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 37

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	CYGNUS X-1	299.5392	35.2589	299.069624	35.122644	313.628523	54.317489	71.36219421	3.13231837	55.3254	54957.7006828704	2009-05-06 16:48:59	54958.1356365741	2009-05-07 03:15:19	404075060	19.4345	300	19.4345	19.4505	0	19.4345	2	1	0	2	1	0	0	15.2795	15.2795	37.5579	0	PROCESSED	57546.5121412037	2016-06-07 12:17:29	54922	2009-04-01 00:00:00	54976.0885300926	2009-05-25 02:07:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075060/	Quick Look
2	CYGNUS X-1	299.5373	35.2573	299.067717	35.121052	313.625096	54.316504	71.3600172	3.13281014	53.4895	54976.3582060185	2009-05-25 08:35:49	54976.8259722222	2009-05-25 19:49:24	404075090	20.9252	300	20.9252	20.9332	0	20.9252	2	1	0	2	1	0	0	16.1164	16.1164	40.412	1	PROCESSED	57546.6796296296	2016-06-07 16:18:40	54922	2009-04-01 00:00:00	54992.6651736111	2009-06-10 15:57:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075090/	Quick Look
3	CYGNUS X-1	299.5294	35.2515	299.059794	35.115286	313.611339	54.313209	71.35169447	3.13529932	46.7675	54984.481400463	2009-06-02 11:33:13	54984.9870833333	2009-06-02 23:41:24	404075110	17.4502	300	19.037	17.7782	0	17.4502	1	1	0	1	1	0	0	15.0409	15.0409	43.6879	1	PROCESSED	57547.4475462963	2016-06-08 10:44:28	54922	2009-04-01 00:00:00	54994.4091087963	2009-06-12 09:49:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075110/	Quick Look
4	CYGNUS X-1	299.6354	35.1397	299.164908	35.003038	313.686688	54.178801	71.30132058	3.00311627	241.1557	55159.514224537	2009-11-24 12:20:29	55160.1328587963	2009-11-25 03:11:19	404075180	21.7685	300	21.7685	22.4805	0	22.4725	5	2	0	3	1	0	0	11.4064	11.4064	53.4358	0	PROCESSED	57549.5783680556	2016-06-10 13:52:51	54922	2009-04-01 00:00:00	55176.294849537	2009-12-11 07:04:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075180/	Quick Look
5	CYGNUS X-1	299.5895	35.2721	299.119922	35.135631	313.702443	54.316106	71.39489928	3.10413213	91.3103	54929.2562847222	2009-04-08 06:09:03	54929.8224421296	2009-04-08 19:44:19	404075020	21.3361	300	21.3361	21.3361	0	21.3361	2	1	0	2	1	0	0	13.1258	13.1258	48.914	0	PROCESSED	57546.0782638889	2016-06-07 01:52:42	54922	2009-04-01 00:00:00	54949.4903125	2009-04-28 11:46:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075020/	Quick Look
6	A3112	49.3542	-44.4494	48.920816	-44.631605	25.154749	-59.092558	253.34888003	-56.10584592	209.0003	57003.8439467593	2014-12-12 20:15:17	57006.6182407407	2014-12-15 14:50:16	809116020	97.989	200	97.989	97.989	0	97.989	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.5061458333	2016-08-17 12:08:51	57387	2015-12-31 00:00:00	57017.4238425926	2014-12-26 10:10:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	094527	The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ESRA BULBUL		USJ	9	AO9	A DETAILED STUDY OF CHEMICAL ENRICHMENT OF A3112 OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809116020/	Quick Look
7	CYGNUS X-1	299.6277	35.1371	299.157204	35.000471	313.675062	54.178467	71.29581116	3.00713364	246.5433	55145.8193981482	2009-11-10 19:39:56	55146.4377199074	2009-11-11 10:30:19	404075160	26.0222	300	26.0222	26.0382	0	26.0265	2	1	0	2	1	0	0	18.2505	18.2505	53.416	0	PROCESSED	57549.2577199074	2016-06-10 06:11:07	54922	2009-04-01 00:00:00	55176.2027430556	2009-12-11 04:51:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075160/	Quick Look
8	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
9	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
10	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
