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 518

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	NGC 3660	170.883	-8.6561	170.2492	-8.381454	175.088091	-11.559037	269.10006798	48.35629614	109.6283	56624.1463773148	2013-11-28 03:30:47	56627.0001967593	2013-12-01 00:00:17	708043010	124.7774	120	124.7854	124.7854	0	124.7774	2	2	0	2	1	0	0	109.7692	109.7692	246.5434	2	PROCESSED	57613.5216550926	2016-08-13 12:31:11	57058	2015-02-05 00:00:00	56691.7534953704	2014-02-03 18:05:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082003	We propose a 120-ks observation of NGC 3660, which is a strong candidate for a True Seyfert 2, a Seyfert that intrinsically lacks the broad line regions (BLRs), and challenges the AGN unified scheme. However, a puzzling BeppoSAX observation lingers, which shows excess emission above 10 keV indicative of a Compton thick AGN. Nevertheless, rapid variability below 10 keV and meagre iron line emission (EW=60 eV) strongly argue against this conclusion. Data from the HXD will elucidate the situation, and either dispel this evidence, adding weight to the True Seyfert 2 scenario, or confirm the presence of heavily obscured emission, which may be explained by a partial covering scenario.	EXTRAGALACTIC COMPACT SOURCES	7	B	MURRAY BRIGHTMAN		EUR	8	AO8	NGC 3660: A TRUE SEYFERT 2?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708043010/	Quick Look
2	NGC 4051	180.8556	44.5807	180.217538	44.859022	159.275193	40.404023	148.68917976	70.06918189	135.3482	53684.8015509259	2005-11-10 19:14:14	53687.4315277778	2005-11-13 10:21:24	700004010	119.578	150	119.61	119.61	119.586	119.578	2	2	2	2	1	0	0	120.0047	120.0047	227.1918	3	PROCESSED	57528.0225810185	2016-05-20 00:32:31	54247	2007-05-27 00:00:00	54037.5713078704	2006-10-29 13:42:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001012	We propose to obtain a broad band spectrum of the narrow-line Seyfert 1 (NLS1) NGC 4051. NLS1s are often presumed that they host a relatively small black hole with a very high accretion rate. Such a class would have played an important role in the growth of black holes in a cosmological context. We will measure the intrinsic photon index, amount of reflection, and high energy cutoff for the first time to investigate an accretion disk under a high accretion rate and compare them with conventional broad-line Seyferts.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	0	SWG	THE ACCRETION IN THE NARROW-LINE SEYFERT 1 NGC 4051 PROBED BY A BROAD BAND SPECTRUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700004010/	Quick Look
3	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
4	EMS0071	16.6433	48.9425	15.913472	48.675321	36.903288	38.099489	125.49064727	-13.85403968	69.9406	55392.4123148148	2010-07-15 09:53:44	55392.8855092593	2010-07-15 21:15:08	705010010	23.0102	20	23.0102	23.0102	0	23.0102	2	2	0	2	1	0	0	19.568	19.568	40.8819	0	PROCESSED	57552.6419560185	2016-06-13 15:24:25	55779	2011-08-06 00:00:00	55411.2637384259	2010-08-03 06:19:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050050	We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators".	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5	SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705010010/	Quick Look
5	HOLMBERG IX X-1	149.4869	69.0752	148.468802	69.313718	119.773156	51.703341	141.91661656	41.06840873	124.5	56224.1252199074	2012-10-24 03:00:19	56226.4168981482	2012-10-26 10:00:20	707019030	106.9454	500	106.9454	106.9534	0	106.9614	2	2	0	2	1	0	0	105.0119	105.0119	197.9478	1	PROCESSED	57607.8725462963	2016-08-07 20:56:28	56018	2012-04-01 00:00:00	56240.5429050926	2012-11-09 13:01:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071251	Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy.	EXTRAGALACTIC COMPACT SOURCES	7	A	JON MILLER		USA	7	AO7	A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019030/	Quick Look
6	DA 240 EAST LOBE	117.3573	55.877	116.349381	56.002734	108.151975	34.146502	161.8466677	30.16323196	293.7777	55274.9306134259	2010-03-19 22:20:05	55276.7238657407	2010-03-21 17:22:22	704020010	81.7834	80	81.7834	81.7914	0	81.7914	2	2	0	2	1	0	0	74.3033	74.3033	154.9218	1	PROCESSED	57550.9753587963	2016-06-11 23:24:31	55654	2011-04-03 00:00:00	55286.3268518518	2010-03-31 07:50:40	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040096	Suzaku observations of two giant radio galaxies, 3C 35 and DA 240, with a total size of about 1 Mpc are proposed, in order to detect diffuse inverse Compton X-ray emission from their radio lobes. The X-ray flux from the lobes, in comparison with the radio one, provides a precise determination of electron and magnetic field energies there. A comparison of them with those in smaller radio galaxies is used to probe into the history of jets and lobes.	EXTRAGALACTIC COMPACT SOURCES	7	B	NAOKI ISOBE		JAP	4	AO4	SUZAKU OBSERVATION OF GIANT RADIO GALAXIES AS A PROBE OF JET HISTORY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704020010/	Quick Look
7	VII ZW 403	172.0164	79.0077	171.163549	79.283023	114.484764	62.884943	127.82558857	37.31615306	108.8488	56627.0107638889	2013-12-01 00:15:30	56628.7884027778	2013-12-02 18:55:18	708039010	88.6616	87	88.6616	88.6616	0	88.6616	2	2	0	2	1	0	0	87.3974	87.3974	153.5578	1	PROCESSED	57613.4969328704	2016-08-13 11:55:35	57008	2014-12-17 00:00:00	56639.6396990741	2013-12-13 15:21:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081443	The source of energetic photons that reionized the early universe remains uncertain. Recently, it has been proposed that X-ray binaries in early galaxies made a significant contribution to reionization. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectra with the Suzaku XIS. These observations are important to our understanding of reionization and the formation of early galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	C	PHILIP KAARET		USA	8	AO8	X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708039010/	Quick Look
8	3C 390.3	280.4556	79.7798	281.326844	79.727189	82.097994	76.490616	111.44649344	27.08887917	37.561	56436.3002777778	2013-05-24 07:12:24	56438.6036921296	2013-05-26 14:29:19	708034010	100.3668	100	100.3668	100.3668	0	100.3668	2	2	0	2	1	0	0	109.3267	109.3267	198.9817	3	PROCESSED	57611.4065740741	2016-08-11 09:45:28	56816	2014-06-08 00:00:00	56449.7081365741	2013-06-06 16:59:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081431	We propose simultaneous Suzaku (100 ks) and NuSTAR observations of the broad-line radio galaxy 3C 390.3, to measure Fe K-alpha emission and Compton reflection from the accretion disk. This is crucial for understanding the geometry of the accretion disk and its relation to the production of a powerful, relativistic radio jet. The combination of accurate Compton reflection parameters measured with NuSTAR and a simultaneous estimate of the accretion disk inner radius from Fe K-alpha with Suzaku will place strong constraints on accretion disk models for radio loud AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	B	PATRICK OGLE		USA	8	AO8	ACCRETION AND BLACK HOLE SPIN IN THE POWERFUL, RADIO-LOUD AGN 3C 390.3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708034010/	Quick Look
9	M82 X-1	149.1432	69.7042	148.108278	69.941832	119.044016	52.159559	141.33659361	40.60182861	163.0524	54367.135775463	2007-09-24 03:15:31	54367.8716898148	2007-09-24 20:55:14	702026010	35.5999	40	36.0319	35.5999	0	36.0239	2	2	0	2	1	0	0	30.4749	30.4749	63.5699	1	PROCESSED	57540.0638194444	2016-06-01 01:31:54	54770	2008-10-31 00:00:00	54402.2563657407	2007-10-29 06:09:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020092	We propose Suzaku observations of the intermediate-mass black hole candidate M82 X-1 for spectral study with a wide-band energy range including over 10 keV. In particular, the purpose is to determine a spectral cut-off energy in details in order to improve unified understanding of different mass black holes in comparison with those of stellar-mass black holes and ULXs in nearby galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	C	RYOHEI MIYAWAKI		JAP	2	AO2	HARD X-RAY SPECTRAL STUDY OF M82 X-1 WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702026010/	Quick Look
10	1H0323+342	51.1746	34.1741	50.388045	33.998103	57.519907	15.008853	155.73224486	-18.75935356	251.4848	56352.6173611111	2013-03-01 14:49:00	56354.8078819444	2013-03-03 19:23:21	707015010	101.272	100	101.288	101.272	0	101.288	2	2	0	2	1	0	0	97.1283	97.1283	189.2516	0	PROCESSED	57610.7547916667	2016-08-10 18:06:54	56739	2014-03-23 00:00:00	56372.5724189815	2013-03-21 13:44:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070088	We propose to observe a narrow-line radio-loud gamma-ray emitting Seyfert 1 galaxy 1H0323+342, which is the X-ray brightest among a new class of GeV gamma-ray emitting AGNs, first detected by Fermi/LAT. Based on accurate and high-sensitive measurement of X-ray spectra with Suzaku, we study the presence of Fe-K lines and energy-dependence of time variability, in order to constrain the origin of X-ray emission of this object. This leads to understanding the SED of this object and constraining the jet power.	EXTRAGALACTIC COMPACT SOURCES	7	C	YASUSHI FUKAZAWA		JAP	7	AO7	STUDY OF X-RAY SPECTRAL VARIABILITY OF A NARROW-LINE RADIO-LOUD GAMAM-RAY EMITTING SEYFERT 1 GALAXY 1H0323+342	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707015010/	Quick Look
11	SWIFT J1922.7-1716	290.6403	-17.2233	289.918336	-17.319807	289.738469	4.813727	20.73500926	-14.48356253	80.064	54198.231099537	2007-04-08 05:32:47	54200.4321643518	2007-04-10 10:22:19	702028010	78.6386	80	78.6386	78.6386	0	78.6386	2	2	0	2	1	0	0	61.3533	61.3533	190.1298	0	PROCESSED	57538.1728356482	2016-05-30 04:08:53	54744	2008-10-05 00:00:00	54206.3754166667	2007-04-16 09:00:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020097	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	2	AO2	BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702028010/	Quick Look
12	2MASX J15115979-2119	227.9997	-21.3083	227.279118	-21.120692	231.351076	-3.323732	341.57056512	30.81939061	105.6253	55979.0551388889	2012-02-22 01:19:24	55980.937650463	2012-02-23 22:30:13	706010010	83.8162	80	83.8162	83.8162	0	83.8162	2	2	0	2	1	0	0	82.2568	82.2568	162.6359	1	PROCESSED	57604.7185763889	2016-08-04 17:14:45	56361	2013-03-10 00:00:00	55995.1640393518	2012-03-09 03:56:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060032	We propose to observe two hard X-ray bright narrow-line Seyfert 1 galaxies, which are an important class of objects in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be a fundamental piece of information to better understand accretion physics and ``feedback'' processes in galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	6	AO6	ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED NARROW-LINE SEYFERT 1S	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706010010/	Quick Look
