287.27787622	32.22445477	293.1988	53899.8430671296	2006-06-13 20:14:01	53902.7293287037	2006-06-16 17:30:14	801054010	115.82	120	115.828	115.82	115.828	115.828	2	2	2	2	1	0	0	107.7313	107.7313	249.3528	3	PROCESSED	57534.7187731482	2016-05-26 17:15:02	54394	2007-10-21 00:00:00	53927.2880902778	2006-07-11 06:54:51	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010100	We propose to observe an isolated elliptical galaxy NGC3923, to meaasure a dark matter distribution. The large effective area and stable low background of XIS enable us to measure a faint extended X-ray emission such as the periphery of elliptical galaxies more accurately than ever. Since X-ray bright elliptical galaxies have been found to be surrounded by group-scale emission, X-ray faint elliptical galaxies are the best to investigate the dark matter associated with the galaxy itself. The dark matter around galaxies is a key to resolve the problem of why X-ray bright and faint elliptical galaxies exist. The oxygen abundance distribution is also useful to probe the above issue.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YASUSHI FUKAZAWA		JAP	1	AO1	ACCURATE MEASUREMENT OF DARK MATTER DISTRIBUTION AROUND AN ISOLATED ELLIPTICAL GALAXY NGC3923	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801054010/	Quick Look
220	NGC 4472	187.4441	8.005	186.80838	8.281234	183.627851	10.299036	286.9163593	70.20028227	117.8054	54072.8427893518	2006-12-03 20:13:37	54075.7014699074	2006-12-06 16:50:07	801064010	121.0358	120	121.0358	121.0358	0	121.0358	2	2	0	2	1	0	0	103.4464	103.4464	246.9548	6	PROCESSED	57536.3089467593	2016-05-28 07:24:53	54702	2008-08-24 00:00:00	54089.1857523148	2006-12-20 04:27:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011403	We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MICHAEL LOEWENSTEIN		USA	1	AO1	INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801064010/	Quick Look
221	NGC 4649	190.9148	11.557	190.284732	11.830628	185.371113	14.926523	295.86493189	74.32191724	113.3108	54098.4203703704	2006-12-29 10:05:20	54104.1473263889	2007-01-04 03:32:09	801065010	224.0304	120	224.0304	224.0304	0	224.0304	2	2	0	2	1	0	0	26.3042	26.3042	69.2898	1	PROCESSED	57536.4300578704	2016-05-28 10:19:17	54743	2008-10-04 00:00:00	54132.9809027778	2007-02-01 23:32:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011403	We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MICHAEL LOEWENSTEIN		USA	1	AO1	INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801065010/	Quick Look
222	UGC03957	115.2433	55.429	114.235063	55.545488	106.863653	33.455815	162.22286538	28.93195726	271.243	53841.9927314815	2006-04-16 23:49:32	53842.2828587963	2006-04-17 06:47:19	801072010	10.7714	12	10.7794	10.7794	10.7874	10.7714	1	1	1	1	1	0	0	9.642	9.642	25.0079	0	PROCESSED	57533.4729166667	2016-05-25 11:21:00	54401	2007-10-28 00:00:00	53906.7753240741	2006-06-20 18:36:28	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801072010/	Quick Look
223	A272	28.7603	33.9026	28.031098	33.657734	38.955118	20.665911	137.73606223	-27.1341127	64.9465	53943.0449537037	2006-07-27 01:04:44	53943.6842476852	2006-07-27 16:25:19	801084010	22.2455	21	22.2535	22.2535	22.2455	22.2535	2	2	2	2	1	0	0	24.6035	24.6035	55.2319	0	PROCESSED	57535.0602430556	2016-05-27 01:26:45	54401	2007-10-28 00:00:00	53955.6516782407	2006-08-08 15:38:25	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801084010/	Quick Look
224	A566	106.0915	63.2647	104.91759	63.339113	99.420321	40.34898	152.76309519	25.45548296	285.637	54178.3128587963	2007-03-19 07:30:31	54178.8029976852	2007-03-19 19:16:19	801085010	22.2711	20	22.2711	22.2711	0	22.2711	2	2	0	2	1	0	0	22.1523	22.1523	42.3399	0	PROCESSED	57537.7151157407	2016-05-29 17:09:46	54695	2008-08-17 00:00:00	54185.9799305556	2007-03-26 23:31:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801085010/	Quick Look
225	RXJ 0658	104.704	-55.933	104.461428	-55.862903	130.333928	-77.302143	266.02429497	-21.20357002	164.9362	54095.6181597222	2006-12-26 14:50:09	54098.4099421296	2006-12-29 09:50:19	801089010	101.3845	100	101.3845	101.3845	0	101.3845	2	2	0	2	1	0	0	84.3679	84.3679	241.1547	2	PROCESSED	57637.5971180556	2016-09-06 14:19:51	54702	2008-08-24 00:00:00	54111.5842013889	2007-01-11 14:01:15	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011448	We propose SUZAKU X-ray observations of an intriguing cluster of galaxies, RXJ0658, to determine and characterize the nature of the hard X-ray spectral emission and other nonthermal activity. It also has many other interesting features, such as a cold front, evidence for merger, a shock, and regions of unusually high temperature, all of which are related to the hard X-ray emission and the nonthermal activity. The more accurate measure of the spectral characteristics of the hard component, when combined with the radio and other past X-ray data, can reveal the nature of the emission process and the acceleration mechanism of the relativistic electrons, provide a means of measuring the magnetic field strength, and aid in understanding the process of formation of clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	VAHE PETROSIAN		USA	1	AO1	HARD X-RAY EMISSION FROM CLUSTER RXJ0658	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801089010/	Quick Look
226	RXJ1713-3946	258.5527	-40.0289	257.68331	-39.971559	260.849002	-16.950052	347.19063141	-0.73133412	268.0015	53997.9147569444	2006-09-19 21:57:15	53998.4425925926	2006-09-20 10:37:20	501070010	20.7442	20	20.7442	20.7522	20.7522	20.7522	2	2	2	2	1	0	0	22.0266	22.0266	45.5959	1	PROCESSED	57535.6347685185	2016-05-27 15:14:04	54526	2008-03-01 00:00:00	54021.1763541667	2006-10-13 04:13:57	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501070010/	Quick Look
227	COMA RADIO HALO	194.9267	27.9061	194.323466	28.175433	181.517491	31.325949	56.39742233	88.00849705	295.2687	53886.8435300926	2006-05-31 20:14:41	53890.7439699074	2006-06-04 17:51:19	801097010	178.6572	180	178.6892	178.6572	178.7132	178.6892	2	2	2	2	1	0	0	167.4506	167.4506	336.9758	7	PROCESSED	57534.5953472222	2016-05-26 14:17:18	54401	2007-10-28 00:00:00	53926.6760416667	2006-07-10 16:13:30	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014446	We will observe the central regions of the Coma cluster with the HXD/PIN to detect and characterize the nonthermal Inverse Compton (IC) emission from the radio halo. Coma has the best-studied and brightest radio halo, which makes it the best case to detect IC and the most useful one for testing theories for the origin of radio halos. Previous detections with BeppoSAX and RXTE are controversial. Suzaku is more sensitive, will avoid contamination by nearby AGNs including X Comae, and will detect IC even if it is fainter than the claimed BeppoSAX detection. The HXD/PIN data will allow the cluster magnetic field, and nonthermal energy and pressure to be derived. The XIS observations will be used to determine accurate abundances and gradients in Coma, and to test theories for ICM enrichment.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	CRAIG SARAZIN	KYOKO MATSUSHITA	USJ	1	AO1	NAILING DOWN THE HARD X-RAY INVERSE COMPTON EMISSION FROM THE RADIO HALO IN THE COMA CLUSTER	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801097010/	Quick Look
228	OPHIUCHUS CLUSTER BG	257.0147	-25.0612	256.247464	-24.996818	258.237934	-2.148508	358.58755189	9.10838139	89.7146	54183.5662268518	2007-03-24 13:35:22	54183.9169444444	2007-03-24 22:00:24	801030010	15.2983	15	15.3063	15.3063	0	15.2983	2	2	0	2	1	0	0	14.6351	14.6351	30.296	0	PROCESSED	57537.9841898148	2016-05-29 23:37:14	54736	2008-09-27 00:00:00	54209.5187384259	2007-04-19 12:26:59	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010065	The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUTAKA FUJITA		JAP	1	AO1	PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801030010/	Quick Look
229	AWM7 WEST OFFSET	43.2295	41.594	42.421509	41.389857	53.412323	23.911285	146.06522235	-15.7568529	90.4999	53953.2407060185	2006-08-06 05:46:37	53954.2343171296	2006-08-07 05:37:25	801037010	39.8177	40	39.8497	39.8177	39.8497	39.8497	2	2	2	2	1	0	0	38.1089	38.1089	85.8359	1	PROCESSED	57535.2509375	2016-05-27 06:01:21	54394	2007-10-21 00:00:00	54020.7562384259	2006-10-12 18:08:59	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010076	The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKAYA OHASHI		JAP	1	AO1	SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801037010/	Quick Look
230	A2256	256.0138	78.7112	256.73222	78.776756	102.386288	77.234603	111.08264828	31.72462704	207.9671	54049.8560069445	2006-11-10 20:32:39	54052.0834722222	2006-11-13 02:00:12	801061010	95.5111	100	95.5111	95.5111	0	95.5111	2	2	0	2	1	0	0	103.5789	103.5789	192.4418	4	PROCESSED	57536.1203009259	2016-05-28 02:53:14	54456	2007-12-22 00:00:00	54089.4338425926	2006-12-20 10:24:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010139	A2256 is a nearby (z=0.058) rich cluster with strong X-ray emission. The cluster has variety of indications of a on-going merger; two peaks separated by 3.5 arcmin are clearly visible near the center of X-ray emission, gas temperature map show sub structure and a cold front etc. The velocity distribution of member galaxies also exhibits two or three sub groups in this cluster. We measure the bulk motion of the hot gas using Suzaku XIS, in particular, about 2000km/s velocity difference between the main-cluster and the sub-cluster is the target. We also aim to search for hard X-ray emission claimed by previous missions with Suzaku HXD.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	KIYOSHI HAYASHIDA		JAP	1	AO1	BULK MOTION AND NON THERMAL PROCESS IN THE MERGING CLUSTER A2256	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801061010/	Quick Look
231	SERSIC 159-03	348.4959	-42.7314	347.802109	-43.003937	330.666566	-34.355163	348.33340728	-64.81387916	47.3295	53851.5323611111	2006-04-26 12:46:36	53853.2668055556	2006-04-28 06:24:12	801093010	67.7843	70	67.8003	67.8003	67.7843	67.7923	2	2	2	2	1	0	0	41.5833	41.5833	149.8278	2	PROCESSED	57533.6210532407	2016-05-25 14:54:19	54400	2007-10-27 00:00:00	53907.8625231482	2006-06-21 20:42:02	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012045	We propose to observe the cluster of galaxies Sersic 159-03 using a total exposure time of 70 ks to investigate the soft excess emission previously detected in the observations with ROSAT and XMM-Newton. The superior redistribution function of Suzaku will allow us to determine whether the O VII line emission detected with XMM-Newton is of local (Galactic) origin or is emitted by the warm-hot intergalactic medium (WHIM) in the vicinity of the cluster. The strong soft emission around this cluster together with the much improved response function of the XIS detectors at low energies make Sersic 159-03 the most promising target to unambiguously detect the WHIM for the first time in emission with Suzaku.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JELLE KAASTRA		EUR	1	AO1	O VII LINE EMISSION IN SERSIC 159-03 - WHIM OR GALACTIC ORIGIN?	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801093010/	Quick Look
232	GALACTIC CENTER GC10	266.4308	-29.5343	265.632731	-29.515028	266.867639	-6.131965	359.50116476	-0.33080245	109.7996	54171.9994097222	2007-03-12 23:59:09	54172.6529976852	2007-03-13 15:40:19	501055010	27.2257	25	27.2257	27.2497	0	27.2337	2	2	0	2	1	0	0	21.1819	21.1819	56.4539	0	PROCESSED	57537.6665740741	2016-05-29 15:59:52	54736	2008-09-27 00:00:00	54182.3161342593	2007-03-23 07:35:14	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501055010/	Quick Look
233	A2061	230.3095	30.6453	229.795666	30.824015	216.361499	46.967712	48.13899774	57.1713197	293.2901	53943.6955092593	2006-07-27 16:41:32	53943.9946643518	2006-07-27 23:52:19	801081010	13.8887	14	13.9047	13.9047	13.8887	13.8967	1	1	1	1	1	0	0	11.8443	11.8443	25.8399	0	PROCESSED	57535.0552083333	2016-05-27 01:19:30	54401	2007-10-28 00:00:00	53955.6442939815	2006-08-08 15:27:47	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801081010/	Quick Look
234	A2249	257.46	34.4851	257.00595	34.546595	250.753931	57.089244	57.64541352	34.94797305	129.9858	54114.5939467593	2007-01-14 14:15:17	54115.1252777778	2007-01-15 03:00:24	801082010	22.8156	15	22.8156	22.8236	0	22.8236	1	1	0	1	1	0	0	19.7637	19.7637	45.9039	1	PROCESSED	57536.8308333333	2016-05-28 19:56:24	54695	2008-08-17 00:00:00	54133.0295833333	2007-02-02 00:42:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801082010/	Quick Look
235	GALACTIC CENTER GC9	266.6299	-29.2499	265.833607	-29.231598	267.035089	-5.843458	359.83430056	-0.33104727	109.8001	54171.3410532407	2007-03-12 08:11:07	54171.9988888889	2007-03-12 23:58:24	501054010	26.1044	25	26.1044	26.1044	0	26.1044	2	2	0	2	1	0	0	23.5424	23.5424	56.8299	0	PROCESSED	57537.6542013889	2016-05-29 15:42:03	54736	2008-09-27 00:00:00	54182.2954166667	2007-03-23 07:05:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501054010/	Quick Look