11	SN 1978K	49.5382	-66.5402	49.387343	-66.721221	341.369857	-74.185234	283.41338803	-44.62366671	13.2585	56804.2369097222	2014-05-27 05:41:09	56806.5279398148	2014-05-29 12:40:14	709023010	107.3136	100	107.3216	107.3216	0	107.3136	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.1724074074	2016-08-15 04:08:16	57234	2015-07-31 00:00:00	56866.7205092593	2014-07-28 17:17:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	094341	SN 1978K is a remarkable Type IIn supernova that remains bright at X-ray through radio wavelengths 35 years after its explosion. Our ongoing multiwavelength observations probe the dense medium that was ejected by the progenitor star, possibly a Luminous Blue Variable. While the radio flux dropped steadily, the X-ray and UV/optical fluxes remained surprisingly constant for a decade. However, our most recent XMM observation in 2013 June reveals a significant fading compared to the 2006 Oct Suzaku observation. Here we request a 100 ksec observation to study the spectral evolution during the decay. This will serve as a pathfinder for younger Type IIn supernovae. As secondary science, we will obtain data on the ULXs X-1 and X-2, and the other luminous sources in NGC 1313.	EXTRAGALACTIC COMPACT SOURCES	7	B	IAN SMITH	SHOGO KOBAYASHI	USJ	9	AO9	STUDYING THE LATE-TIME DECAY OF SN 1978K	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709023010/	Quick Look
12	NGC 1332	51.5732	-21.333	51.017829	-21.507123	42.191625	-38.615675	212.17958034	-54.36451308	243.6482	55581.2509027778	2011-01-20 06:01:18	55584.0883333333	2011-01-23 02:07:12	805095010	101.423	100	101.423	101.423	0	101.423	2	2	0	2	1	0	0	89.9683	89.9683	245.1259	2	PROCESSED	57600.7603935185	2016-07-31 18:14:58	55965	2012-02-08 00:00:00	55599.216724537	2011-02-07 05:12:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	054502	Recent observations of relaxed galaxy groups have revealed ubiquitous abundance gradients. The broad peaks of Fe abundance indicate (turbulent) diffusion of metals possibly driven by AGN feedback. Exploiting the low background and good sensitivity of Suzaku XIS, we have found similar gradients in three lower mass (virial mass 5-10E12 Msun) elliptical galaxies, which has important implications for models of feedback and chemical enrichment. We propose to observe another two carefully chosen galaxies, thus starting to build a sample for determining the frequency and properties of such abundance gradients in early-type galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	PHILIP HUMPHREY	RYO NAGINO	USJ	5	AO5	ABUNDANCE GRADIENTS IN EARLY-TYPE GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805095010/	Quick Look
13	A3112	49.3536	-44.4489	48.920211	-44.631107	25.15452	-59.09191	253.34827073	-56.10640985	209.0009	57000.6762037037	2014-12-09 16:13:44	57003.8439351852	2014-12-12 20:15:16	809116010	107.9651	200	107.9651	107.9651	0	107.9651	2	2	0	2	1	0	0	8.1487	8.1487	33.9079	1	PROCESSED	57617.53125	2016-08-17 12:45:00	57387	2015-12-31 00:00:00	57016.2346180556	2014-12-25 05:37:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	094527	The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ESRA BULBUL	KOSUKE SATO	USJ	9	AO9	A DETAILED STUDY OF CHEMICAL ENRICHMENT OF A3112 OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809116010/	Quick Look
14	CYGNUS X-1	299.6653	35.165	299.194917	35.028212	313.740573	54.19441	71.33570459	2.99545336	212.8004	55182.0619328704	2009-12-17 01:29:11	55182.5508564815	2009-12-17 13:13:14	404075070	22.1019	300	22.1019	22.1099	0	23.664	1	1	0	1	1	0	0	3.4607	3.4607	42.236	0	PROCESSED	57549.8755671296	2016-06-10 21:00:49	54922	2009-04-01 00:00:00	55200.4490046296	2010-01-04 10:46:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075070/	Quick Look