13	MARKARIAN 3	93.9187	71.0301	92.469282	71.045623	91.893166	47.615546	143.30552616	22.72176381	268.1895	57104.2423148148	2015-03-23 05:48:56	57104.6266550926	2015-03-23 15:02:23	709022040	23.518	20	23.518	23.526	0	23.526	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.8399305556	2016-08-17 20:09:30	57486	2016-04-08 00:00:00	57119.4206018518	2015-04-07 10:05:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092008	We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each.	EXTRAGALACTIC COMPACT SOURCES	7	A	MATTEO GUAINAZZI		EUR	9	AO9	MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022040/	Quick Look
14	PKS 1345+12	206.9131	12.3498	206.299989	12.598696	200.201065	21.844458	347.38894416	70.20282736	113.9421	54472.3082407407	2008-01-07 07:23:52	54473.6799768518	2008-01-08 16:19:10	702053010	52.9844	50	52.9844	52.9844	0	52.9844	2	2	0	2	1	0	0	45.2034	45.2034	118.5038	4	PROCESSED	57541.3141782407	2016-06-02 07:32:25	54854	2009-01-23 00:00:00	54483.4984375	2008-01-18 11:57:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021341	We wish to take advantage of the sensitivity of Suzaku above 10 keV to constrain the energy source -- starburst or black-hole driven activity -- in three of the brightest warm transitional ultraluminous infrared galaxies, PKS 1345+12, Mrk 463, and 3C 273. 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 time scale variability, another signature of black-hole driven activity. These data will be combined with our A01 spectra and be part of S. Teng's PhD thesis at UMD.	EXTRAGALACTIC COMPACT SOURCES	7	C	SYLVAIN VEILLEUX		USA	2	AO2	SPECTRA OF THE BRIGHTEST WARM ULTRALUMINOUS INFRARED GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702053010/	Quick Look
15	NGC 4593	189.915	-5.3482	189.270103	-5.073686	191.205514	-0.992169	297.48487911	57.39893055	292.7762	56824.1040972222	2014-06-16 02:29:54	56824.8563888889	2014-06-16 20:33:12	709014010	29.7616	30	29.7696	29.7616	0	29.7696	2	2	0	2	1	0	0	24.185	24.185	64.9919	1	PROCESSED	57615.2408449074	2016-08-15 05:46:49	57204	2015-07-01 00:00:00	56835.7291435185	2014-06-27 17:29:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090097	In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	9	AO9	X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014010/	Quick Look
16	AO 0235+164	39.665	16.613	38.972105	16.397631	42.455706	1.088366	156.77598662	-39.11106084	252.4352	56310.722337963	2013-01-18 17:20:10	56311.7418634259	2013-01-19 17:48:17	707021010	43.1028	40	43.1108	43.1188	0	43.1028	2	2	0	2	1	0	0	38.3583	38.3583	88.0698	0	PROCESSED	57608.5604166667	2016-08-08 13:27:00	56709	2014-02-21 00:00:00	56342.5387731482	2013-02-19 12:55:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071402	We request observations of the variable blazar AO 0235+164, to be conducted simultaneously with Fermi and optical and radio telescopes, towards a multi-band campaign. This object has complex X-ray spectrum due to absorption by an intervening galaxy, and Suzaku will be essential in unraveling the effects and composition of that absorber, and for the first time, provide a robust measurement of the underlying blazar X-ray continuum, which, together with the Swift UVOT spectrum, will allow to verify the signature of the bulk-Compton component, due to cold electrons propagating in the relativistic jet. At the highest priority, we request 40 ks for a precise spectral measurement; at a lower priority, we wish to monitor the source for the total of 5 days, with the request of additional 160 ks.	EXTRAGALACTIC COMPACT SOURCES	7	B	GRZEGORZ MADEJSKI		USA	7	AO7	SUZAKU OBSERVATIONS OF THE GAMMA-RAY BLAZAR AO 0235+164	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707021010/	Quick Look
17	NGC 5347	208.2716	33.4399	207.717601	33.685673	191.037943	41.510938	62.06849004	75.29189994	312.225	54627.6603703704	2008-06-10 15:50:56	54628.6064699074	2008-06-11 14:33:19	703011010	42.1611	40	42.1611	42.1611	0	42.1611	2	2	0	2	1	0	0	37.1302	37.1302	81.734	1	PROCESSED	57542.8072569444	2016-06-03 19:22:27	55008	2009-06-26 00:00:00	54637.3250810185	2008-06-20 07:48:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030040	We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	3	AO3	COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703011010/	Quick Look
18	MARKARIAN 79	115.6357	49.8015	114.696355	49.919868	108.437878	27.988088	168.6115046	28.38007803	283.4884	54193.9134953704	2007-04-03 21:55:26	54195.7655439815	2007-04-05 18:22:23	702044010	83.7038	82	83.7118	83.7038	0	83.7118	2	2	0	2	1	0	0	82.1042	82.1042	160.0059	0	PROCESSED	57538.0894444444	2016-05-30 02:08:48	54695	2008-08-17 00:00:00	54203.4223842593	2007-04-13 10:08:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021313	Recently, deep observations of a number of Seyfert AGN with XMM-Newton and Suzaku have established variable and relativistic iron lines as robust features in roughly half of all deep Seyfert spectra. In these sources, the spin of the black hole can be constrained directly through fits to the relativistic iron line. A sample of excellent spectra from well-chosen AGN will facilitate a better understanding of the innermost regime near to black holes, and make correlations with parameters like radio luminosity, star formation rate, and galaxy and black hole mass possible for the first time. We propose to obtain observations of 4 under-exposed Seyfert AGN with promising evidence for broad lines to robustly constrain their spin parameters.	EXTRAGALACTIC COMPACT SOURCES	7	B	JON MILLER		USA	2	AO2	REVEALING BLACK HOLE SPIN IN RELATIVISTIC SEYFERT AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702044010/	Quick Look
19	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
20	IRAS 00182-7112	5.1458	-70.9276	4.573856	-71.205097	312.979414	-61.496651	306.55074146	-45.98323945	33.8687	56050.171087963	2012-05-03 04:06:22	56052.8759143518	2012-05-05 21:01:19	707036010	93.959	90	93.967	93.959	0	93.959	2	2	0	2	1	0	0	86.5766	86.5766	233.6819	1	PROCESSED	57605.3998263889	2016-08-05 09:35:45	56435	2013-05-23 00:00:00	56068.6299537037	2012-05-21 15:07:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071441	We propose to observe with the Hard X-ray Detector onboard Suzaku the two Ultraluminous Infrared Galaxies IRAS 00182-7112 and IRAS 12127-1412, both of which are known to harbour very luminous and highly obscured active galactic nuclei (AGN). An AGN reflection component arising from ionized gas is clearly identified at 2 10 keV: the detection of the direct AGN emission above 10 keV and the measure of the reflection efficiency would provide fundamental information on both the physical structure of Compton-thick AGN embedded in a nuclear starburst and their feedback on the surrounding environment.	EXTRAGALACTIC COMPACT SOURCES	7	B	EMANUELE NARDINI		USA	7	AO7	THE PHYSICAL STRUCTURE OF COMPTON-THICK AGN/ULIRGS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707036010/	Quick Look
21	E1821+643	275.5207	64.3306	275.456094	64.303959	318.282096	86.807262	93.98984501	27.40177083	228.4067	56239.7868981482	2012-11-08 18:53:08	56241.8217708333	2012-11-10 19:43:21	707016010	100.4132	100	100.4132	100.4132	0	100.4132	2	2	0	2	1	0	0	95.5411	95.5411	175.7799	2	PROCESSED	57608.0299421296	2016-08-08 00:43:07	56631	2013-12-05 00:00:00	56265.6966319444	2012-12-04 16:43:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070089	Central engines of AGN are considered to be generally in Multi-Zone Comptonization (MZC) condition (e.g., Noda et al. 2011a,b). To verify this thing on a high-luminosiy AGN, we suggest to observe Radio-Quiet Quasar E1821+643 By Suzaku. Utilizing a time variability of each Comptonization component, we will resolve spectral variable components, and study whether the central engine of E1821+643 is in MZC condition or not.	EXTRAGALACTIC COMPACT SOURCES	7	C	HIROUMI NODA		JAP	7	AO7	SUZAKU STUDY OF MULTI-ZONE COMPTONIZATION PICTURE ON THE CENTRAL ENGINE OF RADIO-QUIET QUASAR E1821+643	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707016010/	Quick Look
22	SWIFT J1200.8+0650	180.2185	6.7488	179.57779	7.027186	177.502279	6.275772	270.13481807	66.34579154	293.0035	54617.9027662037	2008-05-31 21:39:59	54619.9280555556	2008-06-02 22:16:24	703009010	84.4866	80	84.5106	84.4866	0	84.5106	2	2	0	2	1	0	0	71.1109	71.1109	174.9638	3	PROCESSED	57542.752037037	2016-06-03 18:02:56	55003	2009-06-21 00:00:00	54634.1479282407	2008-06-17 03:33:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030034	The hard X-ray survey with Swift BAT have been finding various types of AGNs. Many buried AGNs with very low scattered X-rays have been discovered, for example. We propose to obtain broad band spectra of Compton-thin buried AGNs in the Swift sample. The data will be used to measure the amount of absoption in the direct and reflected emission and to constrain the structure of the obscuring matter around the AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	3	AO3	THE STRUCTURE OF BURIED COMPTON-THIN AGNS DISCOVERED BY SWIFT	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703009010/	Quick Look
23	J081618.99+482328.4	124.0768	48.3841	123.174595	48.53824	114.890427	27.844597	171.01809871	33.69777889	298.4793	54917.0925462963	2009-03-27 02:13:16	54919.0946643518	2009-03-29 02:16:19	703042010	90.9224	90	90.9224	90.9224	0	90.9224	2	2	0	2	1	0	0	81.0739	81.0739	172.9637	2	PROCESSED	57545.9726736111	2016-06-06 23:20:39	55329	2010-05-13 00:00:00	54930.3718055556	2009-04-09 08:55:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031337	We have discovered polar broad absorption-line quasars (BALQSOs) from their radio variabilities. We know their inclination angles. Our results derived from the archival Chandra data of one polar BALQSO indicate that the X-ray emissions are from the jet and the X-ray absorbing gas is located at tens of parsecs above the accretion disk corona. We want to confirm these results at high confidence level using better signal to noise ratio data from a big observatory, like SUZAKU. In addition, we propose to observe three more polar BALQSOs, which have wide range of radio/UV/X-ray properties. Our primary science goal of this proposal is to determine the radial distribution of the X-ray absorbing gas in 4 polar BALQSOs.	EXTRAGALACTIC COMPACT SOURCES	7	C	KAJAL GHOSH		USA	3	AO3	PROBING THE INNER STRUCTURE OF AGNS USING THE POLAR BALQSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703042010/	Quick Look
24	QSO 1222+216	186.229	21.3887	185.599657	21.665582	176.758525	22.008941	255.03812277	81.66761796	123.6044	56988.9003125	2014-11-27 21:36:27	56989.2953240741	2014-11-28 07:05:16	709025010	13.4002	15	0	0	0	13.4002	0	0	0	2	1	0	0	12.0474	12.0474	31.4359	0	PROCESSED	57617.406099537	2016-08-17 09:44:47	57368	2015-12-12 00:00:00	57002.0161111111	2014-12-11 00:23:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092023		EXTRAGALACTIC COMPACT SOURCES	7	C	MARCUS LANGEJAHN		EUR	9	AO9	false	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709025010/	Quick Look