236	JUPITER	226.6349	-16.1983	225.936085	-16.00589	228.727521	1.247844	344.01962259	35.67652355	118.4908	53793.86	2006-02-27 20:38:24	53794.9585532407	2006-02-28 23:00:19	401001040	42.2558	36	42.2638	42.2638	42.2638	42.2558	2	2	2	2	1	0	0	35.7067	35.7067	94.9059	2	PROCESSED	57533.1103819444	2016-05-25 02:38:57	54401	2007-10-28 00:00:00	53906.5712615741	2006-06-20 13:42:37	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011003	We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure.	GALACTIC POINT SOURCES	4	C	RONALD ELSNER		USA	1	AO1	JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001040/	Quick Look
237	NGC 5044	198.8504	-16.3899	198.183934	-16.125889	203.593771	-7.791309	311.2339251	46.09520433	290.0016	53918.7631712963	2006-07-02 18:18:58	53919.3600115741	2006-07-03 08:38:25	801046010	19.7466	20	19.7466	19.7466	19.7466	19.7466	2	2	2	2	1	0	0	17.9716	17.9716	51.562	1	PROCESSED	57534.8255208333	2016-05-26 19:48:45	54394	2007-10-21 00:00:00	53930.6133217593	2006-07-14 14:43:11	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010092	We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KYOKO MATSUSHITA		JAP	1	AO1	THE METAL DISTRIBUTION OF THE NGC 5044 GROUP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801046010/	Quick Look
238	XTE J1856+053	284.159	5.396	283.54361	5.329341	286.008229	28.053142	38.32644604	1.30563349	89.2928	54178.8141666667	2007-03-19 19:32:24	54179.4321643518	2007-03-20 10:22:19	901004010	24.476	25	24.476	24.476	0	24.476	1	1	0	1	1	0	0	20.1108	20.1108	53.3919	0	PROCESSED	57537.7386805556	2016-05-29 17:43:42	54171	2007-03-12 00:00:00	54185.38	2007-03-26 09:07:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	017020	Observation for a outburst of XTE J1856+053 (ATEL #1024)	GALACTIC POINT SOURCES	9	A	SWG		JAP	1	TOO	TOO OBSERVATION OF XTE J1856+053	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/901004010/	Quick Look
239	4U 1705-44	257.2313	-44.1028	256.328133	-44.039108	260.196098	-21.094402	343.32206131	-2.34487049	297.0793	54014.4242708333	2006-10-06 10:10:57	54015.0891087963	2006-10-07 02:08:19	401046030	20.065	20	20.065	20.065	20.065	20.065	2	2	2	2	1	0	0	17.9196	17.9196	57.4239	2	PROCESSED	57535.7945138889	2016-05-27 19:04:06	54526	2008-03-01 00:00:00	54021.6765162037	2006-10-13 16:14:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011112	We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state.	GALACTIC POINT SOURCES	4	A	ANDREW YOUNG		USA	1	AO1	REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046030/	Quick Look
240	PERSEUS CLUSTER	49.9436	41.5175	49.116107	41.336843	58.603575	22.345195	150.56798595	-13.25929387	66.0393	53976.788275463	2006-08-29 18:55:07	53980.0793865741	2006-09-02 01:54:19	101012010	150.9051	150	150.9051	150.9211	150.9371	150.9211	6	6	6	6	1	0	0	142.5334	142.5334	284.336	3	PROCESSED	57535.5159375	2016-05-27 12:22:57	53826	2006-04-01 00:00:00	54024.8648726852	2006-10-16 20:45:25	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015016	We propose the observation of Perseus cluster for 150ks. To recover the energy resolution of the XIS, we will try the periodic charge injection method. However, the charge injection will change calibrations such as gain, QE and so on dramatically. To study the change of the clibrations, Perseus cluster is one of the best targets, because it is extended over the whole XIS FOV and the iron K line from the cluster is extremely strong. For the first 50ks, the observation will be done with the normal mode without the charge injection. For the second and third 50ks, we will do the charge injections with every 54 and 108 rows, repectively.	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	1	AO1	PERSEUS OBSERVATION FOR CALIBRATIONS ON THE PERIODIC CHARGE INJECTION METHOD	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101012010/	Quick Look
241	M17	275.2076	-16.1829	274.486266	-16.206429	275.030512	7.16685	15.0906551	-0.7606192	110.1996	53805.8263425926	2006-03-11 19:49:56	53808.5349421296	2006-03-14 12:50:19	501003010	102.7021	100	102.7101	102.7101	102.7021	102.7101	2	2	2	2	1	0	0	92.5661	92.5661	233.9678	4	PROCESSED	57533.2492939815	2016-05-25 05:58:59	54394	2007-10-21 00:00:00	53905.822662037	2006-06-19 19:44:38	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010066	Recent Chandra observations discovered that HII regions possess a few MK extended plasma, but the origin of the emission is still unknown. We propose to observe M17, which has the most spectacular sample of such emission. A superb soft-band response of XIS will enable us to measure the strengths of O and N emission lines, giving us strong arguments to elucidate the cause of the emission. A 300 ks Chandra observation is planned this year in addition to the existing 40 ks data, which will help us to discriminate the point source contribution.	GALACTIC DIFFUSE EMISSION	5	A	MASAHIRO TSUJIMOTO		JAP	1	AO1	XIS INVESTIGATION FOR THE ORIGIN OF DIFFUSE X-RAY EMISSION IN GALACTIC H II REGIONS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501003010/	Quick Look
242	CTB 37B	258.4918	-38.2006	257.636889	-38.143005	260.643359	-15.13191	348.64561092	0.37683278	270.1267	53974.0604976852	2006-08-27 01:27:07	53976.2398032407	2006-08-29 05:45:19	501007010	82.8151	80	82.8711	82.8151	82.8791	82.8631	2	2	2	2	1	0	0	68.8603	68.8603	188.2779	2	PROCESSED	57535.4428703704	2016-05-27 10:37:44	54526	2008-03-01 00:00:00	54053.4840162037	2006-11-14 11:36:59	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010042	The Galactic Plane Survey with HESS found several new TeV sources, called as "dark particle accelerators". They must be powerful cosmic-ray accelerators, although their origin is still unknown due to the lack of information in other wavelengths. We investigate one of the extended sample with radio SNR counterpart, CTB 37B, which is marginally detected on the edge of ASCA GIS. ASCA spectrum shows rather soft power-law feature, indicating that there are both thermal and non-thermal X-ray emission. With the low background of XISs and HXD, parameters of both components are determined with 80 ks exposure. The non-thermal component suggests the new sample of accelerators, and the thermal compopent reveals the condition of the proton acceleration site, for the first time.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	1	AO1	UNCOVERING THE NATURE OF DARK PARTICLE ACCELERATORS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501007010/	Quick Look
243	GX 339-4	255.7025	-48.7916	254.754666	-48.72059	259.573177	-25.865576	338.93635594	-4.32587966	86.7489	54143.2316087963	2007-02-12 05:33:31	54146.2003009259	2007-02-15 04:48:26	401068010	77.2053	100	83.8935	77.2053	0	82.1138	2	2	0	2	1	0	0	94.026	94.026	256.484	4	PROCESSED	57537.4905208333	2016-05-29 11:46:21	54535	2008-03-10 00:00:00	54167.7751851852	2007-03-08 18:36:16	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011146	Skewed iron emission lines from the inner accretion disk and broad-band disk reflection spectra are incisive diagnostics of relativistic effects and the inner accretion flow geometry in black hole binaries. With its high effective area, efficient instrument modes, and sensitivity in hard X-rays, Suzaku is ideally suited to fully exploit these diagnostics. We request a total of 154 ksec in up to four observations to observe a black hole transient in outburst, using a scheme tailored to accommodate different source fluxes and Suzaku's observing windows. We will support these observations with a global multi-wavelength network of observatories. Understanding accretion onto black holes is central to NASA's ``SEU'' research theme.	GALACTIC POINT SOURCES	4	A	JON MILLER		USA	1	AO1-TOO	SUZAKU OBSERVATIONS OF A BLACK HOLE TRANSIENT IN OUTBURST	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401068010/	Quick Look
244	UGC5101	144.0189	61.4178	143.073331	61.641673	122.524313	43.933823	152.38145034	42.89433298	112.6892	54039.7635300926	2006-10-31 18:19:29	54040.396087963	2006-11-01 09:30:22	701002020	42.166	35	42.166	42.174	42.182	42.182	2	2	2	2	1	0	0	33.5589	33.5589	54.6519	0	PROCESSED	57536.0043518518	2016-05-28 00:06:16	54735	2008-09-26 00:00:00	54063.3945949074	2006-11-24 09:28:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010001	We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASATOSHI IMANISHI		JAP	1	AO1	COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701002020/	Quick Look
245	PKS 0558-504	89.9334	-50.4402	89.629898	-50.441281	89.86386	-73.882062	257.95215413	-28.57698713	210.2147	54119.7661805556	2007-01-19 18:23:18	54120.3203009259	2007-01-20 07:41:14	701011030	21.2563	20	21.2563	21.2563	0	21.2563	2	2	0	2	1	0	0	19.1145	19.1145	47.87	0	PROCESSED	57536.8847916667	2016-05-28 21:14:06	54735	2008-09-26 00:00:00	54133.3934259259	2007-02-02 09:26:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010057	Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	C	YOSHITO HABA		JAP	1	AO1	SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011030/	Quick Look
246	SWIFT J1628.1+5145	246.9541	51.8388	246.639575	51.948443	220.797096	71.358115	79.81767806	42.92326404	60.2479	53840.7843518518	2006-04-15 18:49:28	53841.3904976852	2006-04-16 09:22:19	701016010	23.589	20	23.605	23.597	23.589	23.597	1	1	1	1	1	0	0	20.6261	20.6261	52.3599	2	PROCESSED	57533.4625231482	2016-05-25 11:06:02	54394	2007-10-21 00:00:00	53905.7494444444	2006-06-19 17:59:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010133	Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background".	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	1	AO1	DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701016010/	Quick Look
247	SS 433	287.9531	4.9906	287.335307	4.906206	290.183209	27.182001	39.69950989	-2.2379409	78.6445	53829.6109606482	2006-04-04 14:39:47	53830.5327662037	2006-04-05 12:47:11	401003010	38.6767	40	38.6767	38.6767	38.6767	38.6767	2	2	2	2	1	0	0	28.2411	28.2411	79.634	1	PROCESSED	57533.395162037	2016-05-25 09:29:02	54394	2007-10-21 00:00:00	53906.1478125	2006-06-20 03:32:51	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010031	SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber.	GALACTIC POINT SOURCES	4	A	NOBUYUKI KAWAI		JAP	1	AO1	SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401003010/	Quick Look
248	NGC 4151	182.6375	39.4139	182.006166	39.692011	164.091601	36.628069	155.05374688	75.05753801	112.1087	54087.8369097222	2006-12-18 20:05:09	54090.3848726852	2006-12-21 09:14:13	701034010	124.9796	125	124.9796	124.9796	0	124.9796	2	2	0	2	1	0	0	131.2741	131.2741	220.1059	3	PROCESSED	57536.4582060185	2016-05-28 10:59:49	54702	2008-08-24 00:00:00	54132.849537037	2007-02-01 20:23:20	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011327	We propose a 100 ks Suzaku observation of the brightest Seyfert Galaxy in the sky. Given the broad band-pass, and high sensitivity, the proposed observations will provide a high-quality spectrum which will allow us to search for variability in the high-ionized absorber (compared to previous observations). We will be able to obtain stringent constraints on the "Reflection Hump" and compare it to the strength of the Fe Kalpha emission line - thus providing a direct test of Reflection models. The proposed program will also complement observations of fainter and more exotic Seyferts likely to be observed during AO-1.	EXTRAGALACTIC COMPACT SOURCES	7	A	IAN GEORGE		USA	1	AO1	DECOUPLING THE COMPONENTS IN THE BRIGHTEST SEYFERT: NGC 4151	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701034010/	Quick Look
249	HESS J1837-069	279.4395	-6.8651	278.765532	-6.909152	279.755327	16.256333	25.2664546	-0.10276403	102.6144	54164.5341898148	2007-03-05 12:49:14	54165.4286342593	2007-03-06 10:17:14	401026010	42.1911	40	42.1911	42.1991	0	42.2071	2	2	0	2	1	0	0	37.7021	37.7021	77.2599	1	PROCESSED	57537.6010185185	2016-05-29 14:25:28	54750	2008-10-11 00:00:00	54171.2613425926	2007-03-12 06:16:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010131	The HESS (High Energy Stereoscopic System) collaboration has recently reported the TeV survey of the inner-part of the Galaxy, which revealed the existence of a new population of gamma-ray objects. Most of which are unknown, but at least two of them, HESS J1813-178 and HESS J1837-069 are point-like, and the ASCA Galactic survey and the INTEGRAL survey detected the counterparts in 0.5-10 keV and 20-100 keV, respectively. Making full use of Suzaku's wide-band spectral capability, we will study spectral characteristics of HESS J1813-178 and HESS J1837-069 in 0.5 keV to ~200 keV, and investigate for their origins. We will also carry out pulse-search to evaluate the pulsar-wind hypothesis.	GALACTIC POINT SOURCES	4	B	KEN EBISAWA		JAP	1	AO1	INVESTIGATION OF TWO HESS SOURCES DETECTED WITH INTEGRAL	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401026010/	Quick Look