15	CYGNUS X-1	299.6549	35.1555	299.184474	35.018756	313.721426	54.188323	71.32314713	2.99775182	222.7295	55173.647349537	2009-12-08 15:32:11	55174.1043287037	2009-12-09 02:30:14	404075200	20.0166	300	20.0166	21.7526	0	21.8593	1	1	0	1	1	0	0	17.4426	17.4426	39.4719	0	PROCESSED	57549.7233912037	2016-06-10 17:21:41	54922	2009-04-01 00:00:00	55189.2752430556	2009-12-24 06:36:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075200/	Quick Look
16	CYGNUS X-1	299.5891	35.272	299.119523	35.135533	313.701858	54.316122	71.39464341	3.10435878	91.3113	54935.7650462963	2009-04-14 18:21:40	54936.1473958333	2009-04-15 03:32:15	404075030	17.1088	300	17.1088	17.1168	0	17.1088	2	1	0	2	1	0	0	12.986	12.986	33.0279	1	PROCESSED	57546.1452662037	2016-06-07 03:29:11	54922	2009-04-01 00:00:00	54949.5303240741	2009-04-28 12:43:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075030/	Quick Look
17	CYGNUS X-1	299.6021	35.1308	299.131607	34.994279	313.637751	54.179562	71.27949874	3.02171591	263.2299	55125.3772106482	2009-10-21 09:03:11	55125.8404398148	2009-10-21 20:10:14	404075130	20.4985	300	20.4985	20.5065	0	20.4985	2	1	0	2	1	0	0	15.163	15.163	40.0159	0	PROCESSED	57548.9405208333	2016-06-09 22:34:21	54922	2009-04-01 00:00:00	55134.2701967593	2009-10-30 06:29:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075130/	Quick Look
18	CYGNUS X-1	299.6206	35.1339	299.150096	34.997301	313.663881	54.177403	71.29004535	3.01042005	252.1788	55138.8946180556	2009-11-03 21:28:15	55139.4106365741	2009-11-04 09:51:19	404075150	22.6168	300	22.6168	22.6248	0	22.6168	2	1	0	2	1	0	0	14.061	14.061	44.5759	1	PROCESSED	57549.0593981482	2016-06-10 01:25:32	54922	2009-04-01 00:00:00	55149.4202199074	2009-11-14 10:05:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075150/	Quick Look
19	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
20	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
21	3C382	278.7516	32.7087	278.287499	32.667445	283.134608	55.751017	61.3132426	17.46021716	69.589	54217.9621412037	2007-04-27 23:05:29	54220.8119097222	2007-04-30 19:29:09	702125010	130.58	120	130.588	130.58	0	130.588	2	2	0	2	1	0	0	122.4707	122.4707	246.1958	2	PROCESSED	57538.5400694444	2016-05-30 12:57:42	54777	2008-11-07 00:00:00	54228.2765740741	2007-05-08 06:38:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	024353	We propose Suzaku observations of the X-ray bright Broad-Line Radio Galaxy 3C382 to study its complex broad-band X-ray spectrum and its variability on longer timescales. To this end, we ask for 3 separate observations of 40 ks each, to be scheduled randomly but not less than a couple of days apart. We aim at probing the origin of the reflection features and strong soft excess in 3C382, ultimately determining the structure and ionization state of the accretion flow. The addition of 3C382 to the Suzaku program (already including 3C120 and 3C390.3) will allow us to explore BLRGs central engines over a wide range of accretion/jet parameters.	EXTRAGALACTIC COMPACT SOURCES	7	B	RITA SAMBRUNA	Jun Kataoka	USJ	2	AO2	THE HIGH-ENERGY SPECTRA OF BROAD-LINE RADIO GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702125010/	Quick Look
22	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