25	EMS0857	198.1882	0.8497	197.548985	1.114667	196.443673	7.917565	314.828891	63.22804034	111.0249	55578.1935532407	2011-01-17 04:38:43	55578.746087963	2011-01-17 17:54:22	705011010	22.07	20	22.078	22.07	0	22.085	1	1	0	1	1	0	0	15.3267	15.3267	47.7279	0	PROCESSED	57600.6315046296	2016-07-31 15:09:22	55962	2012-02-05 00:00:00	55595.4732986111	2011-02-03 11:21:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050050	We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators".	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5	SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705011010/	Quick Look
26	3C454.3	343.4951	16.1379	342.877484	15.871411	351.362437	21.321746	86.10833014	-38.194784	252.9263	55525.0494675926	2010-11-25 01:11:14	55526.0141087963	2010-11-26 00:20:19	705021010	41.0252	40	41.0332	41.0332	0	41.0252	2	2	0	2	1	0	0	37.1412	37.1412	83.3278	0	PROCESSED	57554.2391319445	2016-06-15 05:44:21	55916	2011-12-21 00:00:00	55550.1355439815	2010-12-20 03:15:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050052	We propose 40 ksec x 2 (at most) Suzaku ToO observations - from a list of five -of GeV-bright flat spectrum radio quasars (FSRQs) that would be triggered by significant flaring (with E>100 MeV flux of 2x10^(-6) photons/cm^2/s or greater) in the Fermi all-sky monitoring. Those observations will be coordinated with optical and Swift XRT observations, with the goal of obtaining broadband spectra and light-curves during a flare gamma-ray activity. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the content and by extension, the accelertation process of the jet and energization of the radiating particles.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5-TOO	SUZAKU TOO OBSERVATION OF GIANT FLARE IN FRSQS TRIGGERED BY FERMI-LAT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705021010/	Quick Look
27	SMC X-1	19.2828	-73.4495	18.951598	-73.712645	312.330174	-66.477022	300.41169288	-43.55280074	39.2778	55706.0851851852	2011-05-25 02:02:40	55706.6745833333	2011-05-25 16:11:24	706030050	17.8463	18	17.8463	18.1823	0	18.1001	2	2	0	1	1	0	0	16.6829	16.6829	50.9139	0	PROCESSED	57602.111099537	2016-08-02 02:39:59	56092	2012-06-14 00:00:00	55725.1651736111	2011-06-13 03:57:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030050/	Quick Look
28	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
29	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
30	NGC 1365	53.3976	-36.1412	52.920229	-36.30818	36.797911	-53.03906	237.95777124	-54.60123537	60.7695	55392.8956597222	2010-07-15 21:29:45	55399.3676273148	2010-07-22 08:49:23	705031020	302.1753	450	302.1753	302.1833	0	302.1833	2	2	0	2	1	0	0	251.0612	251.0612	425.5339	2	PROCESSED	57552.8844791667	2016-06-13 21:13:39	55287	2010-04-01 00:00:00	55413.8216435185	2010-08-05 19:43:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051112	We propose 3 observations (~4 days each) of the Seyfert galaxy NGC 1365, at 2-week intervals. We aim to use eclipses to unambiguously identify the broad Fe K line, examine variability of the HXD/PIN excess, and to search for changes in the physical properties of the ionized absorber in this bright, nearby AGN. Shorter observations of this galaxy with XMM-Newton, Chandra and Suzaku showcase several remarkable physical traits: (1) FeXXV and FeXXVI K-shell absorption lines (the highest s/n detection so far among AGN), (2) rapidly varying cold absorption, (3) a highly significant relativistic Fe K emission line, and (4) a factor ~4 excess flux at high energies. The proposed observations will provide legacy spectra for what is arguably the single most physically-revealing obscured AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	LAURA BRENNEMAN		USA	5	AO5	A LONG LOOK AT NGC 1365: DISC TOMOGRAPHY, IONIZED ABSORPTION AND HIGH ENERGY EXCESS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705031020/	Quick Look
31	NGC 7130	327.065	-34.8962	326.317147	-35.128916	317.224283	-20.334869	10.02903365	-50.33744977	78.4767	54597.5198726852	2008-05-11 12:28:37	54598.56625	2008-05-12 13:35:24	703012010	44.4931	40	44.4931	44.4931	0	44.4931	1	1	0	1	1	0	0	36.7677	36.7677	90.3759	1	PROCESSED	57542.510474537	2016-06-03 12:15:05	54975	2009-05-24 00:00:00	54609.0170949074	2008-05-23 00:24:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030040	We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	3	AO3	COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703012010/	Quick Look
32	ESO 511-G030	214.8456	-26.6457	214.126189	-26.416188	221.40386	-12.022179	326.23004886	32.21661925	292.391	56156.7622337963	2012-08-17 18:17:37	56157.7960416667	2012-08-18 19:06:18	707023030	51.9172	270	51.9252	51.9252	0	51.9172	3	2	0	2	1	0	0	52.011	52.011	89.3158	3	PROCESSED	57606.8813194444	2016-08-06 21:09:06	56640	2013-12-14 00:00:00	56272.6998148148	2012-12-11 16:47:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071413	The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		USA	7	AO7	MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707023030/	Quick Look
33	SWIFT J2052.0-5704	312.9788	-57.0176	312.02055	-57.205734	297.951069	-37.67562	340.05945565	-38.72742848	73.9304	54945.6280671296	2009-04-24 15:04:25	54946.6863310185	2009-04-25 16:28:19	704010010	45.16	40	45.16	45.168	0	45.168	2	2	0	2	1	0	0	57.6242	57.6242	91.4098	1	PROCESSED	57546.2560416667	2016-06-07 06:08:42	55339	2010-05-23 00:00:00	54973.4487152778	2009-05-22 10:46:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040059	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	4	AO4	SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704010010/	Quick Look
34	SWIFT J1952.4+0237	298.0556	2.5705	297.425623	2.440903	300.700434	23.070542	42.31566647	-12.27488447	82.9116	54929.8284722222	2009-04-08 19:53:00	54931.1079166667	2009-04-10 02:35:24	704011010	47.9211	40	47.9259	47.9211	0	47.9259	2	2	0	2	1	0	0	39.3044	39.3044	110.5258	2	PROCESSED	57546.1208680556	2016-06-07 02:54:03	55324	2010-05-08 00:00:00	54949.4878356482	2009-04-28 11:42:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040059	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	4	AO4	SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704011010/	Quick Look
35	NGC1365	53.4052	-36.1452	52.927869	-36.31215	36.804669	-53.045157	237.96410536	-54.59489483	47.2005	56107.1526041667	2012-06-29 03:39:45	56107.9972916667	2012-06-29 23:56:06	707017010	30.6949	30	30.6949	30.6949	0	30.6949	2	2	0	2	1	0	0	27.8321	27.8321	72.9738	0	PROCESSED	57606.5279050926	2016-08-06 12:40:11	56491	2013-07-18 00:00:00	56125.2372453704	2012-07-17 05:41:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070095	NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. }	EXTRAGALACTIC COMPACT SOURCES	7	B	YASUSHI FUKAZAWA		JAP	7	AO7	MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017010/	Quick Look
36	NGC 3516	166.6957	72.5543	165.843141	72.824666	123.386475	57.973853	133.24670004	42.41457084	283.0856	56435.1473148148	2013-05-23 03:32:08	56436.2952199074	2013-05-24 07:05:07	708006070	51.4752	50	51.4772	51.4752	0	51.4792	2	2	0	2	1	0	0	53.7203	53.7203	99.1658	1	PROCESSED	57611.3639351852	2016-08-11 08:44:04	56383	2013-04-01 00:00:00	56449.6609027778	2013-06-06 15:51:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080066	We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	8	AO8	THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006070/	Quick Look
37	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
38	NGC 2992	146.4207	-14.2696	145.81924	-14.038457	154.003817	-26.061971	249.65504756	28.81616071	88.7924	53693.8781597222	2005-11-19 21:04:33	53694.9759722222	2005-11-20 23:25:24	700005020	37.4935	120	37.6565	39.6915	37.4935	37.8205	1	1	1	1	1	0	0	33.8991	33.8991	94.8479	1	PROCESSED	57528.0334490741	2016-05-20 00:48:10	54247	2007-05-27 00:00:00	54037.7316087963	2006-10-29 17:33:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001013	NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	0	SWG	THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005020/	Quick Look
39	3C 236 BACKGROUND	151.1488	34.7362	150.413548	34.979134	140.636655	21.408004	190.35215815	53.68789407	299.9977	56055.786712963	2012-05-08 18:52:52	56056.7919444444	2012-05-09 19:00:24	707006010	46.2113	40	46.2113	46.2113	0	46.2113	2	2	0	2	1	0	0	44.1095	44.1095	86.8399	0	PROCESSED	57605.3836574074	2016-08-05 09:12:28	56436	2013-05-24 00:00:00	56070.1639930556	2012-05-23 03:56:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070014	Through the Suzaku observations of giant radio galaxies, of which the size is larger than about 1 Mpc, we are going to reveal a picture that the jets in radio galaxies become inactive as they evolve from 500 kpc to 1 Mpc. However, the current Suzaku sample of the giant radio galaxies is far from being satisfactory to make a definite conclusion. Therefore, we propose a Suzaku observation of 3C 236, one of the most giant radio galaxy in the Universe.	EXTRAGALACTIC COMPACT SOURCES	7	A	NAOKI ISOBE		JAP	7	AO7	INVESTIGATION INTO EVOLUTION OF THE JET ENERGETICS, THROUGH THE SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 236	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707006010/	Quick Look
40	IRASF01475-0740	27.4875	-7.3766	26.863598	-7.624293	22.745573	-17.452267	160.69718538	-65.86110455	68.025	54661.0549652778	2008-07-14 01:19:09	54662.3023032407	2008-07-15 07:15:19	703065010	57.9147	50	57.9147	57.9183	0	57.9263	2	2	0	2	1	0	0	51.1257	51.1257	107.6988	0	PROCESSED	57543.0527546296	2016-06-04 01:15:58	55051	2009-08-08 00:00:00	54683.4056712963	2008-08-05 09:44:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032030	We propose 50ks observations of IRASF01475-0740 and NGC 3147, both of which are Seyfert 2s apparently unobscured in X-rays. Unsatisfied with this apparent contradiction, we seek Suzaku observations with two main aims. First, high energy observations with the HXD can reveal whether a deeply buried AGN is present above 10 keV. Second, the XIS observations will probe sensitively for short time-scale variability below 10 keV, the detection of which would establish unambiguously that the objects have genuinely unobscured nuclei and rule out the alternatives of scattered light or X-ray binaries.	EXTRAGALACTIC COMPACT SOURCES	7	A	KIRPAL NANDRA		EUR	3	AO3	SOLVING THE MYSTERY OF UNOBSCURED SEYFERT 2 GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703065010/	Quick Look