250	APM 08279+5255	127.9229	52.7639	126.990699	52.933179	116.237243	32.72103	165.74356471	36.23970609	100.0676	54040.3996643518	2006-11-01 09:35:31	54041.9690277778	2006-11-02 23:15:24	701057020	102.295	100	102.303	102.311	102.311	102.295	2	2	2	2	1	0	0	95.624	95.624	135.5778	1	PROCESSED	57536.0492592593	2016-05-28 01:10:56	54695	2008-08-17 00:00:00	54088.5241782407	2006-12-19 12:34:49	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011353	Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	1	AO1	VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057020/	Quick Look
251	NGC 5728	220.5794	-17.3095	219.88301	-17.096936	223.49481	-1.485509	337.26599487	38.0606459	290.4081	53935.7359143518	2006-07-19 17:39:43	53936.6264930556	2006-07-20 15:02:09	701079010	41.3077	40	41.3077	41.3077	41.3077	41.3077	2	2	2	2	1	0	0	39.569	39.569	76.9419	0	PROCESSED	57535.0121064815	2016-05-27 00:17:26	54400	2007-10-27 00:00:00	53943.5061111111	2006-07-27 12:08:48	3.0.22.43	6	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012016	The high-energy detectors onboard Swift and INTEGRAL have started to survey the hard X-ray sky above 10 keV. Although limited to bright X-ray fluxes (~10^-11 cgs), the large area surveyed so far has allowed to build up sizable sa mples of hard X-ray selected AGN almost unbiased against X-ray absorption. The AGN content of these surveys is dominated by obscured AGN. We have identified 3 objects which are most likely obscured by Compton-thick matter and very bright above 10 keV. We propose to observe them with Suzaku for 40 ks each to study their broad-band X-ray spectra and unveil previously unknown nearby heavily obscured AGN, with important consequences for the study of the AGN evolution and the synthesis of the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREA COMASTRI		EUR	1	AO1	BRIGHT COMPTON THICK GALAXIES IN THE BACKYARD	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701079010/	Quick Look
252	1RX J154814.5-452845	237.0511	-45.4226	236.175049	-45.269354	245.126412	-24.783918	332.46961393	7.07040697	85.7358	54132.6368518518	2007-02-01 15:17:04	54135.3543865741	2007-02-04 08:30:19	401037010	99.4541	100	99.4541	99.4621	0	99.4701	2	2	0	2	1	0	0	86.8552	86.8552	234.7838	3	PROCESSED	57537.0252777778	2016-05-29 00:36:24	54702	2008-08-24 00:00:00	54139.4767939815	2007-02-08 11:26:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011102	Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber.	GALACTIC POINT SOURCES	4	A	KOJI MUKAI		USA	1	AO1	BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401037010/	Quick Look
253	4U 1705-44	257.2281	-44.1019	256.324944	-44.038193	260.193555	-21.093723	343.32141433	-2.34248879	264.0666	53996.5173611111	2006-09-18 12:25:00	53996.8619675926	2006-09-18 20:41:14	401046020	17.134	20	17.342	17.134	17.334	17.334	1	1	1	1	1	0	0	15.4477	15.4477	29.7679	0	PROCESSED	57535.6082175926	2016-05-27 14:35:50	54526	2008-03-01 00:00:00	54020.9055555556	2006-10-12 21:44:00	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011112	We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state.	GALACTIC POINT SOURCES	4	A	ANDREW YOUNG		USA	1	AO1	REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046020/	Quick Look
254	GALACTIC CENTER GC11	266.231	-29.8182	265.431151	-29.797955	266.700372	-6.420209	359.16839231	-0.33075371	109.7993	54172.6536111111	2007-03-13 15:41:12	54173.2086111111	2007-03-14 05:00:24	501056010	26.5374	25	26.5454	26.5454	0	26.5374	2	2	0	2	1	0	0	25.2789	25.2789	47.946	0	PROCESSED	57537.6702199074	2016-05-29 16:05:07	54736	2008-09-27 00:00:00	54182.3328125	2007-03-23 07:59:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501056010/	Quick Look
255	SWIFTJ2000.6+3210	300.0869	32.2033	299.597811	32.064769	312.685822	51.280995	68.99570836	1.1443147	87.4233	53837.6619212963	2006-04-12 15:53:10	53837.9139351852	2006-04-12 21:56:04	401053010	12.4384	20	12.444	12.4512	12.4512	12.4384	1	1	1	1	1	0	0	9.8767	9.8767	21.7679	0	PROCESSED	57533.4456134259	2016-05-25 10:41:41	54775	2008-11-05 00:00:00	53927.3549189815	2006-07-11 08:31:05	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011132	INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	1	AO1	HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401053010/	Quick Look
256	ABELL 2199 CENTER	247.1922	39.484	246.76294	39.592842	233.179095	60.039777	62.84241749	43.66620611	252.3681	54009.2972222222	2006-10-01 07:08:00	54009.8967361111	2006-10-01 21:31:18	801056010	24.9282	25	25.4799	24.9282	25.4799	25.4799	2	2	2	2	1	0	0	20.519	20.519	51.7939	1	PROCESSED	57535.7247453704	2016-05-27 17:23:38	54735	2008-09-26 00:00:00	54021.2246990741	2006-10-13 05:23:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010138	Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	1	AO1	PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801056010/	Quick Look
257	GC SGR D NORTH	266.9758	-27.7178	266.189062	-27.7012	267.305981	-4.305004	1.30220378	0.20283685	108.7992	54173.2100578704	2007-03-14 05:02:29	54174.7883564815	2007-03-15 18:55:14	501058010	63.2422	63	63.2502	63.2422	0	63.2582	2	2	0	2	1	0	0	51.1479	51.1479	136.3519	0	PROCESSED	57537.7302546296	2016-05-29 17:31:34	54735	2008-09-26 00:00:00	54182.440462963	2007-03-23 10:34:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501058010/	Quick Look
258	A3667_NW_17OFF	302.8177	-56.56	301.819585	-56.708877	291.523842	-35.547493	341.18808838	-33.22347241	74.1682	53861.293912037	2006-05-06 07:03:14	53861.7356944444	2006-05-06 17:39:24	801095010	17.2586	20	17.2826	17.2746	17.2666	17.2586	1	1	1	1	1	0	0	14.2555	14.2555	38.1519	1	PROCESSED	57533.636099537	2016-05-25 15:15:59	54735	2008-09-26 00:00:00	53913.7593518518	2006-06-27 18:13:28	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	013080	We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA	CRAIG SARAZIN	JUS	1	AO1	SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801095010/	Quick Look
259	RXJ1713-3946	257.9704	-39.5791	257.105134	-39.519003	260.343852	-16.539668	347.29183097	-0.10508063	267.9995	53989.172025463	2006-09-11 04:07:43	53989.5306365741	2006-09-11 12:44:07	501063010	18.422	20	18.422	18.422	18.422	18.422	2	2	2	2	1	0	0	17.7597	17.7597	30.9719	1	PROCESSED	57535.5249537037	2016-05-27 12:35:56	54526	2008-03-01 00:00:00	54021.1086458333	2006-10-13 02:36:27	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501063010/	Quick Look
260	CYGNUS_LOOP_P12	313.7421	31.2725	313.223564	31.080937	328.639569	46.215284	74.99964096	-8.84356964	62.1405	53864.7943055556	2006-05-09 19:03:48	53865.1391087963	2006-05-10 03:20:19	501029010	13.5426	10	13.5426	13.5426	13.5426	13.5426	2	2	2	2	1	0	0	2.1567	2.1567	29.78	1	PROCESSED	57534.2604166667	2016-05-26 06:15:00	54394	2007-10-21 00:00:00	53914.0447916667	2006-06-28 01:04:30	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501029010/	Quick Look
261	3EGJ1234 1318_1	188.0173	-13.3363	187.367898	-13.060386	192.646727	-9.069223	295.70141073	49.26333697	109.7313	54081.3723032407	2006-12-12 08:56:07	54081.9273032407	2006-12-12 22:15:19	801031010	19.4098	20	19.4178	19.4178	0	19.4098	2	2	0	2	1	0	0	18.7228	18.7228	47.9499	1	PROCESSED	57536.3099768518	2016-05-28 07:26:22	54735	2008-09-26 00:00:00	54094.2359722222	2006-12-25 05:39:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010068	We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ?sim 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TOMONORI TOTANI		JAP	1	AO1	CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801031010/	Quick Look
262	3EGJ1234 1318_2	188.017	-13.0869	187.367769	-12.810986	192.545784	-8.84065	295.65674578	49.51103665	109.9322	54081.9277777778	2006-12-12 22:16:00	54082.7766087963	2006-12-13 18:38:19	801032010	30.9427	30	30.9667	30.9587	0	30.9427	2	2	0	2	1	0	0	26.083	26.083	73.3339	1	PROCESSED	57536.3393055556	2016-05-28 08:08:36	54735	2008-09-26 00:00:00	54094.2665740741	2006-12-25 06:23:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010068	We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ?sim 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TOMONORI TOTANI		JAP	1	AO1	CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801032010/	Quick Look
263	A3667_NW_17OFF	302.869	-56.6666	301.869632	-56.815685	291.522519	-35.657764	341.06051648	-33.2513141	258.9342	54038.8325578704	2006-10-30 19:58:53	54039.0106944444	2006-10-31 00:15:24	801095020	11.9634	10	11.9794	11.9794	11.9634	11.9714	1	1	1	1	1	0	0	8.724	8.724	15.3839	0	PROCESSED	57535.9848032407	2016-05-27 23:38:07	54735	2008-09-26 00:00:00	54056.1858796296	2006-11-17 04:27:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	013080	We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA	CRAIG SARAZIN	JUS	1	AO1	SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801095020/	Quick Look
264	SNR 0509-67.5	77.3855	-67.5341	77.403087	-67.594899	342.98809	-84.999306	278.15788525	-34.58671131	68.6442	53965.2623032407	2006-08-18 06:17:43	53966.1640509259	2006-08-19 03:56:14	501041010	51.2762	50	51.2762	51.2762	51.2762	51.2762	2	2	2	2	1	0	0	50.8294	50.8294	77.89	1	PROCESSED	57535.3081365741	2016-05-27 07:23:43	54526	2008-03-01 00:00:00	54020.7617592593	2006-10-12 18:16:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010072	Hot plasma in young supernova remnants (SNRs) are generally in the state of non-equilibrium ionization (NEI), hence strong L-shell lines of Si, Fe and other elements appear in soft energy band (<1keV). With the observations with Chandra and XMM, quite large ambiguity of ionization age for each element remains because of the limited energy resolution in the soft energy band. Utilizing the supreme energy resolution and background property of Suzaku/XIS, we propose the observation of the youngest type Ia SNR in the LMC, 0509-67.5. We correctly diagnose the NEI plasma of this SNR by determining the ionization age and electron temperature for each element component and constrain the ejecta structure of Type Ia SNR.	GALACTIC DIFFUSE EMISSION	5	C	HIROSHI NAKAJIMA		JAP	1	AO1	NEI PLASMA DIAGNOSTICS OF A YOUNG TYPE IA SNR:0509-67.5	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501041010/	Quick Look
265	GALACTIC CENTER	265.9791	-28.902	265.18515	-28.880549	266.454701	-5.510331	359.8343278	0.33569605	108.8002	54169.6271990741	2007-03-10 15:03:10	54170.1633564815	2007-03-11 03:55:14	501046010	25.211	25	25.227	25.211	0	25.243	2	2	0	2	1	0	0	25.0087	25.0087	46.2919	0	PROCESSED	57537.6350925926	2016-05-29 15:14:32	54736	2008-09-27 00:00:00	54179.4773842593	2007-03-20 11:27:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501046010/	Quick Look
266	GALACTIC CENTER	265.7083	-29.9322	264.907837	-29.909421	266.247634	-6.546909	358.83372455	-0.00453222	269.0002	54017.5695486111	2006-10-09 13:40:09	54018.2808333333	2006-10-10 06:44:24	501051010	21.869	20	21.877	21.877	21.869	21.877	2	2	2	2	1	0	0	21.1322	21.1322	61.4459	0	PROCESSED	57535.8166435185	2016-05-27 19:35:58	54735	2008-09-26 00:00:00	54053.5109953704	2006-11-14 12:15:50	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501051010/	Quick Look
267	RXJ1713-3946	258.5534	-39.7289	257.686429	-39.671569	260.823727	-16.651038	347.43430559	-0.55631777	267.9997	53991.0497337963	2006-09-13 01:11:37	53991.4460300926	2006-09-13 10:42:17	501068010	21.0015	20	21.0175	21.0095	21.0015	21.0255	2	2	2	2	1	0	0	21.2093	21.2093	34.2339	1	PROCESSED	57535.5599537037	2016-05-27 13:26:20	54526	2008-03-01 00:00:00	54021.2424537037	2006-10-13 05:49:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501068010/	Quick Look
268	A3667_NW_RELIC	302.5617	-56.3599	301.565299	-56.507728	291.421165	-35.317169	341.42703548	-33.08195751	74.7123	53858.7409837963	2006-05-03 17:47:01	53861.2933449074	2006-05-06 07:02:25	801094010	94.3946	95	94.4026	94.3946	94.3946	94.4026	3	3	3	3	1	0	0	56.2506	56.2506	220.489	4	PROCESSED	57533.7274074074	2016-05-25 17:27:28	54394	2007-10-21 00:00:00	53913.7574189815	2006-06-27 18:10:41	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	013080	We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA	CRAIG SARAZIN	JUS	1	AO1	SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801094010/	Quick Look
269	LMC X-3 OFF FIELD 1	85.5783	-64.5441	85.521216	-64.565729	45.792643	-87.283954	274.09377866	-31.6918405	324.0002	53847.1442361111	2006-04-22 03:27:42	53848.0099421296	2006-04-23 00:14:19	501097010	43.6067	50	43.6067	43.6067	43.6067	43.6067	2	2	2	2	1	0	0	42.0261	42.0261	74.7459	0	PROCESSED	57533.5339583333	2016-05-25 12:48:54	54526	2008-03-01 00:00:00	53907.3335763889	2006-06-21 08:00:21	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011256	The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona.	GALACTIC DIFFUSE EMISSION	5	A	Q. DANIEL WANG		USA	1	AO1	A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501097010/	Quick Look