23	COMA11	194.6305	28.3939	194.027281	28.663593	180.9862	31.643484	72.26601068	87.98563538	292.5148	54270.6441782407	2007-06-19 15:27:37	54272.0078009259	2007-06-21 00:11:14	802082010	53.0217	50	53.0217	53.0217	0	53.0217	2	2	0	2	1	0	0	46.6673	46.6673	117.806	2	PROCESSED	57539.0191203704	2016-05-31 00:27:32	54695	2008-08-17 00:00:00	54322.5438888889	2007-08-10 13:03:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	024438	Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JOEL BREGMAN	Yoh Takei	USJ	2	AO2	THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802082010/	Quick Look
24	A496 P-CENTER	68.4146	-13.2791	67.835234	-13.38285	64.149602	-34.804694	209.60984883	-36.48888222	55.8718	54680.8514814815	2008-08-02 20:26:08	54682.0543865741	2008-08-04 01:18:19	803073010	44.2607	30	44.2607	44.2607	0	44.2607	1	1	0	1	1	0	0	36.9355	36.9355	103.904	2	PROCESSED	57543.1885416667	2016-06-04 04:31:30	55059	2009-08-16 00:00:00	54693.2133796296	2008-08-15 05:07:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	034424	A496 is a "normal" nearby cluster that has been the testbed for metal enrichment models in clusters and, more recently, of different mechanisms to generate cold fronts. Suzaku's excellent spectral resolution, low background and high effective area, combined with the moderate temperatures of this cluster allows us to probe, with two short exposures, into the large scale metal enrichment processes through determination of elemental abundance ratios out to half the virial radius for the first time.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	RENATO DUPKE	KYOKO MATSUSHITA	USJ	3	AO3	LARGE SCALE METAL ENRICHMENT MECHANISMS IN ABELL 496	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803073010/	Quick Look
25	CYGNUS X-1	299.5814	35.2712	299.11183	35.134765	313.691248	54.317484	71.39067981	3.10930809	85.1433	54949.7099884259	2009-04-28 17:02:23	54950.2175925926	2009-04-29 05:13:20	404075050	20.5212	300	20.5292	20.5354	0	20.5212	2	1	0	2	1	0	0	12.4013	12.4013	43.8459	0	PROCESSED	57546.4475462963	2016-06-07 10:44:28	54922	2009-04-01 00:00:00	54976.2030671296	2009-05-25 04:52:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075050/	Quick Look
26	CYGNUS X-1	299.6355	35.1397	299.165007	35.003038	313.68682	54.178773	71.30136328	3.00304649	241.2259	55152.2855092593	2009-11-17 06:51:08	55152.9418287037	2009-11-17 22:36:14	404075170	23.4485	300	23.4485	23.8885	0	23.8805	2	1	0	2	1	0	0	18.7071	18.7071	56.6918	3	PROCESSED	57549.4356597222	2016-06-10 10:27:21	54922	2009-04-01 00:00:00	55162.2019212963	2009-11-27 04:50:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075170/	Quick Look
27	CYGNUS X-1	299.6537	35.1518	299.183253	35.015061	313.717721	54.185168	71.31947353	2.99665901	225.8159	55166.2922453704	2009-12-01 07:00:50	55166.8904398148	2009-12-01 21:22:14	404075190	22.4155	300	22.4155	22.4315	0	22.4235	2	1	0	2	1	0	0	13.1578	13.1578	51.6739	0	PROCESSED	57549.6647222222	2016-06-10 15:57:12	54922	2009-04-01 00:00:00	55181.288912037	2009-12-16 06:56:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075190/	Quick Look
28	COMABKG	198.7472	31.648	198.161117	31.912033	183.000201	36.170261	75.72732699	83.16527783	295.0754	54272.0100347222	2007-06-21 00:14:27	54272.7015046296	2007-06-21 16:50:10	802083010	30.7831	30	30.7831	30.7831	0	30.7831	2	2	0	2	1	0	0	26.5058	26.5058	59.7399	0	PROCESSED	57539.0181597222	2016-05-31 00:26:09	54702	2008-08-24 00:00:00	54333.4315393518	2007-08-21 10:21:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	024438	Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JOEL BREGMAN	Yoh Takei	USJ	2	AO2	THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802083010/	Quick Look
29	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