41	3C120	68.2993	5.3535	67.634764	5.249056	67.434072	-16.404208	190.3755878	-27.39480435	262.4873	53789.4598726852	2006-02-23 11:02:13	53790.8748958333	2006-02-24 20:59:51	700001030	40.9073	160	40.9073	40.9073	40.9073	40.9073	2	2	2	2	1	0	0	38.4817	38.4817	77.876	2	PROCESSED	57533.073900463	2016-05-25 01:46:25	54247	2007-05-27 00:00:00	54041.5149189815	2006-11-02 12:21:29	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001003	Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	0	SWG	BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001030/	Quick Look
42	MCG-6-30-15	203.9713	-34.2978	203.254904	-34.042659	215.172989	-22.546967	313.28925681	27.67845448	102.4359	53762.928275463	2006-01-27 22:16:43	53765.368275463	2006-01-30 08:50:19	700007030	96.6919	300	96.6919	96.6919	96.6999	96.6999	2	2	2	2	1	0	0	89.8194	89.8194	210.8019	5	PROCESSED	57532.8529861111	2016-05-24 20:28:18	54247	2007-05-27 00:00:00	54040.8156828704	2006-11-01 19:34:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001035	The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales .	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREW FABIAN		JAP	0	SWG	REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007030/	Quick Look
43	0836+714	130.267	70.829	129.006808	71.006559	109.318804	50.076677	143.62710847	34.4182022	294.8268	53809.7578125	2006-03-15 18:11:15	53810.5836111111	2006-03-16 14:00:24	700010010	55.6261	50	55.6341	55.6341	55.6261	55.6341	2	2	2	2	1	0	0	47.4058	47.4058	71.3419	1	PROCESSED	57533.2238541667	2016-05-25 05:22:21	54247	2007-05-27 00:00:00	54041.9651851852	2006-11-02 23:09:52	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001061	We propose two 50 ks observations, one for each of two EGRET blazars, 1510-089 (OR -017) and 0836+710 (4C +71.07). Both objects show extremely hard X-ray spectra, with photon indices about 1.3. The blazar 1510-089 ($z = 0.361$) is among a few OVV quasars showing prominent soft X-ray excess. The blazar 0836+710 ($z = 2.172)$ is the brightest X-ray source among the high redshift ($z>2$) quasars, and its very hard X-ray spectrum extends down to soft X-rays. Studying spectral shape and variability in the soft X-ray band relative to variability in the mid X-ray and optical bands can help to reveal nature of the soft X-ray excess of unknown origin, and multifrequency variability studies can provide constraints on the structure of jets on subparsec scales.	EXTRAGALACTIC COMPACT SOURCES	7	A	GREG MADEJSKI		JAP	0	SWG	TESTING THE SHOCK-IN-JET MODEL FOR NONTHERMAL FLARES IN BLAZARS VIA SUZAKU OBSERVATIONS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700010010/	Quick Look
44	SWIFT J0746.3+2548	116.6142	25.8792	115.852151	26.002245	113.853224	4.615293	194.5201067	22.91801121	97.0095	53678.357974537	2005-11-04 08:35:29	53680.5862847222	2005-11-06 14:04:15	700011010	99.4284	100	99.5235	100.4524	99.4284	99.7235	2	2	2	2	1	0	0	87.6995	87.6995	192.472	4	PROCESSED	57527.9575694445	2016-05-19 22:58:54	54247	2007-05-27 00:00:00	54037.5799074074	2006-10-29 13:55:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001087	Recently the BAT gamma-ray detector onboard Swift satellite has discovered very flat hard X-ray sources with photon index ~ 1.5 above 100 keV. The x-ray spectrum obtained with the XRT on Swiftis highly variable on time scales < 90 minutes. This variability and flat continuum spectrum suggests that this source is classified as a blazar. If this association is real, we have a precious chance to obtain spectrum upto several hundred keV in the source frame of the source. This wide range is of particularly importanceto study the blazar spectrum, or the electron distribution.	EXTRAGALACTIC COMPACT SOURCES	7	A	TADAYUKI TAKAHASHI		JAP	0	SWG	SUZAKU OBSERVATION OF A HIGH REDSHIFT BLAZAR RECENTLY DISCOVERED BY THE BAT ON SWIFT		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700011010/	Quick Look
45	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
46	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
47	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
48	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
49	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
50	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
51	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
52	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
53	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
54	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
55	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
56	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
57	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
58	OJ 287 FLARE	133.7115	20.1695	132.996174	20.360602	130.493887	2.661227	206.74425687	35.84822718	98.7868	54411.475	2007-11-07 11:24:00	54413.896099537	2007-11-09 21:30:23	702008010	112.044	100	112.052	112.06	0	112.044	2	2	0	2	1	0	0	102.9238	102.9238	209.1519	3	PROCESSED	57540.5116087963	2016-06-01 12:16:43	54791	2008-11-21 00:00:00	54423.3848032407	2007-11-19 09:14:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020024	OJ 287 is a promissing candidate of a suppermassive binary black hole, based on its periodic flare with a cycle of about 12 years. The next flare is predicted to take place on the fall, 2007. Therefore, two Suzaku exposures on OJ 287 is proposed, coordinated with radio, optical and very high energy gamma-ray observations. The first observation is on the spring to obtained the multi-wavelength spectrum of the target in its quiescent phase. The second is planned to be in a form of ToO observation on the fall, which will be triggered by an optical flare. The nature of the flare will be extensively investigated in these observatsions.	EXTRAGALACTIC COMPACT SOURCES	7	A	NAOKI ISOBE		JAP	2	AO2-TOO	MULTI-WAVELENGTH OBSERVATION OF PREDICTED FLARE OF SUPERMASSIVE BINARY BLACK HOLE CANDIDATE, OJ 287	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702008010/	Quick Look
59	IC 3639	190.1935	-36.8078	189.517353	-36.533453	205.04698	-29.556314	300.55692841	26.01476797	293.9494	54293.1966435185	2007-07-12 04:43:10	54294.4133564815	2007-07-13 09:55:14	702011010	53.3912	50	53.3912	53.3912	0	53.3912	2	2	0	2	1	0	0	48.4852	48.4852	105.11	1	PROCESSED	57539.1904050926	2016-05-31 04:34:11	54709	2008-08-31 00:00:00	54339.5331365741	2007-08-27 12:47:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020034	Seyfert 2 galaxies often have an nucleus obscured by thick matter. Risaliti et al. found that Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy s population by studying the distribution of absorbing column densities among Seyfert 2 galaxies. This result is important to discuss on the structure and evolution of active galactic nuclei. However, it is difficult to classify Seyfert 2 galaxies into Compton thick and thin objects only by using their X-ray spectra below 10 keV. Therefore, there may be Compton thin objects among Risaliti s Compton thick sample. In order to make the distribuion of the column density more reliable, we propose the Suzaku observations of heavily obscured AGNs with NH >1E25cm-2.	EXTRAGALACTIC COMPACT SOURCES	7	B	HISAMITSU AWAKI		JAP	2	AO2	SUZAKU OBSERVATIONS OF THE HEAVILY OBSCURED AGNS WITH NH>1E25 CM-2	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702011010/	Quick Look
60	NGC5548	214.4933	25.1285	213.926392	25.358693	201.994196	36.40686	31.9338138	70.49848107	305.6607	54289.4186921296	2007-07-08 10:02:55	54290.1182175926	2007-07-09 02:50:14	702042040	30.6996	30	30.6996	30.6996	0	30.6996	1	1	0	1	1	0	0	28.8279	28.8279	60.4319	1	PROCESSED	57539.1330324074	2016-05-31 03:11:34	54695	2008-08-17 00:00:00	54328.4843402778	2007-08-16 11:37:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021307	We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	2	AO2	NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042040/	Quick Look
61	NGC5548	214.4959	25.1277	213.928994	25.357885	201.997272	36.407089	31.932758	70.49602002	293.6791	54296.5817013889	2007-07-15 13:57:39	54297.4168865741	2007-07-16 10:00:19	702042050	30.0197	30	30.0277	30.0357	0	30.0197	2	2	0	2	1	0	0	26.3004	26.3004	58.971	1	PROCESSED	57539.274849537	2016-05-31 06:35:47	54707	2008-08-29 00:00:00	54340.3894328704	2007-08-28 09:20:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021307	We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	2	AO2	NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042050/	Quick Look
62	NGC5548	214.4979	25.1264	213.930994	25.35658	201.999984	36.406639	31.92993093	70.49400067	281.7605	54317.0262268518	2007-08-05 00:37:46	54318.0211111111	2007-08-06 00:30:24	702042080	38.7757	210	38.7837	38.7917	0	38.7757	1	1	0	1	1	0	0	32.6497	32.6497	85.9519	0	PROCESSED	57539.4187037037	2016-05-31 10:02:56	54714	2008-09-05 00:00:00	54347.3528472222	2007-09-04 08:28:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021307	We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	2	AO2	NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042080/	Quick Look
63	FAIRALL 9	20.9481	-58.8141	20.470954	-59.074601	340.57309	-59.156739	295.06951561	-57.81752905	48.1772	54258.155462963	2007-06-07 03:43:52	54260.5766666667	2007-06-09 13:50:24	702043010	167.7983	164	167.7983	167.8063	0	167.8143	2	2	0	2	1	0	0	136.4834	136.4834	209.1758	2	PROCESSED	57538.9238425926	2016-05-30 22:10:20	54773	2008-11-03 00:00:00	54265.5470717593	2007-06-14 13:07:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021313	Recently, deep observations of a number of Seyfert AGN with XMM-Newton and Suzaku have established variable and relativistic iron lines as robust features in roughly half of all deep Seyfert spectra. In these sources, the spin of the black hole can be constrained directly through fits to the relativistic iron line. A sample of excellent spectra from well-chosen AGN will facilitate a better understanding of the innermost regime near to black holes, and make correlations with parameters like radio luminosity, star formation rate, and galaxy and black hole mass possible for the first time. We propose to obtain observations of 4 under-exposed Seyfert AGN with promising evidence for broad lines to robustly constrain their spin parameters.	EXTRAGALACTIC COMPACT SOURCES	7	A	JON MILLER		USA	2	AO2	REVEALING BLACK HOLE SPIN IN RELATIVISTIC SEYFERT AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702043010/	Quick Look