270	MRK 1073	48.7401	42.0969	47.912237	41.911835	57.846592	23.153427	149.47083071	-13.26071681	81.0781	53949.235162037	2006-08-02 05:38:38	53949.3834722222	2006-08-02 09:12:12	701007010	3.4746	40	3.4746	3.4806	3.4786	3.4766	1	1	1	1	1	0	0	4.1358	4.1358	12.806	0	PROCESSED	57535.0684375	2016-05-27 01:38:33	54735	2008-09-26 00:00:00	54132.9684490741	2007-02-01 23:14:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010037	We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	1	AO1	COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701007010/	Quick Look
271	AWM7 EAST OFFSET	44.0318	41.5949	43.221288	41.393422	54.035202	23.723269	146.61375919	-15.47239178	90.4995	53952.2676967593	2006-08-05 06:25:29	53953.2398611111	2006-08-06 05:45:24	801036010	38.5361	40	38.5361	38.5361	38.5361	38.5361	1	1	1	1	1	0	0	37.541	37.541	83.9599	0	PROCESSED	57535.0870138889	2016-05-27 02:05:18	54394	2007-10-21 00:00:00	54020.7498726852	2006-10-12 17:59:49	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010076	The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	TAKAYA OHASHI		JAP	1	AO1	SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801036010/	Quick Look
272	MRK421	166.0521	38.1644	165.357194	38.434126	151.189395	29.439264	179.96763761	64.99940635	318.3733	53853.2821412037	2006-04-28 06:46:17	53854.2711226852	2006-04-29 06:30:25	701024010	41.4709	40	41.4789	41.4709	41.4789	41.4789	2	2	2	2	1	0	0	34.7033	34.7033	85.4301	1	PROCESSED	57533.6140162037	2016-05-25 14:44:11	54394	2007-10-21 00:00:00	53908.0343055556	2006-06-22 00:49:24	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010157	We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV)	EXTRAGALACTIC COMPACT SOURCES	7	A	TADAYUKI TAKAHASHI		JAP	1	AO1	SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701024010/	Quick Look
273	NGC 5506	213.312	-3.2124	212.663098	-2.97888	212.190832	9.596053	339.14600253	53.80603682	287.3743	53955.6875578704	2006-08-08 16:30:05	53957.003900463	2006-08-10 00:05:37	701030010	47.7531	150	47.7531	47.7531	47.7531	47.7531	2	2	2	2	1	0	0	41.0973	41.0973	113.7259	2	PROCESSED	57535.2578587963	2016-05-27 06:11:19	54695	2008-08-17 00:00:00	54116.2715740741	2007-01-16 06:31:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011312	NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	A	TRACEY TURNER		USA	1	AO1	SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030010/	Quick Look
274	IRAS08572+3915	135.0664	39.0091	134.264876	39.204772	126.11779	21.048672	183.47368885	40.96543811	300.022	53839.0903240741	2006-04-14 02:10:04	53840.7752199074	2006-04-15 18:36:19	701053010	77.1974	75	77.2214	77.1974	77.2134	77.2214	2	2	2	2	1	0	0	62.3339	62.3339	145.4999	9	PROCESSED	57533.486875	2016-05-25 11:41:06	54401	2007-10-28 00:00:00	53906.2114699074	2006-06-20 05:04:31	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011344	Ultraluminous infrared galaxies (ULIRGs) produce the energy outputs of quasars with nearly all the power emerging in the far-IR via reprocessing of optical, UV, and X-ray radiation by dust. The ultimate nuclear power source, be it AGN or compact starburst, of ULIRGs has been the focus of much debate since their discovery with the IRAS mission. While observations with Spitzer are unlocking the secrets of many nearby ULIRGs, some have nuclei that are apparently so obscured as to be optically thick even in the mid-IR. We have chosen three local ULIRGs, IRAS 08572+3915, IRAS15250+3609, and IRAS20551-4250 that are IR-bright, yet highly obscured for deep Suzaku observations to search for the tell-tale signs of a buried AGN: hard X-ray emission behind significant column densities of HI gas.	EXTRAGALACTIC COMPACT SOURCES	7	A	SARAH GALLAGHER		USA	1	AO1	ULTRAHARD X-RAY CASE STUDIES OF ULIRGS WITH DEEP SILICATE ABSORPTION	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701053010/	Quick Look
275	MKN 841	225.9811	10.3761	225.377197	10.570593	220.178092	26.525473	11.09749436	54.61837916	292.433	54304.6970949074	2007-07-23 16:43:49	54306.218912037	2007-07-25 05:15:14	701084020	50.9253	50	50.9253	50.9333	0	50.9333	2	2	0	2	1	0	0	47.6556	47.6556	131.4738	2	PROCESSED	57539.3432060185	2016-05-31 08:14:13	54800	2008-11-30 00:00:00	54339.5240277778	2007-08-27 12:34:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012028	We propose to perform two 50 ks Suzaku observations of Mkn 841, at an interval of a few months, in order to elucidate the origin of its different X-ray components. Strong soft excess and complex iron line profile are known to be present in this source and recent XMM observations reveal their extreme and puzzling spectral and temporal behaviors. Nevertheless, while the XMM observations help to better constrain their natures, their physical interpretation strongly suffer from the lack of data above 10 keV. Two dedicated Suzaku observations will provide crucial information for our understanding of these components, allowing 1) to obtain high S/N and striclty simultaneous broad band X-ray spectra from the soft X-ray up to the reflection bump and 2) to study their spectral variability behaviors	EXTRAGALACTIC COMPACT SOURCES	7	B	PIERRE-OLIVIER PETRUCCI		EUR	1	AO1	PROBING THE ORIGIN OF THE STRONG SOFT EXCESS AND PUZZLING REFLECTION COMPONENTS IN MKN 841	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701084020/	Quick Look
276	A2104E	235.1486	-3.297	234.495076	-3.136609	233.617797	15.850396	2.9252225	39.1285511	117.6908	54118.1261226852	2007-01-18 03:01:37	54118.6850231482	2007-01-18 16:26:26	801003010	22.7847	20	22.7847	22.7847	0	22.7847	2	2	0	2	1	0	0	17.7352	17.7352	48.2879	1	PROCESSED	57536.8549189815	2016-05-28 20:31:05	54735	2008-09-26 00:00:00	54132.8631365741	2007-02-01 20:42:55	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010012	We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO HATTORI		JAP	1	AO1	TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801003010/	Quick Look
277	A399/401 FILAMENT	44.7475	13.2485	44.061375	13.049612	46.15841	-3.573964	164.45015039	-39.12843885	74.1756	53966.1736921296	2006-08-19 04:10:07	53969.4641666667	2006-08-22 11:08:24	801020010	151.0601	150	151.0601	151.0681	151.0681	151.0681	2	2	2	2	1	0	0	142.2036	142.2036	284.2738	5	PROCESSED	57535.3984837963	2016-05-27 09:33:49	54526	2008-03-01 00:00:00	54021.1056944444	2006-10-13 02:32:12	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010063	Although warm-hot intergalactic medium (WHIM) is supposed to account for most of the baryon in the Universe, its detection is extremely difficult. Here, we propose to observe the cosmological filament between clusters A399 and A401 with Suzaku. We try to detect the OVII emission line and confirm the existence of WHIM in the filament. We expect that the density of the WHIM in the filament is high, and that the detection will be easier than that in other regions in the Universe. Moreover, since the redshift of the filament is relatively high, we can discriminate between the OVII mission from the WHIM and that from our Galaxy by studying the redshift of the line.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YUTAKA FUJITA		JAP	1	AO1	THE DETECTION OF WHIM IN THE A399/401 FILAMENT	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801020010/	Quick Look
278	ABELL 2204	248.0963	5.6404	247.481247	5.74563	245.314616	27.222606	21.10023438	33.35451369	261.3606	53995.3098958333	2006-09-17 07:26:15	53996.5098958333	2006-09-18 12:14:15	801091010	49.1113	55	49.1113	49.1113	49.1113	49.1113	2	2	2	2	1	0	0	51.9372	51.9372	103.6439	1	PROCESSED	57535.6038194444	2016-05-27 14:29:30	54526	2008-03-01 00:00:00	54020.8840277778	2006-10-12 21:13:00	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012018	Measurements of the intracluster gas temperatures out to large radii, where most of the cluster mass resides, are of the utmost importance for the use of clusters in precision cosmology and for studies of cluster physics. Previous attempts to measure temperatures at the cluster virial radius have failed. Here we show that such measurements appear feasible now for the first time with the Suzaku X-ray CCDs. Furthermore, we show that A2204 and A2163 are optimal targets for such an investigation. We, therefore, propose to observe A2204 for 55 ks and A2163 for 100 ks to measure the gas temperature to 10% and 15% accuracy (1-sigma), respectively, out to the cluster virial radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	THOMAS REIPRICH		EUR	1	AO1	A2204 AND A2163: GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801091010/	Quick Look
279	THE CRAB OFFSETS	83.6331	21.9589	82.881145	21.926215	84.096743	-1.351596	184.60466298	-5.81410844	87.5062	53996.8758680556	2006-09-18 21:01:15	53996.9515509259	2006-09-18 22:50:14	101011060	3.368	2	3.368	3.368	3.368	3.368	1	1	1	1	1	0	0	2.716	2.716	6.5279	0	PROCESSED	57535.6113888889	2016-05-27 14:40:24	53826	2006-04-01 00:00:00	54104.4231481482	2007-01-04 10:09:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	015015	We propose observing multiple offset pointings of the Crab nebula.	CALIBRATION	1	A	YOSHITOMO MAEDA		JAP	1	AO1	CRAB OFFSET POINTINGS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011060/	Quick Look
280	SGR1900+14	286.803	9.3875	286.206177	9.3084	289.573902	31.693472	43.07594962	0.80149907	86.5533	53826.3631597222	2006-04-01 08:42:57	53826.9113310185	2006-04-01 21:52:19	401022010	17.0562	20	17.7046	21.7074	21.6555	17.0562	1	2	1	1	1	0	0	14.3604	14.3604	47.336	1	PROCESSED	57533.34875	2016-05-25 08:22:12	54394	2007-10-21 00:00:00	53906.0977893518	2006-06-20 02:20:49	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010124	We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs.	GALACTIC POINT SOURCES	4	A	YUJIN NAKAGAWA		JAP	1	AO1-TOO	PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR"	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401022010/	Quick Look
281	CYGNUS X-2	326.1653	38.3323	325.647427	38.10178	346.69525	47.972917	87.3318132	-11.3049847	76.3142	53871.8636805556	2006-05-16 20:43:42	53872.7293171296	2006-05-17 17:30:13	401049010	39.3903	37	39.3903	39.4063	39.3903	39.3903	2	1	2	2	1	0	0	36.8804	36.8804	74.786	1	PROCESSED	57534.3858217593	2016-05-26 09:15:35	54401	2007-10-28 00:00:00	53927.6429166667	2006-07-11 15:25:48	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011113	The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme.	GALACTIC POINT SOURCES	4	B	JON MILLER		USA	1	AO1	A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401049010/	Quick Look
282	1E 1841-045	280.3141	-4.8735	279.649841	-4.921767	280.812771	18.180712	27.4352849	0.03686802	77.3227	53844.4525462963	2006-04-19 10:51:40	53847.1328009259	2006-04-22 03:11:14	401100010	97.9622	100	97.9622	97.9702	97.9709	97.9709	2	2	2	2	1	0	0	63.474	63.474	231.5399	2	PROCESSED	57533.5748032407	2016-05-25 13:47:43	54401	2007-10-28 00:00:00	53907.2806597222	2006-06-21 06:44:09	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014204	Anomalous X-ray Pulsars are young radio-quiet pulsars with unconventional properties challenging conventional wisdom on neutron star formation and evolution. Their slow rotation periods, unprecedented for their apparent youth, point to enormous surface magnetic fields, a thousand times stronger than the typical inferred radio-pulsar field. The origin of the X-ray emission from these pulsars is still being debated. The recent discovery of a hard nonthermal pulsed X-ray emission from 1E 1841-045 with RXTE well beyond 10keV, can probably be explain by a magnetospheric origin and should extend above 100keV. The HXD onboard Suzaku gives us a unique opportunity to characterize the high-energy part of the emission with the added advantage to use the XIS to characterize the lower energy data.	GALACTIC POINT SOURCES	4	A	ILANA HARRUS	MIKIO NORII	USJ	1	AO1	SUZAKU OBSERVATIONS OF THE ANOMALOUS X-RAY PULSAR 1E~1841-045 IN THE SNR KES 73	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401100010/	Quick Look
283	SDSSJ084234.9+362503	130.6534	36.3531	129.855939	36.532969	123.380084	17.503637	186.36195466	37.19411123	266.2333	53868.6856018518	2006-05-13 16:27:16	53871.41625	2006-05-16 09:59:24	701004010	109.9556	120	109.9716	109.9636	109.9556	109.9636	2	2	2	2	1	0	0	127.2306	127.2306	235.8948	1	PROCESSED	57534.3648032407	2016-05-26 08:45:19	54400	2007-10-27 00:00:00	53920.287650463	2006-07-04 06:54:13	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010036	Type 2 QSOs are one of the key class to understand the structure and evolution of AGN, origin of the Cosmic X-ray background, and the history of black hole growth. We propose to measure a hard X-ray spectrum of the most luminous and brightest type 2 QSO candidate in the Sloan Digital Sky Survey. The selection by optical narrow line spectra is not biased toward Compton-thin AGNs and enables us to investigate the true nature of type 2 QSOs. The data will be used to measure the absorption column density, intrinsic luminosity, and to constrain the structure of the absorber.	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	1	AO1	THE MOST LUMINOUS TYPE 2 QSO IN SDSS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701004010/	Quick Look