30	CYGNUS X-1	299.6086	35.1319	299.138103	34.995352	313.646938	54.178814	71.28321336	3.01775246	259.2069	55130.2652314815	2009-10-26 06:21:56	55130.7481365741	2009-10-26 17:57:19	404075140	23.1042	300	23.1042	23.1282	0	23.1202	2	1	0	2	1	0	0	20.011	20.011	41.716	0	PROCESSED	57548.9943171296	2016-06-09 23:51:49	54922	2009-04-01 00:00:00	55141.3539467593	2009-11-06 08:29:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075140/	Quick Look
31	CYGNUS X-1	299.5964	35.2723	299.126812	35.135802	313.711652	54.314398	71.39800953	3.09942804	95.8123	54924.0537384259	2009-04-03 01:17:23	54924.5654282407	2009-04-03 13:34:13	404075010	15.3091	300	15.3091	15.3188	0	15.3108	2	1	0	2	1	0	0	15.5374	15.5374	44.2039	1	PROCESSED	57546.0113425926	2016-06-07 00:16:20	54922	2009-04-01 00:00:00	54949.4917824074	2009-04-28 11:48:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075010/	Quick Look
32	CYGNUS X-1	299.5337	35.2545	299.064105	35.118267	313.618737	54.314854	71.35609035	3.13386262	50.0944	54980.4956712963	2009-05-29 11:53:46	54981.0586226852	2009-05-30 01:24:25	404075100	28.7845	300	28.7845	28.7845	0	28.7845	1	1	0	1	1	0	0	25.7389	25.7389	48.6319	1	PROCESSED	57546.7292476852	2016-06-07 17:30:07	54922	2009-04-01 00:00:00	54994.3872800926	2009-06-12 09:17:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075100/	Quick Look
33	CYGNUS X-1	299.5272	35.2497	299.057586	35.113495	313.607401	54.312117	71.34921869	3.1358965	44.7834	54986.8208333333	2009-06-04 19:42:00	54987.3356944444	2009-06-05 08:03:24	404075120	16.8733	300	16.8813	16.8894	0	16.8733	2	1	0	2	1	0	0	6.7647	6.7647	44.4779	1	PROCESSED	57547.4806018518	2016-06-08 11:32:04	54922	2009-04-01 00:00:00	55001.0163078704	2009-06-19 00:23:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075120/	Quick Look
34	COMABKG2	194.3428	28.1403	193.738458	28.410336	180.855412	31.302815	70.87532192	88.34137752	297.3385	54272.7041550926	2007-06-21 16:53:59	54273.4897453704	2007-06-22 11:45:14	802084010	31.9731	30	31.9731	33.5956	0	33.5956	2	2	0	2	1	0	0	28.853	28.853	67.8501	1	PROCESSED	57539.0184143518	2016-05-31 00:26:31	54695	2008-08-17 00:00:00	54318.5135648148	2007-08-06 12:19:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	024438	Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JOEL BREGMAN	Yoh Takei	USJ	2	AO2	THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802084010/	Quick Look
35	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
36	CYGNUS X-1	299.5791	35.2719	299.109539	35.135475	313.68862	54.318776	71.39029863	3.11127562	84.0536	54944.1674768518	2009-04-23 04:01:10	54944.6252777778	2009-04-23 15:00:24	404075040	18.014	300	18.0166	18.014	0	18.0166	1	1	0	1	1	0	0	16.3277	16.3277	39.55	0	PROCESSED	57546.2094097222	2016-06-07 05:01:33	54922	2009-04-01 00:00:00	54966.3125	2009-05-15 07:30:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075040/	Quick Look
37	CYGNUS X-1	299.5434	35.2592	299.073819	35.122926	313.634234	54.316619	71.36423878	3.12954641	57.7977	54971.0242592593	2009-05-20 00:34:56	54971.6043865741	2009-05-20 14:30:19	404075080	21.3404	300	21.3404	21.3484	0	21.3404	2	1	0	2	1	0	0	17.4954	17.4954	50.1199	1	PROCESSED	57546.6088888889	2016-06-07 14:36:48	54922	2009-04-01 00:00:00	54992.6546875	2009-06-10 15:42:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	044131	In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.	GALACTIC POINT SOURCES	4	A	JON MILLER	SHIN YAMADA	USJ	4	AO4	A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404075080/	Quick Look

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