64	NGC 1052	40.2309	-8.2134	39.616406	-8.42693	35.027708	-22.668341	181.91154484	-57.92833515	49.7745	54297.4313888889	2007-07-16 10:21:12	54299.87875	2007-07-18 21:05:24	702058010	100.6691	100	100.6691	100.6691	0	100.6691	2	2	0	2	1	0	0	83.4998	83.4998	211.4278	2	PROCESSED	57539.327037037	2016-05-31 07:50:56	54707	2008-08-29 00:00:00	54339.9136458333	2007-08-27 21:55:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021355	Accretion onto supermassive black holes is thought to play a major role in the production of relativistic jets. Our understanding of jet production remains elusive, however, because we cannot image the accretion flow. Fortunately, the Fe K line offers a direct probe of accretion. As part of a multi-mission monitoring program of the radio loud AGN NGC 1052, we propose two 100 ksec Suzaku observations to obtain best-quality X-ray spectra at two epochs to determine the true continuum shape and thus probe the relativistic iron line, determine line and continuum variability patterns and possibly investigate how the structure of the accretion disk changes when there are jet ejection events. Our aim is to determine what leads supermassive black holes to launch powerful jets.	EXTRAGALACTIC COMPACT SOURCES	7	A	KIMBERLY WEAVER		USA	2	AO2	PROBING THE DISK-JET CONNECTION IN AGN WITH AN INTENSIVE MULTIWAVELENGTH MONITORING CAMPAIGN OF NGC 1052	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702058010/	Quick Look
65	Q1946+7658	296.1546	77.0965	296.596903	76.972833	64.242641	76.919523	109.22346589	23.50098326	3.7704	54294.4255902778	2007-07-13 10:12:51	54294.6432175926	2007-07-13 15:26:14	702060010	13.1636	13	13.1636	13.1636	0	13.1636	1	1	0	1	1	0	0	13.9282	13.9282	18.7759	0	PROCESSED	57539.2591782407	2016-05-31 06:13:13	54706	2008-08-28 00:00:00	54339.4067824074	2007-08-27 09:45:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021361	The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars.	EXTRAGALACTIC COMPACT SOURCES	7	C	GEORGE CHARTAS		USA	2	AO2	AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702060010/	Quick Look
66	Q1334-0033	204.1954	-0.819	203.55335	-0.564423	202.702904	8.620784	326.07775276	59.99926461	306.9566	54295.3551736111	2007-07-14 08:31:27	54295.7084953704	2007-07-14 17:00:14	702067010	13.9621	15	13.9621	13.9621	0	13.9621	1	1	0	1	1	0	0	13.0064	13.0064	30.5199	0	PROCESSED	57539.262337963	2016-05-31 06:17:46	54710	2008-09-01 00:00:00	54340.4777430556	2007-08-28 11:27:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021361	The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars.	EXTRAGALACTIC COMPACT SOURCES	7	C	GEORGE CHARTAS		USA	2	AO2	AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702067010/	Quick Look
67	Q1548+0917	237.6002	9.1581	236.997547	9.308492	232.970531	28.527987	18.5566992	44.16075413	106.1242	54513.4560763889	2008-02-17 10:56:45	54514.16	2008-02-18 03:50:24	702068010	32.1133	23	32.1213	32.1213	0	32.1133	1	1	0	1	1	0	0	29.4756	29.4756	60.8159	0	PROCESSED	57541.5745601852	2016-06-02 13:47:22	54889	2009-02-27 00:00:00	54522.1462731482	2008-02-26 03:30:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021361	The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars.	EXTRAGALACTIC COMPACT SOURCES	7	C	GEORGE CHARTAS		USA	2	AO2	AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702068010/	Quick Look
68	MRK 417	162.3659	22.9016	161.688757	23.166381	154.921054	14.241178	214.84390845	62.11471123	281.9359	54238.6593402778	2007-05-18 15:49:27	54239.5730555556	2007-05-19 13:45:12	702078010	41.5066	40	41.5066	41.5066	0	41.5066	2	2	0	2	1	0	0	39.3385	39.3385	78.9239	0	PROCESSED	57538.6952662037	2016-05-30 16:41:11	54695	2008-08-17 00:00:00	54245.0002430556	2007-05-25 00:00:21	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021374	Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702078010/	Quick Look
69	NGC 1142	43.7827	-0.1295	43.142852	-0.331581	41.283841	-16.101856	175.79604248	-49.86350093	73.9096	54302.4506481482	2007-07-21 10:48:56	54303.4308333333	2007-07-22 10:20:24	702079010	40.5697	40	40.5697	40.5697	0	40.5697	2	2	0	2	1	0	0	36.5404	36.5404	84.6799	1	PROCESSED	57539.2980902778	2016-05-31 07:09:15	54706	2008-08-28 00:00:00	54339.1106828704	2007-08-27 02:39:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021374	Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702079010/	Quick Look
70	MCG +04-48-002	307.1488	25.8021	306.615298	25.635019	318.241154	43.22286	67.06317106	-7.53431612	93.9583	54208.4668634259	2007-04-18 11:12:17	54209.4134143518	2007-04-19 09:55:19	702081010	41.2988	40	41.3068	41.2988	0	41.3068	2	2	0	2	1	0	0	37.7466	37.7466	81.7699	2	PROCESSED	57538.398275463	2016-05-30 09:33:31	54695	2008-08-17 00:00:00	54217.0231712963	2007-04-27 00:33:22	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021374	Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702081010/	Quick Look
71	TYPE2AGN	216.4026	35.2819	215.878545	35.506676	198.09088	46.269263	60.85487771	68.34395808	307.3753	54292.1781712963	2007-07-11 04:16:34	54292.6183333333	2007-07-11 14:50:24	702090010	19.8387	19	19.8467	19.8547	0	19.8387	2	2	0	2	1	0	0	20.87	20.87	38.0159	0	PROCESSED	57539.1533912037	2016-05-31 03:40:53	54706	2008-08-28 00:00:00	54339.0120833333	2007-08-27 00:17:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021376	We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs.	EXTRAGALACTIC COMPACT SOURCES	7	C	CHRISTINE JONES		USA	2	AO2	OBSCURED AGN AND XBONGS IN BOOTES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702090010/	Quick Look
72	IC4329A	207.3319	-30.3107	206.617741	-30.062544	216.345447	-17.778019	317.49747069	30.91844112	292.4395	54313.2280092593	2007-08-01 05:28:20	54314.0419444444	2007-08-02 01:00:24	702113010	25.4534	25	25.4534	25.4534	0	25.4534	2	2	0	2	1	0	0	21.4422	21.4422	70.292	1	PROCESSED	57539.3768287037	2016-05-31 09:02:38	54710	2008-09-01 00:00:00	54340.5826273148	2007-08-28 13:58:59	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022009	IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASSIMO CAPPI		EUR	2	AO2	SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113010/	Quick Look
73	IC4329A	207.3317	-30.3084	206.617549	-30.060244	216.344382	-17.775948	317.49797139	30.92070724	297.0437	54328.4922106482	2007-08-16 11:48:47	54329.1612731482	2007-08-17 03:52:14	702113040	24.2194	25	24.2194	24.2194	0	24.2194	2	2	0	2	1	0	0	20.2031	20.2031	57.8	1	PROCESSED	57539.604537037	2016-05-31 14:30:32	54730	2008-09-21 00:00:00	54351.1843171296	2007-09-08 04:25:25	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022009	IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASSIMO CAPPI		EUR	2	AO2	SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113040/	Quick Look
74	IRAS 10565+2448	164.8573	24.5988	164.182449	24.867063	156.396321	16.702388	212.34078465	64.72788111	119.4619	54410.6325	2007-11-06 15:10:48	54411.4675347222	2007-11-07 11:13:15	702115010	39.4232	30	39.4232	39.4232	0	39.4232	2	2	0	2	1	0	0	35.7388	35.7388	72.1459	0	PROCESSED	57540.4702893518	2016-06-01 11:17:13	54791	2008-11-21 00:00:00	54423.1618518518	2007-11-19 03:53:04	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022023	We propose for 30ks Suzaku observations of two ultra-luminous infrared galaxies that lack sensitive 2keV constraints to provide a complete census of Active Galactic Nuclei (AGN) activity in ULIRGs out to 200Mpc. Six (~75%) of the eight ULIRGs in our sample for which we already have sensitive >2keV constraints host AGN activity, indicating that black-hole growth is ubiqitious in the most luminous local galaxies. Our proposed observations are sensitive enough to identify luminous AGN activity (L_X=3x10^{43} erg/s) out to ~40keV, to accurately quantify the properties of less luminous AGN activity, and to identify and quantify the star-formation activity. In addition the results will be used to better understand the z~2 ULIRG population, the likely progenitors of todays massive galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	C	DAVID ALEXANDER		EUR	2	AO2	A COMPLETE CENSUS OF AGN ACTIVITY IN ULTRA-LUMINOUS GALAXIES OUT TO 200 MPC	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702115010/	Quick Look
75	AKN 564	340.6246	29.7785	340.037211	29.516371	355.343017	34.767845	92.13720271	-25.27363853	56.6178	54277.5375694444	2007-06-26 12:54:06	54279.8002199074	2007-06-28 19:12:19	702117010	99.9781	100	99.9861	99.9861	0	99.9781	2	2	0	2	1	0	0	87.2253	87.2253	195.4739	1	PROCESSED	57539.0843518518	2016-05-31 02:01:28	54703	2008-08-25 00:00:00	54333.5152199074	2007-08-21 12:21:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022024	Narrow Line Seyfert 1 galaxies show complex X-ray behaviour. At low flux levels their 2-10~keV spectra are hard, with a huge excess at lower energies. Conversely, at high fluxes, the same objects show a soft 2-10 keV spectrum, with moderate soft excess. This behaviour can be explained either by reflection or absorption models. It is important to distinguish between these scenarios as they imply critical differences in the inferred physics of the accretion flow. There is already good Suzaku data on the hard 2-10 keV spectra from a GT observation of NGC4051. We propose to compare this with 100ks of data from Akn564, the brightest NLS1 at 10keV having a soft 2-10keV spectrum, so as to use the full range of spectral behaviour seen in NLS1's to determine the origin of the soft excess.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRIS DONE		EUR	2	AO2	UNDERSTANDING THE ORIGIN OF SPECTRAL COMPLEXITY IN NLS1: AKN564	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702117010/	Quick Look
76	ESO 323-G032	193.3499	-41.5832	192.653913	-41.311875	210.129179	-32.696187	303.32560645	21.28704922	104.5857	54456.5856481482	2007-12-22 14:03:20	54458.1459953704	2007-12-24 03:30:14	702119010	79.2494	80	80.8178	79.2494	0	80.8014	2	2	0	2	1	0	0	86.8967	86.8967	134.7778	1	PROCESSED	57540.9568055556	2016-06-01 22:57:48	54854	2009-01-23 00:00:00	54483.1116203704	2008-01-18 02:40:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022033	The high-energy detectors onboard Swift and INTEGRAL are mapping the hard (>10 keV) X-ray sky. Although limited to bright X-ray fluxes (~1e-11 erg/cm2/s), the large area surveyed so far has allowed to build up sizable samples of hard X-ray selected AGN almost unbiased against X-ray absorption. On the basis of a careful analysis of the available X-ray observations below 10 keV, we identified a sample of relatively bright AGN which are likely to be obscured by Compton-thick (logN_H >24) cold gas. Two of them were observed in EAO-1 and the results confirmed our predictions. We propose further Suzaku observations of 3 bright objects (F(20-40 keV) ~ 0.7-1.4 x 1e-11 erg/cm2/s) which will allow us to unveil previously unknown nearby heavily obscured AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREA COMASTRI		EUR	2	AO2	BRIGHT COMPTON-THICK GALAXIES IN THE BACKYARD - PART II	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702119010/	Quick Look