284	RXJ1713-3946	258.942	-39.4278	258.077115	-39.372323	261.109643	-16.326699	347.8535904	-0.62405701	268.0013	53998.4433912037	2006-09-20 10:38:29	53998.8467476852	2006-09-20 20:19:19	501071010	21.1741	20	21.1741	21.1981	21.1901	21.1821	1	1	1	1	1	0	0	18.3387	18.3387	34.8399	0	PROCESSED	57535.634537037	2016-05-27 15:13:44	54526	2008-03-01 00:00:00	54020.8878009259	2006-10-12 21:18:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010158	We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR.	GALACTIC DIFFUSE EMISSION	5	A	TADAYUKI TAKAHASHI		JAP	1	AO1	HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501071010/	Quick Look
285	M81	148.8559	68.9951	147.832512	69.232018	119.540473	51.512284	142.17660014	40.93097712	281.1688	53863.0052083333	2006-05-08 00:07:30	53864.5209953704	2006-05-09 12:30:14	701022010	103.5186	100	103.5266	103.5266	103.5266	103.5186	2	2	2	2	1	0	0	70.7369	70.7369	130.9421	0	PROCESSED	57534.2973726852	2016-05-26 07:08:13	54397	2007-10-24 00:00:00	53913.9816550926	2006-06-27 23:33:35	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010151	We propose observations of the nearby Low Luminosity AGN, M81 and M106, for 100 ks for each target. We aim to detect both targets up to ~200 keV for the first time. We will determine the photon indices of the hard X-ray power-law continuum, with searching for other possible characteristics such as Compton hump around 10-20 keV and cutoff around 100-200 keV which would lead major discoveries. We will study the shape of Fe-K line(s) around 6-7 keV and their time variances. Our goal is to compare their hard X-ray spectra with those of SWG seyfert galaxies, with unprecedented accuracy, to study the accresion mechanism of LLAGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	TAKESHI ITOH		JAP	1	AO1	OBSERVATIONS OF HARD X-RAYS FROM LOW LUMINOSITY ACTIVE GALACTIC NUCLEI	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701022010/	Quick Look
286	SWIFT J0350.1-5019	57.5315	-50.3337	57.174394	-50.483946	28.735241	-67.001155	259.74491819	-49.02538792	320.5309	53838.5046875	2006-04-13 12:06:45	53838.6752199074	2006-04-13 16:12:19	701017010	2.6998	20	2.7158	2.7158	2.6998	2.7078	2	2	2	2	1	0	0	1.1771	1.1771	9.165	0	PROCESSED	57533.4464930556	2016-05-25 10:42:57	54750	2008-10-11 00:00:00	53905.4679398148	2006-06-19 11:13:50	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010133	Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background".	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	1	AO1	DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017010/	Quick Look
287	GALACTIC CENTER GC2	265.779	-29.1853	264.9833	-29.162875	266.287161	-5.798531	359.50136289	0.33591697	108.7998	54170.1638773148	2007-03-11 03:55:59	54170.7946064815	2007-03-11 19:04:14	501047010	25.599	25	25.607	25.599	0	25.623	1	1	0	1	1	0	0	19.0886	19.0886	54.4799	0	PROCESSED	57537.6398611111	2016-05-29 15:21:24	54736	2008-09-27 00:00:00	54182.2693865741	2007-03-23 06:27:55	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010074	We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA	MOTOHIDE KOKUBUN	JAP	1	AO1	MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501047010/	Quick Look
288	LMC X-3 OFF FIELD 1	85.5246	-64.555	85.467763	-64.576889	45.273362	-87.277293	274.10794908	-31.71433471	145.4977	54039.3159722222	2006-10-31 07:35:00	54039.7509722222	2006-10-31 18:01:24	501097020	15.3749	10	15.3749	15.3829	15.3829	15.3829	2	2	2	2	1	0	0	14.9263	14.9263	37.58	0	PROCESSED	57536.0002314815	2016-05-28 00:00:20	54526	2008-03-01 00:00:00	54088.8072222222	2006-12-19 19:22:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011256	The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona.	GALACTIC DIFFUSE EMISSION	5	A	Q. DANIEL WANG		USA	1	AO1	A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501097020/	Quick Look
289	Z348	16.7077	1.0407	16.065796	0.773597	15.79467	-5.606239	131.03941429	-61.58850223	247.9196	54110.9286689815	2007-01-10 22:17:17	54111.5259722222	2007-01-11 12:37:24	801050010	22.6477	23	22.6477	22.6477	0	22.6477	2	2	0	2	1	0	0	21.3403	21.3403	51.589	1	PROCESSED	57536.8362384259	2016-05-28 20:04:11	54735	2008-09-26 00:00:00	54133.0321643518	2007-02-02 00:46:19	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010098	We propose to carry out the Suzaku/XIS observations of 4 massive clusters at low redshifts (z <0.3). Combining the X-ray data with the existing Subaru datasets that allow us to directly reconstruct the mass distribution from the gravitational lensing measurements, we will investigate the physical relations between the mass and gas distributions to understand the nature of cluster in a quantitative way.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	TOSHIFUMI FUTAMASE		JAP	1	AO1	THE ULTIMATE GRAVITATIONAL LENSING STUDY OF GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801050010/	Quick Look
290	A2104S	235.0317	-3.4139	234.377731	-3.253044	233.528717	15.709214	2.71321412	39.14413145	117.9978	54120.3324884259	2007-01-20 07:58:47	54120.8266087963	2007-01-20 19:50:19	801004010	17.3234	20	17.3234	17.3234	0	17.3234	2	2	0	2	1	0	0	13.8291	13.8291	42.6819	1	PROCESSED	57536.8854166667	2016-05-28 21:15:00	54750	2008-10-11 00:00:00	54137.3891898148	2007-02-06 09:20:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010012	We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MAKOTO HATTORI		JAP	1	AO1	TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801004010/	Quick Look
291	IIZW108	318.5228	2.5728	317.890055	2.365228	321.781705	17.722745	53.56011975	-29.86052353	77.7227	53864.5319791667	2006-05-09 12:46:03	53864.7883680556	2006-05-09 18:55:15	801075010	11.6052	11	11.6052	11.6052	11.6052	11.6052	2	2	2	2	1	0	0	9.632	9.632	22.1499	1	PROCESSED	57534.2579398148	2016-05-26 06:11:26	54401	2007-10-28 00:00:00	53913.9958564815	2006-06-27 23:54:02	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801075010/	Quick Look
292	4U1700-37	255.9894	-37.8441	255.139416	-37.774677	258.577099	-14.956185	347.75582102	2.17172645	269.6945	53991.447662037	2006-09-13 10:44:38	53992.918912037	2006-09-14 22:03:14	401058010	81.4425	80	81.4569	81.4704	81.4425	81.4544	3	3	3	3	1	0	0	82.1093	82.1093	127.109	1	PROCESSED	57535.6097916667	2016-05-27 14:38:06	54526	2008-03-01 00:00:00	54053.5428240741	2006-11-14 13:01:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011135	The compact object in the massive X-ray binary 4U1700-37/HD153919 has been inferred to be a neutron star based on its spectral shape, but no pulsations have been observed. One possible explanation for the absence of observed pulsations is that the pulsed signal is beamed in directions other than our line of sight. This can be tested using Suzaku by searching for pulsations in the iron K line. This line is formed efficiently under almost all conditions of ionization and temperature, and so represents an X-ray bolometer which should respond to pulsed X-rays no matter where they are pointed. We plan to make such a search, and to probe the other properties of the wind and compact object in this system by observing with Suzaku for 80 ks away from eclipse.	GALACTIC POINT SOURCES	4	A	TIMOTHY KALLMAN		USA	1	AO1	IRON LINE VARIABILITY IN 4U1700-37	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401058010/	Quick Look
293	ALGOL	47.0831	40.8965	46.267674	40.705521	56.181748	22.363141	149.0355551	-14.93487401	244.4771	54167.6197222222	2007-03-08 14:52:24	54169.6132986111	2007-03-10 14:43:09	401093010	102.1642	105	102.1642	102.1642	0	102.1642	2	2	0	2	1	0	0	102.4729	102.4729	172.1928	1	PROCESSED	57537.6825810185	2016-05-29 16:22:55	54736	2008-09-27 00:00:00	54186.3983564815	2007-03-27 09:33:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012024	Stellar and solar coronae reveal high-energy phenomena including the presence of accelerated electrons, explosive dissipation of magnetic energy, and heating to extreme temperatures. Many of these processes are likely to be physically related. We propose to use Suzaku's suite of instruments to observe the interplay between thermal and non-thermal high-energy processes in the active, eclipsing binary Algol. Our prime objective is the observation of hard X-rays above 10 keV, but also the appearance of an Fe fluorescence line that could be induced either by irradiation from flaring plasma or by electron beams. These models can be distinguished by correlating the emission with nonthermal hard X-rays as possibly detected by the HXD.	GALACTIC POINT SOURCES	4	C	MANUEL GUEDEL		EUR	1	AO1	A SYNOPTIC VIEW OF HIGH-ENERGY PHENOMENA IN THE CORONA OF ALGOL	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401093010/	Quick Look
294	SERPENS X-1	279.9934	5.0285	279.376671	4.981655	281.288405	28.078275	36.11311789	4.83561165	256.1423	54032.2853819444	2006-10-24 06:50:57	54033.2259143518	2006-10-25 05:25:19	401048010	37.1578	37	37.1578	37.2698	37.2058	37.1658	2	1	2	2	1	0	0	31.0695	31.0695	81.2399	2	PROCESSED	57535.9734722222	2016-05-27 23:21:48	54526	2008-03-01 00:00:00	54056.4719328704	2006-11-17 11:19:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011113	The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme.	GALACTIC POINT SOURCES	4	B	JON MILLER		USA	1	AO1	A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401048010/	Quick Look
295	4U 1636-536	250.2273	-53.7542	249.230886	-53.657708	256.461437	-31.236858	332.91122007	-4.81806999	91.2447	54153.2955787037	2007-02-22 07:05:38	54154.3544560185	2007-02-23 08:30:25	401050020	40.096	38	40.096	40.104	0	40.096	2	1	0	2	1	0	0	35.55	35.55	91.4779	0	PROCESSED	57537.4821990741	2016-05-29 11:34:22	54525	2008-02-29 00:00:00	54158.392037037	2007-02-27 09:24:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011117	Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.	GALACTIC POINT SOURCES	4	A	JEROEN HOMAN		USA	1	AO1	THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050020/	Quick Look
296	IGRJ16493-4348	252.3173	-43.8652	251.422595	-43.77854	256.400238	-21.254215	341.31911758	0.57823277	287.444	54013.8822916667	2006-10-05 21:10:30	54014.4204166667	2006-10-06 10:05:24	401054010	21.1998	20	21.2158	21.2158	21.1998	21.2078	3	3	3	3	1	0	0	20.2197	20.2197	46.4639	1	PROCESSED	57535.7818634259	2016-05-27 18:45:53	54695	2008-08-17 00:00:00	54025.4796412037	2006-10-17 11:30:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011132	INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	1	AO1	HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401054010/	Quick Look
297	SGR 1806-20	272.166	-20.4729	271.421316	-20.481616	272.022208	2.952663	9.94279657	-0.27364584	269.9473	53987.9261921296	2006-09-09 22:13:43	53989.1668287037	2006-09-11 04:00:14	401092010	48.9155	50	48.9155	48.9235	48.9315	48.9315	1	1	1	1	1	0	0	55.4085	55.4085	107.1759	1	PROCESSED	57535.5272453704	2016-05-27 12:39:14	54526	2008-03-01 00:00:00	54021.1112615741	2006-10-13 02:40:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012017	The soft gamma-ray repeater SGR 1806-20 has recently emitted the most powerful giant flare ever observed from these sources. This probably involved a large scale restructuring of the magnetosphere, leading to observable variations in the properties of its persistent emission, from IR to hard X-rays. We propose to observe SGR 1806-20 with Suzaku considering the unique opportunity offered by this satellite to study the spectrum of this source simultaneously both in the soft and hard X-ray bands. We also suggest to coordinate this observation with a simultaneous XMM-Newton one, in order to obtain a significantly better determination of the broad band spectral parameters.	GALACTIC POINT SOURCES	4	B	SANDRO MEREGHETTI		EUR	1	AO1	COORDINATED SUZAKU AND XMM-NEWTON OBSERVATIONS OF SGR 1806-20 AFTER THE GIANT FLARE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401092010/	Quick Look
298	RX J1347.5-1145	206.856	-11.8093	206.189594	-11.560184	209.147124	-0.679556	323.97916756	48.76108187	292.056	53916.7756597222	2006-06-30 18:36:57	53918.7600115741	2006-07-02 18:14:25	801013010	69.6611	75	69.6611	69.6611	69.6611	69.6611	2	2	2	2	1	0	0	60.982	60.982	171.3759	0	PROCESSED	57534.8555671296	2016-05-26 20:32:01	54394	2007-10-21 00:00:00	53926.4810300926	2006-07-10 11:32:41	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010014	We propose to obtain broad-band spectra of the most X-ray luminous cluster of galaxies RXJ1347.5-1145 at z=0.45. Our previous high-resolution Sunyaev-Zel'dovich obvervations of this cluster revealed that it exhibits an unusually violent merger activity. Its high X-ray luminosity ensures the unprecedented high-quality spectra with Suzaku. It is indeed a unique target to probe gas physics and particle acceleration mechanism associated with the violent mergers at high redshift. The continuum observations with HXD and XIS as well as the iron line spectroscopy will specify the physical states of both thermal and non-thermal components of the ICM. Combined with the Chandra and our SZ data, the Suzaku data will accomplish the first comprehensive modeling of a violent merger in distant clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	NAOMI OTA		JAP	1	AO1	BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801013010/	Quick Look
299	OPHIUCHUS CLUSTER 5	258.0184	-23.1077	257.261763	-23.048099	258.982957	-0.123527	0.73892155	9.49336651	88.7652	54181.8276736111	2007-03-22 19:51:51	54182.4890277778	2007-03-23 11:44:12	801026010	24.2557	15	24.2557	24.2557	0	24.2557	2	2	0	2	1	0	0	19.2271	19.2271	57.1359	0	PROCESSED	57537.9767013889	2016-05-29 23:26:27	54736	2008-09-27 00:00:00	54186.2070949074	2007-03-27 04:58:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010065	The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUTAKA FUJITA		JAP	1	AO1	PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801026010/	Quick Look
300	M87 CENTER	187.7366	12.4456	187.103964	12.721646	182.061198	14.477269	283.82387862	74.55209055	120.529	54068.9187037037	2006-11-29 22:02:56	54071.1266666667	2006-12-02 03:02:24	801038010	98.1831	100	98.1831	98.1831	0	98.1831	1	1	0	1	1	0	0	88.2503	88.2503	190.7308	2	PROCESSED	57536.2829050926	2016-05-28 06:47:23	54735	2008-09-26 00:00:00	54090.4156134259	2006-12-21 09:58:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010084	The black hole at the center of M87 is one of the most heaviest in the universe. Recently TeV-gamma ray emission from M87 was found. M87 is thus a very strong candidate for an accelerator of ultra-high energy cosmic rays. We aim at the detection of non-thermal hard X-rays from M87 to clarify the mechanism of the particle acceleration. The giant elliptical galaxy M87 is at the center of the Virgo cluster of galaxies, which is the nearest cluster. We can investigate the distribution of various metal elements. We will clarify how the metals, especially oxygen, diffuse to the intracluster space from the galaxy M87.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	HIRONORI MATSUMOTO		JAP	1	AO1	NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801038010/	Quick Look
301	PERSEUS CL OFFSET	49.6445	42.068	48.814215	41.886236	58.537476	22.936041	150.06631202	-12.92163855	65.996	53980.0800925926	2006-09-02 01:55:20	53980.7668287037	2006-09-02 18:24:14	801049010	29.2438	30	29.2559	29.2479	29.2518	29.2438	2	2	2	2	1	0	0	25.6729	25.6729	59.3299	1	PROCESSED	57535.4121296296	2016-05-27 09:53:28	54526	2008-03-01 00:00:00	54021.3135416667	2006-10-13 07:31:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010097	We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	1	AO1	MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049010/	Quick Look
302	PERSEUS CL OFFSET	50.2242	41.1004	49.398659	40.920786	58.698225	21.886134	150.98569591	-13.49005998	65.9967	53981.4552662037	2006-09-03 10:55:35	53982.1418287037	2006-09-04 03:24:14	801049030	32.8396	30	32.8556	32.8476	32.8396	32.8636	1	1	1	1	1	0	0	31.0313	31.0313	59.288	0	PROCESSED	57535.4291087963	2016-05-27 10:17:55	54526	2008-03-01 00:00:00	54020.8372106482	2006-10-12 20:05:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010097	We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	1	AO1	MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049030/	Quick Look
303	ABELL 2199 OFFSET 2	247.3619	39.6495	246.934152	39.757579	233.32636	60.237575	63.07626508	43.54039287	251.2564	54011.5284722222	2006-10-03 12:41:00	54012.1578587963	2006-10-04 03:47:19	801058010	22.7072	25	22.7232	22.7072	22.7232	22.7232	2	2	2	2	1	0	0	20.704	20.704	54.36	0	PROCESSED	57535.7442476852	2016-05-27 17:51:43	54735	2008-09-26 00:00:00	54024.6719907407	2006-10-16 16:07:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010138	Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	1	AO1	PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801058010/	Quick Look
304	M101	210.8841	54.3679	210.442342	54.607302	174.405989	59.838606	101.97854462	59.72940376	150.2959	54062.5790625	2006-11-23 13:53:51	54064.7182175926	2006-11-25 17:14:14	801063010	98.8522	100	98.8762	98.8522	0	98.8762	2	2	0	2	1	0	0	89.6125	89.6125	184.802	2	PROCESSED	57536.2145486111	2016-05-28 05:08:57	54455	2007-12-21 00:00:00	54088.707650463	2006-12-19 16:59:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011402	We wish to obtain a Suzaku spectrum of the diffuse X-ray emission in a typical galactic disk. The spectral resolution obtainable with Chandra/XMM does not allow the decomposition of the spectrum into more than two thermal components. The higher spectral resolution, better soft response, and lower instrumental background of Suzaku will allow the decomposition into at least three thermal components, and will place constraints on the number of thermal components and the distribution of temperatures and emission measures. The more refined fitting allowed by Suzaku spectra will allow a greater understanding of the sources of the X-ray emission. Given the Suzaku spatial resolution and detector size, M101 is the best observable example of a "typical" galactic disk.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	K. KUNTZ		USA	1	AO1	SOFT DIFFUSE X-RAY EMISSION FROM M101	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801063010/	Quick Look
305	SN 1987A	83.9013	-69.2655	83.9928	-69.294887	307.391677	-86.458548	279.69660922	-31.92548266	330.0004	53894.6930555556	2006-06-08 16:38:00	53895.6683449074	2006-06-09 16:02:25	801090010	39.6464	40	39.6464	39.6464	39.6464	39.6464	2	2	2	2	1	0	0	39.2519	39.2519	84.2399	0	PROCESSED	57534.6267592593	2016-05-26 15:02:32	54400	2007-10-27 00:00:00	53928.1346527778	2006-07-12 03:13:54	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012006	In an early Suzaku observation during the SWG time in November 2005 we have already obtained an excellent XIS spectrum. The flux of SN 1987A continues to rise exponentially with an e-folding time of ~800 days. The abundances in the ejecta could be measured with unprecedented accuracy. We confirm that Oxygen and Iron are significantly underabundant with respect to other elements, indicating the formation of dust, maybe even black rust grains (Fe3O4). We propose to monitor the chemical evolution of SN 1987A with Suzaku for 40 ksec in AO-1, where we expect about twice the previous flux. The exponential brightening and the chemical abundance is expected to change, when the full inner ring is engulfed. Simultaneously we can search for a periodic hard signal from the putative pulsar.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	G NTHER HASINGER		EUR	1	AO1	SN 1987A - A RUSTY REMNANT?	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801090010/	Quick Look
306	CXOU J164710.2-455216	251.7964	-45.87	250.884129	-45.780896	256.291708	-23.290157	339.54853507	-0.43200811	286.2915	54001.2911689815	2006-09-23 06:59:17	54002.205775463	2006-09-24 04:56:19	901002010	38.6794	40	38.6874	38.6954	38.6961	38.6794	1	1	1	1	1	0	0	35.0799	35.0799	79.0159	1	PROCESSED	57535.6726851852	2016-05-27 16:08:40	54002	2006-09-24 00:00:00	54026.4631134259	2006-10-18 11:06:53	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	017002	N/A	GALACTIC COMPACT OBJECT	9	A	SWG		JAP	1	TOO	TOO OBSERVATION OF CXOU J164710.2-455216	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/901002010/	Quick Look
307	NGC 5506	213.3095	-3.2029	212.660624	-2.969373	212.1852	9.604154	339.1508826	53.81542712	91.2728	54131.0918055556	2007-01-31 02:12:12	54132.6279513889	2007-02-01 15:04:15	701030030	57.4063	150	57.4143	57.4063	0	57.4143	2	2	0	2	1	0	0	47.7027	47.7027	132.6858	0	PROCESSED	57536.9491666667	2016-05-28 22:46:48	54695	2008-08-17 00:00:00	54139.3642361111	2007-02-08 08:44:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011312	NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	A	TRACEY TURNER		USA	1	AO1	SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030030/	Quick Look
308	CIRCINUS GALAXY	213.2971	-65.3336	212.329588	-65.099539	238.600438	-47.951762	311.32997737	-3.80345965	276.4798	53937.5207986111	2006-07-21 12:29:57	53939.0475	2006-07-23 01:08:24	701036010	108.0217	100	108.0457	108.0217	108.0457	108.0297	2	2	2	2	1	0	0	94.272	94.272	131.8879	1	PROCESSED	57535.0550578704	2016-05-27 01:19:17	54401	2007-10-28 00:00:00	53943.5986574074	2006-07-27 14:22:04	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011331	The light of AGN dominates the hard cosmic X-ray background. However, the contribution of Compton thick objects is poorly constrained because they emit chiefly above the energy range where Chandra and XMM are sensitive. Here we propose to observe the Circinus galaxy, one of the two brightest AGN reflection sources below 10 keV and with a known high column density. Our observations below 10 keV will provide CCD spectra of the rich emission line and continuum spectra, allowing limited photoionization modelling and searches for variability, possibly seen in Circinus. In the range 10 - 60 keV, we shall obtain a spectrum of the directly viewed continuum with unprecedented S/N in the key band for the HCXB. Above 60 keV, we will detect Circinus and check whether the spectrum has a rollover.	EXTRAGALACTIC COMPACT SOURCES	7	B	ANDREW WILSON		USA	1	AO1	THE HARD X-RAY BACKGROUND, COMPTON-THICK AGN AND WATER VAPOR MEGAMASERS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701036010/	Quick Look
309	APM 08279+5255	127.9195	52.7471	126.987464	52.916366	116.240703	32.704357	165.76446097	36.2381521	299.485	54183.9301041667	2007-03-24 22:19:21	54186.4654513889	2007-03-27 11:10:15	701057030	117.1433	125	117.1433	117.1513	0	117.1433	2	2	0	2	1	0	0	110.9324	110.9324	219.0418	3	PROCESSED	57538.0464467593	2016-05-30 01:06:53	54702	2008-08-24 00:00:00	54209.5933680556	2007-04-19 14:14:27	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011353	Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	1	AO1	VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057030/	Quick Look
310	1ES 1553+113	238.8999	11.1305	238.306227	11.275519	233.852477	30.750337	21.81691499	43.96274027	296.7536	53940.6127777778	2006-07-24 14:42:24	53941.8036342593	2006-07-25 19:17:14	701070010	55.6355	55	55.6435	55.6515	55.6515	55.6355	2	2	2	2	1	0	0	53.2015	53.2015	102.8819	0	PROCESSED	57535.0418171296	2016-05-27 01:00:13	54401	2007-10-28 00:00:00	53955.6133680556	2006-08-08 14:43:15	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011376	Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra.	EXTRAGALACTIC COMPACT SOURCES	7	A	ANITA REIMER		USA	1	AO1	CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701070010/	Quick Look
311	1ES 1959+650	299.9645	65.1588	299.84329	65.020024	7.34886	77.791428	98.00607393	17.68746705	45.1602	53878.0509606482	2006-05-23 01:13:23	53880.1718055556	2006-05-25 04:07:24	701075010	98.8622	100	98.8782	98.8622	98.8702	98.8782	2	2	2	2	1	0	0	96.106	96.106	183.2028	2	PROCESSED	57534.4674305556	2016-05-26 11:13:06	54408	2007-11-04 00:00:00	53928.2478472222	2006-07-12 05:56:54	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012002	We request to observe 1ES1959+650 and 1ES2344+514 for 100 ks each with SUZAKU simultaneously with the Whipple Cherenkov telescope. Whipple will extensively monitor these sources for months in 2006-2007. There are three well defined scientific cases that we would like to address. We want to study 1) the correlation between the soft and hard X-ray and TeV fluxes and spectra, extremely variable in these sources, sometimes showing extreme conditions; 2) the mystery of the ''orphan'' flares; i.e. events observed only in the TeV gamma rays without a counterpart in the X-rays: this is currently not understood in the framework of SSC models; 3) the origin of the lag observed between soft and hard X-ray variability in some blazars and the implications for the TeV emission.	EXTRAGALACTIC COMPACT SOURCES	7	A	GIANPIERO TAGLIAFERRI		EUR	1	AO1	JETS ON TEST: SIMULTANEOUS X-RAY AND TEV OBSERVATIONS OF 1ES1959+650 AND 1ES2344+514	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701075010/	Quick Look
312	ABELL 2199 OFFSET 1	247.0269	39.6504	246.598636	39.759978	232.832467	60.158374	63.06766091	43.79825488	251.7923	54009.8973958333	2006-10-01 21:32:15	54010.4467476852	2006-10-02 10:43:19	801057010	24.6315	25	24.6315	24.6315	24.6315	24.6315	2	2	2	2	1	0	0	25.5343	25.5343	47.454	0	PROCESSED	57535.7339814815	2016-05-27 17:36:56	54735	2008-09-26 00:00:00	54021.2449189815	2006-10-13 05:52:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010138	Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	1	AO1	PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801057010/	Quick Look
313	ABELL 2199 OFFSET 3	247.3596	39.3165	246.92934	39.424595	233.528009	59.920137	62.61707687	43.53145251	252.4737	54012.1589351852	2006-10-04 03:48:52	54012.6786921296	2006-10-04 16:17:19	801059010	25.2467	25	25.2467	25.2467	25.2467	25.2467	1	1	1	1	1	0	0	20.505	20.505	44.8879	1	PROCESSED	57535.7507291667	2016-05-27 18:01:03	54735	2008-09-26 00:00:00	54025.4730092593	2006-10-17 11:21:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010138	Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MADOKA KAWAHARADA		JAP	1	AO1	PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801059010/	Quick Look