77	PKS2126-15	322.2988	-15.6437	321.609655	-15.862975	319.629627	-0.752825	35.92993079	-41.86589251	72.3882	54576.0912384259	2008-04-20 02:11:23	54578.4238310185	2008-04-22 10:10:19	703001010	81.9214	80	81.9214	81.9364	0	81.9454	2	2	0	2	1	0	0	71.5414	71.5414	201.5279	3	PROCESSED	57542.3941087963	2016-06-03 09:27:31	54961	2009-05-10 00:00:00	54594.3427777778	2008-05-08 08:13:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030003	We propose intensive Suzaku observations (80ksec each) of two "primitive" blazars at z > 3.3, with a highly unusual SED. ROXA J081009.9 (z=4.0) was recently found by a short Swift/XRT exposure (6 ksec) with a luminosity well in excess of 10^47 ergs/s, but its synchrotron power peaking above 10 keV. This may suggest the bulk Lorentz factor of the jet could reach ~1000 like GRBs, though quite conspicuous among the AGN jets. Meanwhile, unusual SED of PKS2126-15 (z=3.3) , where the synchrotron peaking at GHz and the inverse Compton peaks at ~10 keV, is most likely due to the presence of ultra-massive black hole with 2x10^10 Ms. These new-types are only found in highly distant universe, and maybe categorized as primitive blazars.	EXTRAGALACTIC COMPACT SOURCES	7	B	JUN KATAOKA		JAP	3	AO3	UNVEILING NEW-TYPE "PRIMITIVE" BLAZARS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703001010/	Quick Look
78	SWIFT J2009.0-6103	302.158	-61.0495	301.087298	-61.195509	289.575526	-39.777943	335.84532046	-32.77756596	73.0628	54563.6948148148	2008-04-07 16:40:32	54564.600775463	2008-04-08 14:25:07	703015010	43.7268	40	43.7268	43.7268	0	43.7268	2	2	0	2	1	0	0	36.1996	36.1996	78.268	1	PROCESSED	57542.2661342593	2016-06-03 06:23:14	54953	2009-05-02 00:00:00	54580.2454976852	2008-04-24 05:53:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030045	Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	3	AO3	DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703015010/	Quick Look
79	NGC3227	155.8768	19.8688	155.194236	20.122176	150.387557	9.143202	216.98485011	55.4460253	111.8565	54790.7083333333	2008-11-20 17:00:00	54792.374525463	2008-11-22 08:59:19	703022040	64.5679	50	64.5759	64.5679	0	64.5759	2	2	0	2	1	0	0	46.622	46.622	143.9478	1	PROCESSED	57544.506412037	2016-06-05 12:09:14	54557	2008-04-01 00:00:00	54812.4380324074	2008-12-12 10:30:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031013	We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	3	AO3	NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022040/	Quick Look
80	NGC3227	155.8768	19.8687	155.194236	20.122076	150.387594	9.143109	216.98501654	55.44599229	109.926	54802.6028125	2008-12-02 14:28:03	54803.7231365741	2008-12-03 17:21:19	703022060	51.4105	50	51.4105	51.4105	0	51.4105	2	2	0	2	1	0	0	39.6836	39.6836	96.7818	1	PROCESSED	57544.6321875	2016-06-05 15:10:21	54557	2008-04-01 00:00:00	54812.4432407407	2008-12-12 10:38:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031013	We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	3	AO3	NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022060/	Quick Look
81	SN 2006JD	120.5331	0.8102	119.888824	0.950282	122.553341	-19.245849	220.45612728	16.05834455	284.354	54578.4377777778	2008-04-22 10:30:24	54579.6807175926	2008-04-23 16:20:14	703026010	54.1968	50	54.2048	54.1968	0	54.2048	2	2	0	2	1	0	0	52.0488	52.0488	107.3398	1	PROCESSED	57542.379837963	2016-06-03 09:06:58	54957	2009-05-06 00:00:00	54588.1523611111	2008-05-02 03:39:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031241	Supernovae (SNe) 2005kd and 2006jd are some of the brightest SNe ever detected in X-rays. The high X-ray luminosities (>E41 erg/s) are the results of the SN shock interacting with dense material in the environment of the SNe. We propose one Suzaku observation of each SN to obtain high-quality spectra that will be used to measure the temperature of the forward and reverse shock and to establish the rate of decline in comparison with existing Swift, Chandra and XMM-Newton data. The data will further be used to measure the circumstellar matter density and mass-loss rate of the progenitors to probe the nature of the SN progenitors. Our science objectives rely on Suzaku's uniqueness, i.e. the large collecting area, good spectral resolution, and the high sensitivity in the hard X-ray band.	EXTRAGALACTIC COMPACT SOURCES	7	B	STEFAN IMMLER		USA	3	AO3	SUZAKU OBSERVATIONS OF X-RAY BRIGHT SUPERNOVAE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703026010/	Quick Look
82	ESO 103- G 035	279.5941	-65.4238	278.351287	-65.467222	275.354112	-42.161198	329.78379096	-23.17817546	291.5832	54761.6331597222	2008-10-22 15:11:45	54764.1717476852	2008-10-25 04:07:19	703031010	91.442	80	91.442	91.45	0	91.45	2	2	0	2	1	0	0	81.0096	81.0096	219.282	2	PROCESSED	57544.3339467593	2016-06-05 08:00:53	55148	2009-11-13 00:00:00	54782.4220023148	2008-11-12 10:07:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031322	X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s.	EXTRAGALACTIC COMPACT SOURCES	7	B	VALENTINA BRAITO		USA	3	AO3	THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703031010/	Quick Look
83	Q0551-3637	88.2027	-36.6207	87.768974	-36.630505	87.117827	-60.044705	242.37463259	-26.91966553	321.5977	54600.5596643518	2008-05-14 13:25:55	54601.2044444444	2008-05-15 04:54:24	703036020	21.6143	22	21.6143	21.6143	0	21.6183	2	2	0	2	1	0	0	18.2831	18.2831	55.684	1	PROCESSED	57542.5389236111	2016-06-03 12:56:03	54979	2009-05-28 00:00:00	54613.0157060185	2008-05-27 00:22:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031334	Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	3	AO3	A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703036020/	Quick Look
84	Q0329-385	52.7815	-38.4067	52.316664	-38.576045	34.470474	-54.910107	241.941352	-54.89845774	23.7676	54633.4249421296	2008-06-16 10:11:55	54634.1898611111	2008-06-17 04:33:24	703038010	30.203	29	30.219	30.203	0	30.219	2	2	0	2	1	0	0	25.2925	25.2925	66.082	1	PROCESSED	57542.8370601852	2016-06-03 20:05:22	55010	2009-06-28 00:00:00	54644.1762615741	2008-06-27 04:13:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031334	Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	3	AO3	A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703038010/	Quick Look
85	1ES1426+428	217.0602	42.6327	216.573667	42.855515	193.163684	52.913705	77.47261603	64.96709047	324.5702	54622.8702662037	2008-06-05 20:53:11	54625.0856944444	2008-06-08 02:03:24	703063010	101.1662	100	101.1662	101.1742	0	101.1742	2	2	0	2	1	0	0	92.1456	92.1456	191.3937	3	PROCESSED	57542.7937731482	2016-06-03 19:03:02	55003	2009-06-21 00:00:00	54636.5084953704	2008-06-19 12:12:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032021	Simultaneous optical/UV, X-ray and TeV observations are a powerful tool to study the innermost regions of blazar jets, probing the physical state of the jet close to its base. We propose to perform a long SUZAKU observation of the extreme hard-X-ray blazar 1ES 1426+428, simultaneously with MAGIC TeV observations, combined with a series of short Swift observations. With SUZAKU we will study the evolution of the X-ray emission over timescales of minutes-hours, providing important insight into the structure of the emission region and the physical process producing the radiation. We will characterize the synchrotron part of the SED and see how it correlates with the TeV spectrum, disentangling the main physical parameters and probing the still poorly known cosmic IR background.	EXTRAGALACTIC COMPACT SOURCES	7	A	GIANPIERO TAGLIAFERRI		EUR	3	AO3	THE EXTREME BLAZAR 1ES 1426+428: TESTING THE JET	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703063010/	Quick Look
86	1739+518	264.9784	52.1719	264.694846	52.196929	257.680013	75.396251	79.52646168	31.85370007	22.9152	54985.7571759259	2009-06-03 18:10:20	54986.3641087963	2009-06-04 08:44:19	704008010	22.4868	20	22.4948	22.4948	0	22.4868	2	2	0	2	1	0	0	28.2378	28.2378	52.4319	0	PROCESSED	57547.4536458333	2016-06-08 10:53:15	55367	2010-06-20 00:00:00	54998.1968634259	2009-06-16 04:43:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040049	We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	4	AO4	SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704008010/	Quick Look
87	CENTAURUS_A	201.3322	-43.0688	200.598815	-42.808768	217.137097	-31.383435	309.48334217	19.37141452	298.7164	55048.3079513889	2009-08-05 07:23:27	55049.7029398148	2009-08-06 16:52:14	704018020	51.2787	50	51.2787	51.2947	0	51.2867	2	2	0	2	1	0	0	43.7332	43.7332	120.5059	1	PROCESSED	57548.0839699074	2016-06-09 02:00:55	55430	2010-08-22 00:00:00	55062.3520023148	2009-08-19 08:26:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040085	We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku.	EXTRAGALACTIC COMPACT SOURCES	7	A	YASUSHI FUKAZAWA		JAP	4	AO4	SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704018020/	Quick Look
88	ESO 548-G081	55.4927	-21.1949	54.941134	-21.353755	46.730142	-39.596754	213.74761618	-50.8353425	69.3236	55046.3350462963	2009-08-03 08:02:28	55047.1946064815	2009-08-04 04:40:14	704026010	39.4112	40	39.4192	39.4192	0	39.4112	2	2	0	2	1	0	0	36.1429	36.1429	74.2599	0	PROCESSED	57548.0531481482	2016-06-09 01:16:32	55427	2010-08-19 00:00:00	55060.8071875	2009-08-17 19:22:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041402	The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples.	EXTRAGALACTIC COMPACT SOURCES	7	B	LISA WINTER		USA	4	AO4	SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704026010/	Quick Look
89	MCG +04-22-042	140.9461	22.9693	140.230202	23.184366	136.125191	7.311314	205.9821846	43.11036681	106.3587	55157.3309259259	2009-11-22 07:56:32	55158.2634143518	2009-11-23 06:19:19	704028010	40.962	40	40.994	40.962	0	40.986	1	1	0	1	1	0	0	35.8969	35.8969	80.5599	0	PROCESSED	57549.5187384259	2016-06-10 12:26:59	55542	2010-12-12 00:00:00	55176.1858101852	2009-12-11 04:27:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041402	The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples.	EXTRAGALACTIC COMPACT SOURCES	7	B	LISA WINTER		USA	4	AO4	SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704028010/	Quick Look
90	1H0323+342	51.1507	34.2411	50.363828	34.065013	57.518057	15.07869	155.67406743	-18.71640786	76.7168	55038.1604513889	2009-07-26 03:51:03	55040.2084722222	2009-07-28 05:00:12	704034010	84.0884	80	84.0884	84.2404	0	84.3524	2	2	0	2	1	0	0	74.2979	74.2979	176.9379	0	PROCESSED	57548.0010532407	2016-06-09 00:01:31	55419	2010-08-11 00:00:00	55050.8162847222	2009-08-07 19:35:27	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041408	Recent radio observations reveal blazar-like properties in some radio-loud narrow line Seyfert-1 AGNs. 1H0323+342, classified as this class of AGNs, shows prominent hard X-ray emission with a hard photon index. Since the spectrum in hard X-ray is reminiscent of blazar, its X-ray spectrum seems to have different components originated from disk and jet. Thanks to sensitive X-ray detectors extending to the hard X-ray band, Suzaku observation is expected to resolve a possible multi-component structure in the spectrum. Since beamed radiation from jet is highly variable, spectral temporal behavior is also vital information to distinguish the emission origin. As this source is located relatively nearby (z=0.061), the source is an excellent target to investigate the emission from disk and jet.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASAAKI HAYASHIDA		USA	4	AO4	SUZAKU OBSERVATION OF 1H0323+342: A PECULIAR SEYFERT-1 --PROBING THE DISK AND JET CONNECTION IN AGN--	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704034010/	Quick Look
91	MCG0208	43.0963	-8.5129	42.484335	-8.717227	37.842662	-23.868775	185.55840319	-55.88722126	57.4541	55016.0987037037	2009-07-04 02:22:08	55017.2134722222	2009-07-05 05:07:24	704045010	42.9115	40	42.9435	42.9115	0	42.9195	2	2	0	2	1	0	0	36.7878	36.7878	96.286	5	PROCESSED	57547.7724768518	2016-06-08 18:32:22	55395	2010-07-18 00:00:00	55027.1160532407	2009-07-15 02:47:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041414	We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc.	EXTRAGALACTIC COMPACT SOURCES	7	A	EZEQUIEL TREISTER		USA	4	AO4	THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704045010/	Quick Look
92	SDSS J1352+4239	208.1832	42.6476	207.663098	42.893525	184.337785	49.439251	88.11360974	70.09649039	316.6443	54984.9959375	2009-06-02 23:54:09	54985.7502199074	2009-06-03 18:00:19	704050010	32.0745	30	32.0825	32.0745	0	32.0825	2	2	0	2	1	0	0	29.5021	29.5021	65.1639	0	PROCESSED	57547.4324652778	2016-06-08 10:22:45	55364	2010-06-17 00:00:00	54994.4273032407	2009-06-12 10:15:19	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041422	BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction.	EXTRAGALACTIC COMPACT SOURCES	7	A	XINYU DAI		USA	4	AO4	X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704050010/	Quick Look
93	SDSS J0943+5417	145.8252	54.2751	144.963883	54.504193	127.754031	37.9036	161.23003018	46.41565232	274.2141	54975.5889236111	2009-05-24 14:08:03	54976.3473611111	2009-05-25 08:20:12	704052010	34.2264	30	34.2264	34.2264	0	34.2264	2	2	0	2	1	0	0	32.0591	32.0591	65.5179	2	PROCESSED	57546.6638773148	2016-06-07 15:55:59	55358	2010-06-11 00:00:00	54992.6588888889	2009-06-10 15:48:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041422	BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction.	EXTRAGALACTIC COMPACT SOURCES	7	A	XINYU DAI		USA	4	AO4	X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704052010/	Quick Look
94	MR 2251-178	343.5217	-17.5814	342.855263	-17.84794	338.051604	-9.763358	46.19628588	-61.32288878	63.4108	54958.1447222222	2009-05-07 03:28:24	54961.4675231482	2009-05-10 11:13:14	704055010	136.924	130	136.932	136.924	0	136.9399	2	2	0	2	1	0	0	112.1637	112.1637	287.0576	2	PROCESSED	57546.6278009259	2016-06-07 15:04:02	55343	2010-05-27 00:00:00	54976.3091782407	2009-05-25 07:25:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042002	The bright, nearby (z=0.06398) QSO MR 2251-178 was the first AGN where a warm absorber was detected. There are now thought to be at least two warm absorber components in MR 2251-178; a low ionisation soft X-ray absorber and a putative high velocity (13000 km/s) high ionisation wind, which exhibits absorption lines in the iron K-shell band. We propose a 130 ks observation with Suzaku of MR 2251-178 with the primary goals; (i) to establish the nature of the high ionisation absorber, e.g. an accretion disk wind, through unprecedented high S/N observations in the iron K band with XIS; (ii) to determine the physical parameters of the soft X-ray warm absorber and (iii) to characterise the ionised reflection component and high-energy cut-off thanks to the high energy sensitivity of the HXD.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES	YASUSHI FUKAZAWA	EUR	4	AO4	PROBING THE OUTFLOWING WIND IN MR 2251-178	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704055010/	Quick Look
95	IRAS 04507+0358	73.3635	4.1233	72.703908	4.042054	72.49644	-18.313087	194.58361833	-23.84576016	98.871	55075.0228356482	2009-09-01 00:32:53	55078.1356481482	2009-09-04 03:15:20	704058010	109.0524	100	109.0524	109.0524	0	109.0524	2	2	0	2	1	0	0	84.1098	84.1098	268.9118	3	PROCESSED	57548.5242939815	2016-06-09 12:34:59	55476	2010-10-07 00:00:00	55109.5623842593	2009-10-05 13:29:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042022	According to X-ray synthesis models, Compton-thick AGN (NH>1e24 cm-2) should represent 50% of the total absorbed AGN population. Despite their importance in the cosmological context, only a few of them have been found so far. We have selected a well-defined sample of 31 Compton-thick candidates on the basis on their FX/FIR and X-ray colors. Due to the heavy obscuration, data above 10 keV are fundamental to unveil these sources. We ask here deep Suzaku observations (100 ks on each source) for 2 sources of our sample for which data at energy >10keV are not available yet. These observations will allow to complete the physical characterization (NH and LX) of the bright tail (F(2-10 keV)>5e-12 cgs) of our sample and to add more information to test the prediction of the AGN synthesis model.	EXTRAGALACTIC COMPACT SOURCES	7	B	PAOLA SEVERGNINI		EUR	4	AO4	SUZAKU OBSERVATIONS OF COMPTON-THICK CANDIDATES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704058010/	Quick Look
96	IGR J22517+2218	342.9769	22.2871	342.369941	22.021351	353.695074	27.113044	89.68946946	-32.75751552	253.7359	55161.7610648148	2009-11-26 18:15:56	55163.0086111111	2009-11-28 00:12:24	704060010	52.7265	50	52.7265	52.7265	0	52.7265	2	2	0	2	1	0	0	40.1164	40.1164	107.7779	0	PROCESSED	57549.6312152778	2016-06-10 15:08:57	55545	2010-12-15 00:00:00	55179.2471527778	2009-12-14 05:55:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042027	We propose to observe 4 high-z QSOs observed by INTEGRAL, two of which are newly discovered in hard X-rays. The broadband and the good energy resolution will allow to investigate the spectral behaviour at low energies, and in particular to constraint true absorption $vs$ continuum features scenario. Particularly intriguing is the possible presence of a bulk Compton motion component. A self consistent test of this model could be derived by measuring the peak energy of the Inverse Compton component in the SED, a requirement that further strenghtens the need of a broadband observation with Suzaku. Simultaneous optical, hard X and gamma-ray observations available through WEBT, INTEGRAL and AGILE will also improve the feasibility of the proposed program.	EXTRAGALACTIC COMPACT SOURCES	7	B	ALESSANDRA DE ROSA		EUR	4	AO4	SUZAKU OBSERVATION A SAMPLE OF FOUR RADIO-LOUD/HIGH REDSHIFT QSOS OBSERVED BY INTEGRAL	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704060010/	Quick Look
97	NGC3783	174.7201	-37.7846	174.100385	-37.507469	192.672057	-36.228861	287.44066962	22.89477473	305.9228	55022.9100115741	2009-07-10 21:50:25	55027.0016087963	2009-07-15 00:02:19	704063010	209.5034	200	209.5034	210.3114	0	210.3194	3	2	0	2	1	0	0	174.0404	174.0404	353.4535	2	PROCESSED	57547.9411342593	2016-06-08 22:35:14	54922	2009-04-01 00:00:00	55040.5612615741	2009-07-28 13:28:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046003	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	4	AO4	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704063010/	Quick Look
98	PBC J0216.1+5124	34.0954	51.5104	33.261431	51.278784	50.779826	35.406451	136.13174863	-9.17115539	78.3815	55421.9728356482	2010-08-13 23:20:53	55423.4168171296	2010-08-15 10:00:13	705006010	72.7733	80	72.7964	72.7733	0	72.7964	2	2	0	2	1	0	0	73.5582	73.5582	124.7258	3	PROCESSED	57553.114375	2016-06-14 02:44:42	55804	2011-08-31 00:00:00	55435.2980092593	2010-08-27 07:09:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050024	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	5	AO5	BROAD BAND SPECTRA OF SWIFT/BAT SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705006010/	Quick Look
99	EMS1164	265.9438	-76.3446	264.162094	-76.320567	268.39939	-52.925114	317.07818058	-22.45515073	114.3984	55300.0111689815	2010-04-14 00:16:05	55300.6980439815	2010-04-14 16:45:11	705013010	42.3783	40	42.3836	42.3783	0	42.389	2	2	0	2	1	0	0	39.0487	39.0487	59.3439	1	PROCESSED	57551.2223958333	2016-06-12 05:20:15	55675	2011-04-24 00:00:00	55309.1947453704	2010-04-23 04:40:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050050	We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators".	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5	SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705013010/	Quick Look
100	EMS1395	310.8148	17.1786	310.239098	16.997696	318.830842	33.961912	61.89528011	-15.30299533	74.9546	55319.8076736111	2010-05-03 19:23:03	55320.4342476852	2010-05-04 10:25:19	705015010	23.3002	20	23.3002	23.3002	0	23.3002	2	2	0	2	1	0	0	19.4944	19.4944	54.1299	0	PROCESSED	57551.3813773148	2016-06-12 09:09:11	55696	2011-05-15 00:00:00	55330.2005208333	2010-05-14 04:48:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050050	We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators".	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5	SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705015010/	Quick Look
101	MRK 509	311.0469	-10.7401	310.365769	-10.921688	310.545768	7.110758	35.95684044	-29.86794514	252.3716	55521.595625	2010-11-21 14:17:42	55523.8155092593	2010-11-23 19:34:20	705025010	102.1205	100	102.1285	102.1285	0	102.1205	2	2	0	2	1	0	0	92.0625	92.0625	191.7697	0	PROCESSED	57554.2039930556	2016-06-15 04:53:45	55916	2011-12-21 00:00:00	55550.2628356482	2010-12-20 06:18:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050113	We propose the observation of one of the typical Seyferts I Mrk 509 for 100 ksec to understand how a vry hard component component that varies independently of power-law is created and how the physical structure near SMBH in Seyferts is. The hard component has been found by carrying out timing analysis of hard X-ray band to explain the extremely broad iron line feature of several Seyferts. Taking this component into account, we succeeded to explain the data of MCG 6-30-15 without the extremely broad iron line, though the origin of this component has not been identified yet. Because Mrk 509 has strong flux and large amplitude of hard X-ray variation, we found it is the most suitable object to verify this component and to get alternative interpretation to the extremely broad iron line.	EXTRAGALACTIC COMPACT SOURCES	7	C	HIROFUMI NODA		JAP	5	AO5	VERIFICATION OF A HARD COMPONENT THAT VARIES INDEPENDENTLY OF POWER-LAW IN TYPE I SEYFERT MRK 509	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705025010/	Quick Look
102	CEN A S LOBE NO. 2	200.3949	-45.1401	199.658837	-44.878468	217.502785	-33.539168	308.49497877	17.40582221	289.0008	55419.7766087963	2010-08-11 18:38:19	55420.9641087963	2010-08-12 23:08:19	705033010	81.3878	80	81.3958	81.3878	0	81.4038	2	2	0	2	1	0	0	68.1085	68.1085	102.5858	0	PROCESSED	57552.9708564815	2016-06-13 23:18:02	55812	2011-09-08 00:00:00	55445.267662037	2010-09-06 06:25:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051401	We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays).	EXTRAGALACTIC COMPACT SOURCES	7	B	GRZEGORZ MADEJSKI		USA	5	AO5	SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705033010/	Quick Look