314	AB DOR	82.2881	-65.4658	82.252574	-65.503277	15.679222	-86.688003	275.31538375	-33.00189818	204.2849	54108.0647569444	2007-01-08 01:33:15	54109.4724421296	2007-01-09 11:20:19	401031020	49.0965	45	49.0965	49.0965	0	49.0965	2	2	0	2	1	0	0	44.9611	44.9611	121.6199	2	PROCESSED	57536.5000578704	2016-05-28 12:00:05	54502	2008-02-06 00:00:00	54133.0127083333	2007-02-02 00:18:18	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011021	We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku.	GALACTIC POINT SOURCES	4	B	MARC AUDARD		USA	1	AO1	NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401031020/	Quick Look
315	1RXS J213344.1+51072	323.4354	51.1973	323.001109	50.974362	356.300054	59.716219	94.50909334	-0.42447705	94.0452	53854.2853009259	2006-04-29 06:50:50	53856.2501736111	2006-05-01 06:00:15	401038010	81.9241	80	81.9241	81.9241	81.9241	81.9241	2	2	2	2	1	0	0	62.8881	62.8881	169.7261	3	PROCESSED	57533.6330671296	2016-05-25 15:11:37	54391	2007-10-18 00:00:00	53908.1887962963	2006-06-22 04:31:52	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011102	Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber.	GALACTIC POINT SOURCES	4	A	KOJI MUKAI		USA	1	AO1	BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401038010/	Quick Look
316	V893 SCO	243.8144	-28.6275	243.038085	-28.502934	247.008203	-7.251726	348.06577336	15.88028883	274.6746	53973.4024189815	2006-08-26 09:39:29	53974.056412037	2006-08-27 01:21:14	401041010	18.4978	20	18.4978	18.4978	18.4978	18.4978	2	2	2	2	1	0	0	16.1403	16.1403	56.482	0	PROCESSED	57535.3695601852	2016-05-27 08:52:10	54526	2008-03-01 00:00:00	54053.4763888889	2006-11-14 11:26:00	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011103	The RXTE All-Sky Slew Survey (XSS) catalog, containing 294 objects detected in the 3-20 keV sky, is of great potential use for a variety of purposes. Included in this catalog are two sources identified with lesser known dwarf novae, V893 Sco and SS Aur. Although these are known to be soft X-ray sources from the ROSAT All-sky Survey, there has never been a pointed observation with an imaging X-ray telescope of either object. Here I propose short Suzaku observations of V893 Sco and SS Aur to check the reliability of XSS fluxes, hence that of the luminosity functions derived from the XSS catalog. In addition, such observations serve as a pilot study to determine if these individual dwarf novae may merit further in-depth X-ray studies.	GALACTIC POINT SOURCES	4	B	KOJI MUKAI		USA	1	AO1	CONFIRMING THE IDENTIFICATION OF RXTE ALL-SKY SLEW SURVEY SOURCES WITH DWARF NOVAE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401041010/	Quick Look
317	4U 1636-536	250.2277	-53.7538	249.23129	-53.65731	256.461636	-31.236425	332.91167841	-4.81798429	93.2445	54186.4802777778	2007-03-27 11:31:36	54187.3043287037	2007-03-28 07:18:14	401050040	32.1304	38	32.1304	32.1384	0	32.1304	2	1	0	2	1	0	0	27.7842	27.7842	71.1779	1	PROCESSED	57538.0141782407	2016-05-30 00:20:25	54695	2008-08-17 00:00:00	54209.541412037	2007-04-19 12:59:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011117	Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.	GALACTIC POINT SOURCES	4	A	JEROEN HOMAN		USA	1	AO1	THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050040/	Quick Look
318	4U 1822-37	276.4461	-37.1042	275.595774	-37.133404	275.279951	-13.781506	356.85149319	-11.29112534	258.4537	54010.4563888889	2006-10-02 10:57:12	54011.5189699074	2006-10-03 12:27:19	401051010	37.7434	40	37.7682	37.7682	37.7434	37.7434	2	2	2	2	1	0	0	33.1785	33.1785	91.8059	0	PROCESSED	57535.7615393518	2016-05-27 18:16:37	54695	2008-08-17 00:00:00	54024.6539814815	2006-10-16 15:41:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011121	We propose a 40 ks observation of the accretion disk corona source 4U 1822-37. Despite repeated observations over the years and even excellent high-resolution data from the Chandra Observatory, the nature and origin of the corona and even the source of the Fe K fluorescence emission remains controversial. The spectral resolution of the XIS and the broad-band coverage provided by the combined XIS and HXD instruments make Suzaku uniquely suited to a definitive measurement. Determining the physical conditions in this source is particularly interesting. Because of its geometry 4U 1822-37 is a link between x-ray binaries and AGN, and an therefore serve as a laboratory for studying accretion processes throughout the universe.	GALACTIC POINT SOURCES	4	B	JEAN COTTAM		USA	1	AO1	ACCRETION PHYSICS IN THE ADC SOURCE 4U 1822-37	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401051010/	Quick Look
319	HESSJ1813-178	273.3946	-17.7704	272.66469	-17.785118	273.238499	5.632147	12.87014503	0.01155473	90.9367	54160.8999768518	2007-03-01 21:35:58	54162.2814699074	2007-03-03 06:45:19	401101010	63.8391	65	63.8471	63.8391	0	63.8471	2	2	0	2	1	0	0	57.7561	57.7561	119.3519	1	PROCESSED	57537.5358449074	2016-05-29 12:51:37	54736	2008-09-27 00:00:00	54167.6346990741	2007-03-08 15:13:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	014214	Radio and X-ray observations towards the VHE gamma-ray source HESS J1813-178, initially dubbed being a dark accelerator , suggested its association with a SNR. However, a recent XMM observation confirmed earlier ASCA findings of an extended, center-filled X-ray source, not resembling the contours of the radio-detected SNR. We propose hard X-ray observations to investigate the alternatively plerionic origin of HESS J1813-178, given the wide spectral coverage possible by XIS/HXD. This will clarify the discrepancy between ASCA and recent INTEGRAL data. Constructing a valid spectral energy distribution will enable us to constrain the age and field strength of the particle accelerator powering the synchrotron emission and accurately model the radiation processes up to VHE energies.	GALACTIC POINT SOURCES	4	B	OLAF REIMER	KEN EBISAWA	USJ	1	AO1	IS THE ASSOCIATION OF HESS J1813-178/SNR G12.8-0.0 CONCEALING ITS TRUE PLERIONIC NATURE?	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401101010/	Quick Look
320	CYGNUS_LOOP_P3	313.0409	31.565	312.525205	31.375918	328.010479	46.721185	74.84662265	-8.19493741	240.0003	54418.4174074074	2007-11-14 10:01:04	54418.9377083333	2007-11-14 22:30:18	501014010	16.7648	12	16.7812	16.7808	0	16.7648	2	2	0	2	1	0	0	14.6962	14.6962	44.9439	0	PROCESSED	57540.5210069445	2016-06-01 12:30:15	54798	2008-11-28 00:00:00	54430.2624884259	2007-11-26 06:17:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501014010/	Quick Look
321	DRACO HVC REGION A	243.9602	60.0594	243.754378	60.182015	196.928393	76.754112	91.20688798	42.38144862	79.8192	53814.6161111111	2006-03-20 14:47:12	53816.0050578704	2006-03-22 00:07:17	501004010	61.1798	60	61.1798	61.1798	61.1798	61.1798	2	2	2	2	1	0	0	61.2301	61.2301	119.9879	2	PROCESSED	57533.2956481482	2016-05-25 07:05:44	54394	2007-10-21 00:00:00	53906.0459722222	2006-06-20 01:06:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010069	High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin.	GALACTIC DIFFUSE EMISSION	5	A	TAKESHI TSURU		JAP	1	AO1	SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE -	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501004010/	Quick Look
322	CAR-D1	162.0244	-59.5887	161.531362	-59.324189	202.52434	-58.576902	287.89332648	-0.36746291	282.973	53891.5567361111	2006-06-05 13:21:42	53892.6343055556	2006-06-06 15:13:24	501099010	76.9074	75	76.924	76.932	76.9314	76.9074	2	2	2	2	1	0	0	64.2576	64.2576	93.0899	0	PROCESSED	57534.5127430556	2016-05-26 12:18:21	54401	2007-10-28 00:00:00	53926.947974537	2006-07-10 22:45:05	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011257	Soft X-ray emission nebulae with kT =0.1-0.8 keV, log Lx =33-35 ergs/s, and the size of 1-1000 pc accompany a number of giant HII region, but the origin is not understood yet. The Carinae Nebula is 10-100 times more luminous than any other giant HII region in our Galaxy in soft X-rays. From an XMM-Newton observation of the eastern tip of the nebula called Car-D1, we found marginal CVI, CV and OVII lines. If it is real, the carbon abundance should be more than >6 solar, and the OVII line requires more than 2-temperature components. To detect those emission lines clearly and address the origin and environment of the diffuse plasma, we propose a Suzaku observation of the Car-D1 region, optimized for the XIS BI chip.	GALACTIC DIFFUSE EMISSION	5	B	KENJI HAMAGUCHI		USA	1	AO1	ORIGIN OF THE DIFFUSE X-RAY EMISSION AROUND THE CARINA NEBULA, A MASSIVE STAR FORMING REGION	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501099010/	Quick Look
323	GALACTIC PLANE 111	347.9369	61.9538	347.407091	61.681886	29.574403	58.088255	111.50111702	1.31488521	81.8498	53892.6499652778	2006-06-06 15:35:57	53893.680775463	2006-06-07 16:20:19	501100010	72.1409	75	72.1649	72.1649	72.1649	72.1409	2	2	2	2	1	0	0	61.025	61.025	89.0349	1	PROCESSED	57534.5221064815	2016-05-26 12:31:50	54401	2007-10-28 00:00:00	53927.3325115741	2006-07-11 07:58:49	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011258	We propose to observe the line of sight towards (l,b)=(111.5,1.3). This line of sight was observed by XMM because the line of sight is particularly simple, allowing the isolation of the spectrum of the Local Hot Bubble (LHB). The XMM observation did not isolate the LHB, but did reveal the existance of a cool (kT~0.18 keV) X-ray emitting component between 200 and 2000 pcs away that was morphologically unidentifiable in the ROSAT All-Sky Survey. This component may represent the gas responsible for the 3/4 keV "infill problem", and may represent a previously overlooked high filling factor component of the hot ISM. Suzaku observations along this line of sight, coupled with the Suzaku observation towards MBM12, will allow the isolation of this component.	GALACTIC DIFFUSE EMISSION	5	B	K. KUNTZ		USA	1	AO1	BEYOND THE LOCAL HOT BUBBLE TOWARDS L=111	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501100010/	Quick Look
324	DRACO ENHANCEMENT	239.3128	61.2868	239.109888	61.42925	187.011559	75.692319	93.98685674	43.98646489	194.9053	54048.1213888889	2006-11-09 02:54:48	54049.8515509259	2006-11-10 20:26:14	501101010	43.8628	75	79.4274	79.4274	43.8628	79.4194	2	2	2	2	1	0	0	75.8741	75.8741	149.474	1	PROCESSED	57536.1016319444	2016-05-28 02:26:21	54455	2007-12-21 00:00:00	54088.7470486111	2006-12-19 17:55:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011259	We propose to observe the Draco Enhancement, a region of very bright 1/4 keV emission in the northern Galactic halo that is only 15 degrees from the Suzaku observation of the North Ecliptic Pole. A decomposition of the spectrum of the Galactic halo by Kuntz & Snowden showed that, to within the uncertainties of the ROSAT All-Sky Survey, the halo emission was composed of two thermal components; a uniform hot component with kT~0.25 keV, and a very patchy soft component with kT~0.1 keV. The soft component is found in only a few isolated regions of the sky, of which the Draco Enhancement is the brightest. This emission is too soft to be studied with XMM. Suzaku will allow us to determine the temperature of the soft component or place very strict upper limits on its temperature.	GALACTIC DIFFUSE EMISSION	5	C	K. KUNTZ		USA	1	AO1	THE SOFT COMPONENT OF THE GALACTIC HALO	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501101010/	Quick Look
325	MONOGEM RING WEST	118.3557	8.2507	117.679197	8.381467	118.769502	-12.402687	212.50229712	17.5030797	287.8334	53865.545462963	2006-05-10 13:05:28	53867.1127199074	2006-05-12 02:42:19	501084010	54.2685	50	54.2685	54.2685	54.2685	54.2685	2	2	2	2	1	0	0	43.2312	43.2312	135.3899	2	PROCESSED	57534.3136689815	2016-05-26 07:31:41	54401	2007-10-28 00:00:00	53914.2479282407	2006-06-28 05:57:01	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011243	We propose to acquire the first high-quality, CCD resolution spectrum of the Monogem Ring SNR. The Monogem Ring is a large (D~25 degrees), old (t~10^5 yr) SNR with a soft X-ray spectrum. A 50 ks observation with Suzaku will detect and measure the OVII Triplet and OVIII Lyman-alpha line fluxes. We will use the ratio of these two line complexes to constrain the temperature and ionization timescale of the plasma in this region of the Monogem Ring. Determing the plasma conditions in such evolved SNRs is important for understanding how these remnants merge with and affect the interstellar medium.	GALACTIC DIFFUSE EMISSION	5	B	PAUL PLUCINSKY		USA	1	AO1	THE MONOGEM RING: MEASURING THE O LINE EMISSION WITH SUZAKU	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501084010/	Quick Look
326	3C 390.3	280.629	79.7686	281.497615	79.715169	81.957835	76.491681	111.4356997	27.05756334	197.286	54083.1426851852	2006-12-14 03:25:28	54085.1384722222	2006-12-16 03:19:24	701060010	0.024	100	99.3678	99.3678	0.024	99.3678	2	2	1	2	1	0	0	97.8813	97.8813	172.4199	3	PROCESSED	57536.3784722222	2016-05-28 09:05:00	54702	2008-08-24 00:00:00	54132.9968055556	2007-02-01 23:55:24	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011363	We propose Suzaku observations of the X-ray bright Broad-Line Radio Galaxies 3C382 and 3C390.3 to study their complex broad-band X-ray spectra. The HXD will constrain the continuum above 10 keV, discriminating between competing physically-different models, while at the same time the XIS will determine the parameters of the FeKalpha line and the shape of the soft X-rays. The proposed observations will allow us to shed light on the origin of reflection features in radio-loud AGN, ultimately determining the structure and ionization state of the accretion flow in these objects.	EXTRAGALACTIC COMPACT SOURCES	7	C	RITA SAMBRUNA		USA	1	AO1	THE BROAD-BAND X-RAY SPECTRUM OF BROAD-LINE RADIO GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701060010/	Quick Look
327	CYGNUS_LOOP_P15	312.9857	30.6621	312.465734	30.473222	327.433989	45.909388	74.106397	-8.72540127	61.9987	53880.177974537	2006-05-25 04:16:17	53880.6716898148	2006-05-25 16:07:14	501032010	20.7289	21	20.7289	20.7289	20.7289	20.7289	2	2	2	2	1	0	0	17.476	17.476	42.6349	0	PROCESSED	57534.4101041667	2016-05-26 09:50:33	54394	2007-10-21 00:00:00	53926.2440046296	2006-07-10 05:51:22	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501032010/	Quick Look
328	NGC 7213	332.316	-47.1629	331.53332	-47.408605	315.985734	-33.170959	349.59497628	-52.58020545	231.3714	54030.2323611111	2006-10-22 05:34:36	54032.2759722222	2006-10-24 06:37:24	701029010	90.736	100	90.76	90.744	90.736	90.752	2	2	2	2	1	0	0	90.3418	90.3418	176.5358	0	PROCESSED	57535.9564814815	2016-05-27 22:57:20	54695	2008-08-17 00:00:00	54056.3665162037	2006-11-17 08:47:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011305	We propose a 100ks Suzaku observation of the low luminosity AGN, NGC 7213. Previous observations show a complex iron line and weak or no Compton reflection. However the iron line and reflection hump are poorly constrained, so the line emitting matter could arise from a truncated disk, BLR or a Compton-thin torus. A high quality Suzaku observation will constrain the iron line profile, resolve the ionized emission and unambiguously determine its origin. Using the unique broad bandpass of Suzaku above 10 keV we will place tight constraints on any reflection hump, enabling us to determine if the iron line originates from a truncated disk. This could provide a direct test of the paradigm that the X-ray emission in low accretion rate AGN occurs in a truncated disk system such as an ADAF.	EXTRAGALACTIC COMPACT SOURCES	7	B	JAMES REEVES		USA	1	AO1	DOES THE LOW LUMINOSITY AGN NGC7213 CONTAIN A TRUNCATED ACCRETION DISK?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701029010/	Quick Look
329	IRAS 19254-7245	292.8508	-72.6492	291.381636	-72.754038	280.373528	-50.031737	322.5078751	-28.76929596	279.8892	54041.9830208333	2006-11-02 23:35:33	54044.5967476852	2006-11-05 14:19:19	701052010	113.5123	120	113.5203	113.5203	113.5123	113.5203	2	2	2	2	1	0	0	151.9778	151.9778	225.8099	1	PROCESSED	57536.068125	2016-05-28 01:38:06	54455	2007-12-21 00:00:00	54088.8285185185	2006-12-19 19:53:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011342	We propose a 120 ksec Suzaku exposure of the ULIRG IRAS19254-7245. A previous XMM-Newton observation revealed the presence of a strong iron emission line and a flat continuum, both suggesting that this source hosts a Compton-thick AGN. In this scenario, the 2-10 keV luminosity of IRAS19254-7245 could be greater than 10e44 erg/s. However since no direct continuum is visible in the XMM bandpass, a direct measure of the absorbing column density was not feasible, thus the intrinsic X-ray luminosity of this source was derived only through indirect arguments. The unique bandpass and sensititvity of Suzaku above 10 keV will allow us to confirm the Compton-thick nature of this source and to measure for the first time the intrinsic X-ray luminosity of the AGN hosted in IRAS 19254-7245.	EXTRAGALACTIC COMPACT SOURCES	7	C	VALENTINA BRAITO		USA	1	AO1	ASSESSING THE ENERGETIC BUDGET IN THE SUPERANTENNAE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701052010/	Quick Look
330	A85	10.4739	-9.4292	9.841504	-9.703266	5.843917	-12.80705	115.23010576	-72.15810594	248.2856	54105.4020023148	2007-01-05 09:38:53	54108.0557175926	2007-01-08 01:20:14	801041010	99.2012	100	99.2012	99.2012	0	99.2012	2	2	0	2	1	0	0	84.8139	84.8139	229.2421	2	PROCESSED	57536.5180671296	2016-05-28 12:26:01	54735	2008-09-26 00:00:00	54132.9388773148	2007-02-01 22:31:59	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010088	We propose observations of A2199 and A85 clusters of galaxies with an each exposure time of 100 ks, in order to search for excess hard X-ray emission, to constrain the spectral shape, and to discuss the origin of the hard X-ray emission. Both are listed as the clusters which are detected non-thermal emission signal with 2 sigma confidence level by Beppo SAX PDS detector. In addition, these two clusters only have features of brighter X-ray flux, good size, relatively cool ICM temperature, and including no bright member AGNs. Therefore they are suitable target samples for our observational purpose about estimation photon index and flux for the excess hard X-ray emission with high significance wherever possible.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	RYO SHIBATA		JAP	1	AO1	SEARCH FOR EXCESS HARD X-RAY EMISSION FROM A2199 AND A85 GALAXY CLUSTERS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801041010/	Quick Look
331	UGC5101	143.841	61.3185	142.895417	61.541858	122.479903	43.806931	152.55229096	42.85621781	331.581	53825.1798148148	2006-03-31 04:18:56	53826.3509722222	2006-04-01 08:25:24	701002010	48.9902	70	48.9902	48.9902	48.9902	48.9902	2	2	2	2	1	0	0	43.9748	43.9748	101.1779	0	PROCESSED	57533.3610763889	2016-05-25 08:39:57	54735	2008-09-26 00:00:00	53905.890625	2006-06-19 21:22:30	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010001	We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASATOSHI IMANISHI		JAP	1	AO1	COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701002010/	Quick Look
332	IRAS13224-3809	201.327	-38.416	200.607672	-38.155977	214.865009	-27.173801	310.18598264	23.97820794	118.5234	54126.2420601852	2007-01-26 05:48:34	54131.0849421296	2007-01-31 02:02:19	701003010	197.9376	200	197.9536	197.9376	0	197.9516	2	2	0	2	1	0	0	169.6526	169.6526	418.3978	4	PROCESSED	57537.0458912037	2016-05-29 01:06:05	54777	2008-11-07 00:00:00	54139.7293287037	2007-02-08 17:30:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010028	We propose a 200 ks continuous observation of the narrow-line Seyfert 1 galaxy IRAS13224-3809 in order to understand its remarkable and puzzling spectral and variability properties. Suzaku data will enable us to disentangle the two interpretations adopted so far, namely partial covering and relativistically blurred reflection. If the latter then the appearance of the source is controlled by general relativistic effects. In addition, the ability for Suzaku to conduct long continuous observations will allow us to monitor IRAS13224-3809 for giant amplitude flaring (as seen with ROSAT); therefore enabling us to enhance our understanding of AGN variability.	EXTRAGALACTIC COMPACT SOURCES	7	B	YASUO TANAKA		JAP	1	AO1	THE REMARKABLE NARROW LINE SEYFERT 1 GALAXY IRAS13224-3809	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701003010/	Quick Look
333	SNR 0103-72.6	16.2944	-72.389	15.898915	-72.656584	313.931508	-65.2662	301.47055063	-44.70024477	13.8765	53848.0156018518	2006-04-23 00:22:28	53849.3773032407	2006-04-24 09:03:19	501077010	49.2715	50	49.2795	49.2875	49.2875	49.2715	2	2	2	2	1	0	0	37.1905	37.1905	117.6299	3	PROCESSED	57533.5571296296	2016-05-25 13:22:16	54401	2007-10-28 00:00:00	53907.4220023148	2006-06-21 10:07:41	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011241	We propose Suzaku observations of O-rich supernova remnants (SNRs) 0103-72.6 and 0049-73.6 in the Small Magellanic Cloud (SMC). These SMC SNRs are oldest members (18000 and 14000 yr old) of O-rich SNRs and share X-ray spectral characteristics with a young (1000 yr old) O-rich SNR 0102-7219 which is also in the SMC. While sharing similar spectral features with 0102-7219, the morphologies of 0103-72.6 and 0049-73.6 indicate more evolved phases of the SNR in a similar interstellar environment as 0102-7219. Cross-comparison studies with the high spectral resolution Suzaku/XIS observations among 0103-72.6/0049-73.6 (this proposal) and 0102-7219 (scheduled/observed for the instrument calibrations) will provide a unique opportunity for the study of a long-term evolution of an O-rich SNR.	GALACTIC DIFFUSE EMISSION	5	A	SANGWOOK PARK		USA	1	AO1	BACK TO THE FUTURE: LONG-TERM EVOLUTION OF OXYGET-RICH SUPERNOVA REMNANTS IN THE SMALL MAGELLANIC CLOUD	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501077010/	Quick Look
334	PUP A : BEK	125.942	-42.9405	125.511174	-42.777913	147.596211	-59.401563	260.51799115	-3.16426215	276.3687	53842.2933449074	2006-04-17 07:02:25	53842.5807407407	2006-04-17 13:56:16	501086010	16.0913	15	16.0913	16.0993	16.0913	16.0913	1	1	1	1	1	0	0	9.6985	9.6985	24.797	0	PROCESSED	57533.4850115741	2016-05-25 11:38:25	54401	2007-10-28 00:00:00	53906.8467708333	2006-06-20 20:19:21	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501086010/	Quick Look
335	CYGNUS_LOOP_P19	311.8094	30.0818	311.288879	29.89716	325.768852	45.764417	73.00862935	-8.2918477	237.4997	54087.3411805556	2006-12-18 08:11:18	54087.8245833333	2006-12-18 19:47:24	501036010	18.595	17	18.595	18.595	0	18.595	2	2	0	2	1	0	0	18.355	18.355	41.7559	0	PROCESSED	57536.3627199074	2016-05-28 08:42:19	54744	2008-10-05 00:00:00	54096.1443171296	2006-12-27 03:27:49	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010052	We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	1	AO1	OBSERVATION OF THE CYGNUS LOOP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501036010/	Quick Look
336	XB 1916-053	289.7027	-5.2415	289.037629	-5.333849	290.520863	16.806325	31.35614078	-8.46800846	250.2538	54047.242974537	2006-11-08 05:49:53	54048.1119791667	2006-11-09 02:41:15	401095010	38.4647	40	39.0967	39.0887	38.4647	39.0967	2	2	2	2	1	0	0	37.4857	37.4857	75.082	2	PROCESSED	57536.0684259259	2016-05-28 01:38:32	54735	2008-09-26 00:00:00	54088.866087963	2006-12-19 20:47:10	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012038	We propose Suzaku observations of the dipping low mass X-ray binaries XB1916-053, XB1323-619, EXO0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been recently demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the photoionised absorbers and reliably determine the values of the ionization parameter for each source, and the simultaneous spectra of HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components and to extend the photoionized absorber fits to higher energies. This will test the validity of the ionized absorber model also >10 keV.	GALACTIC POINT SOURCES	4	A	MARIA DIAZ TRIGO		EUR	1	AO1	BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401095010/	Quick Look
337	A2142	239.5312	27.2879	239.014287	27.430116	229.09968	46.49364	44.29837206	48.74478569	138.1624	54104.1546990741	2007-01-04 03:42:46	54105.3891666667	2007-01-05 09:20:24	801055010	51.4525	60	51.4605	51.4525	0	51.4605	2	2	0	2	1	0	0	49.2098	49.2098	106.632	1	PROCESSED	57536.4705555556	2016-05-28 11:17:36	54735	2008-09-26 00:00:00	54111.417037037	2007-01-11 10:00:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	010106	We propose to reveal the formation and evolution of dense core with cold fronts with SUZAKU/XIS. Our strategy of observation is based on the results of Chandra, ROSAT and weak lensing analysis. A2142 is a galaxy cluster which has contact discontinuities, "cold fronts", between cold-dense cores and hot-thin surrounding gas. We have carried out "weak lensing analysis" and derived mass map in A2142. We measure the bulk velocity via Fe-K line in the central region. We derive the merger velocity by observing the temperatures of the heating and non-heating which are expected by our observational results. It leads to understand the formation and evolution of dense core with cold fronts, since the merger and core velocities are closely related to the evolution of dense cores with cold fronts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NOBUHIRO OKABE		JAP	1	AO1	REVEALING COLD FRONTS AND DENSE CORES IN GALAXY CLUSTER A2142	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801055010/	Quick Look

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