103	1RXS J111706.3+20141	169.2749	20.2432	168.614437	20.516401	162.09404	14.35752	225.56577108	67.37465885	120.2309	55510.3081944444	2010-11-10 07:23:48	55511.1543402778	2010-11-11 03:42:15	705036010	34.2125	32	34.2125	34.2125	0	34.2125	2	2	0	2	1	0	0	31.5366	31.5366	73.0979	0	PROCESSED	57554.0402199074	2016-06-15 00:57:55	55903	2011-12-08 00:00:00	55537.0979050926	2010-12-07 02:20:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051402	High frequency peaked BL Lacs are a peculiar subclass of Blazars characterized by non-thermal emission across the whole electromagnetic spectrum. Their spectral energy distributions (SEDs) include two main components: a low-energy component with power peaking in the range from the UV to the X-ray band, and a substantial high-energy component often dominated by gamma-rays. We propose 3 observations (32 ks each) of a selected sample of HBLs to study the behavior of the first component, widely interpreted as synchrotron radiation. First, we will be able to disentangle between different spectral shapes of the synchrotron SED of HBLs. Second, we will use the proposed observations to investigate the properties of the most representative sample of TeV candidate HBLs.	EXTRAGALACTIC COMPACT SOURCES	7	C	FRANCESCO MASSARO		USA	5	AO5	X-RAY CURVED SPECTRA IN HIGH FREQUENCY PEAKED BL LACS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705036010/	Quick Look
104	3C111	64.5838	38.0329	63.747646	37.911608	69.36811	16.396021	161.66828978	-8.81804056	76.1726	55453.9599768518	2010-09-14 23:02:22	55455.7432986111	2010-09-16 17:50:21	705040030	80.3659	80	80.3819	80.3659	0	80.3819	2	2	0	2	1	0	0	70.9533	70.9533	154.0639	2	PROCESSED	57553.468599537	2016-06-14 11:14:47	55835	2011-10-01 00:00:00	55469.3718287037	2010-09-30 08:55:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051412	Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components.	EXTRAGALACTIC COMPACT SOURCES	7	A	RITA SAMBRUNA		USA	5	AO5	PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705040030/	Quick Look
105	MKN 590	33.6477	-0.7713	33.009436	-1.003927	31.140057	-13.460103	163.51612886	-56.94122484	251.1273	55587.0949652778	2011-01-26 02:16:45	55588.2146990741	2011-01-27 05:09:10	705043020	40.9139	150	40.9219	40.9219	0	40.9139	2	2	0	2	1	0	0	37.8699	37.8699	96.7339	1	PROCESSED	57600.7810763889	2016-07-31 18:44:45	55988	2012-03-02 00:00:00	55621.2137731482	2011-03-01 05:07:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051433	We propose a 150 ks Suzaku long-look to study the Compton reflection component, soft excess, ionized emission and possible ionized reflection of the Seyfert 1.2 AGN Mkn 590, which has an unobscured line of sight or "bare nucleus" and as of yet unquantified reflection. We aim to accurately constrain the geometry of the circumnuclear material and determine the ionization states of both the Compton-thin and Compton-thick material surrounding the black hole by studying the origin of the soft excess, determining the likelihood of ionized reflection and accurately measuring the intensity of neutral, H-like and He-like Fe emission lines.	EXTRAGALACTIC COMPACT SOURCES	7	C	ELIZABETH RIVERS		USA	5	AO5	QUANTIFYING THE COMPTON REFLECTION AND IONIZED EMISSION IN MKN 590	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705043020/	Quick Look
106	NGC 4945	196.3636	-49.4659	195.633608	-49.198211	217.017818	-38.639251	305.27160994	13.34216317	120.2557	55590.0873842593	2011-01-29 02:05:50	55591.1182175926	2011-01-30 02:50:14	705047050	46.1076	40	46.1076	46.1076	0	46.1076	2	2	0	2	1	0	0	54.0907	54.0907	89.0518	0	PROCESSED	57600.8100810185	2016-07-31 19:26:31	55969	2012-02-12 00:00:00	55602.2238194445	2011-02-10 05:22:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051442	We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval.	EXTRAGALACTIC COMPACT SOURCES	7	B	GUIDO RISALITI		USA	5	AO5	HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047050/	Quick Look
107	SWIFTJ2344.6-424322	356.1059	-42.7624	355.44614	-43.040118	336.666972	-37.094539	339.65324523	-69.27134863	225.0657	55505.2812731482	2010-11-05 06:45:02	55506.5570601852	2010-11-06 13:22:10	705049010	61.7416	60	61.7416	61.7416	0	61.7416	2	2	0	2	1	0	0	50.3941	50.3941	110.2118	1	PROCESSED	57553.9985532407	2016-06-14 23:57:55	55885	2011-11-20 00:00:00	55518.3162847222	2010-11-18 07:35:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051443	We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec.	EXTRAGALACTIC COMPACT SOURCES	7	C	WAYNE BAUMGARTNER		USA	5	AO5	SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705049010/	Quick Look
108	MCG-03-58-007	342.3795	-19.2152	341.708645	-19.480081	336.393592	-10.851288	42.20057234	-60.96689333	68.5139	55350.7016203704	2010-06-03 16:50:20	55352.8940046296	2010-06-05 21:27:22	705052010	99.0873	100	99.0873	99.0873	0	99.0873	2	2	0	2	1	0	0	81.42	81.42	189.406	1	PROCESSED	57551.8454513889	2016-06-12 20:17:27	55734	2011-06-22 00:00:00	55365.563912037	2010-06-18 13:32:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052011	Despite their relevance, less than two dozens of confirmed Compton-thick (CT) AGN have been found so far. We have recently selected a well defined sample of CT AGN candidates using FX/Fir ratios and X-ray colors. Due to their heavy obscuration, good statistics at 6.4 keV and data above 10 keV are needed to assess the real nature of these sources. We propose deep Suzaku observations (100 and 150 ks) for two sources for which data above 10 keV are not available and the quality of XMM data is poor. This request is a continuation of an approved AO4 proposal. These observations will allow us to possibly unveil two more examples of CT AGN, provide a physical characterization of the relatively bright tail of our sample, and estimate the efficiency of our method in selecting CT AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	PAOLA SEVERGNINI		EUR	5	AO5	SUZAKU OBSERVATIONS OF TWO COMPTON-THICK CANDIDATES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705052010/	Quick Look
109	CENTAURUS B	206.7018	-60.4061	205.845186	-60.15638	231.230588	-45.191821	309.72060452	1.73379394	97.6796	55572.6060763889	2011-01-11 14:32:45	55572.7919444444	2011-01-11 19:00:24	705059010	8.7611	10	8.7691	8.7691	0	8.7611	1	1	0	1	1	0	0	6.4526	6.4526	16.0559	0	PROCESSED	57600.577650463	2016-07-31 13:51:49	55962	2012-02-05 00:00:00	55595.2069675926	2011-02-03 04:58:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052018	We propose a 100 ks Suzaku observation of 4U 1344-60, a poorly studied (because at low Galactic latitude) but bright (about 2 millicrabs) AGN which showed, in an XMM-Newton observation, a strong relativistic disk iron line. The main aim of the proposal is to determine in detail the parameters of the disk, which is possible only with a high quality broad band observation which permits to control the continuum beneath the line. Presently, only Suzaku has the right combination of sensitivity, energy resolution and broad band coverage to achieve this objective.	EXTRAGALACTIC COMPACT SOURCES	7	C	JIRI SVOBODA		EUR	5	AO5	4U 1344-60: A BRIGHT AGN WITH A STRONG RELATIVISTIC IRON LINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705059010/	Quick Look
110	FAIRALL 9	20.848	-58.7784	20.369866	-59.039074	340.553777	-59.094561	295.14856402	-57.86436534	32.7271	55335.1255671296	2010-05-19 03:00:49	55338.764837963	2010-05-22 18:21:22	705063010	229.2963	250	229.302	229.302	0	229.2963	2	2	0	2	1	0	0	174.9412	174.9412	288.656	1	PROCESSED	57551.9874074074	2016-06-12 23:41:52	55287	2010-04-01 00:00:00	55434.4437615741	2010-08-26 10:39:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	056003	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	5	AO5	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705063010/	Quick Look
111	NGC6251_LOBE_BGD2	245.2973	82.3586	246.565183	82.472103	101.108878	73.211894	115.82251183	31.60630628	26.9772	55667.4343981482	2011-04-16 10:25:32	55667.8230902778	2011-04-16 19:45:15	706005010	12.0103	20	12.0183	12.0103	0	12.0263	1	1	0	1	1	0	0	17.5851	17.5851	33.5759	0	PROCESSED	57601.5154976852	2016-08-01 12:22:19	56058	2012-05-11 00:00:00	55690.9834490741	2011-05-09 23:36:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060004	We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	6	AO6	SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706005010/	Quick Look
112	IC 4518A	224.419	-43.1269	223.597719	-42.926611	234.851401	-25.085272	326.11466585	13.99053707	102.9822	55959.1723263889	2012-02-02 04:08:09	55961.0002777778	2012-02-04 00:00:24	706012010	64.3986	60	64.3986	64.3986	0	64.3986	2	2	0	2	1	0	0	57.2381	57.2381	157.9058	1	PROCESSED	57604.5692708333	2016-08-04 13:39:45	56434	2013-05-22 00:00:00	56068.6321064815	2012-05-21 15:10:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060040	We propose to observe the Compton-thin AGN IC 4518A with a very small L_X/L_IR ratio, which has often been employed as an indicator of the presence of a Compton-thick AGN. Our aim is to examine the recent argument that L_X/L_IR is not a good measure of absorption column densities and that this ratio is more dependent on the covering fraction of absorber and intrinsic spectral shape. We measure the spectral slope, covering fraction, and NH, and compare them with the prediction of Monte-Carlo simulations to test the validity of L_X/L_IR as a measure of Compton thickness.	EXTRAGALACTIC COMPACT SOURCES	7	C	YOSHITAKA HIRATA		JAP	6	AO6	BROAD-BAND SPECTRA OF THE COMPTON-THIN AGN IC 4518A WITH A SMALL L_X/L_IR: TESTING VALIDITY OF A COMPTON-THICK INDICATOR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706012010/	Quick Look
113	RX J1633+4718	248.3303	47.3072	247.970126	47.410772	228.761848	67.666439	73.53738657	42.62611906	329.4078	55743.8204050926	2011-07-01 19:41:23	55744.8460069444	2011-07-02 20:18:15	706027010	39.9916	40	39.9916	39.9916	0	39.9916	2	2	0	2	1	0	0	39.6531	39.6531	88.6059	1	PROCESSED	57602.4692013889	2016-08-02 11:15:39	56144	2012-08-05 00:00:00	55775.3057407407	2011-08-02 07:20:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060089	RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time.	EXTRAGALACTIC COMPACT SOURCES	7	A	KIYOSHI HAYASHIDA		JAP	6	AO6	X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027010/	Quick Look
114	SMC X-1	19.2724	-73.4484	18.941012	-73.711562	312.330249	-66.473862	300.41553375	-43.55429702	25.8573	55691.0197337963	2011-05-10 00:28:25	55691.4064814815	2011-05-10 09:45:20	706030040	17.9054	18	17.9214	17.9214	0	17.9054	1	1	0	1	1	0	0	16.8143	16.8143	33.4079	0	PROCESSED	57601.9922222222	2016-08-01 23:48:48	56068	2012-05-21 00:00:00	55701.1543981482	2011-05-20 03:42:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030040/	Quick Look
115	SMC X-1	19.2675	-73.4407	18.935881	-73.70387	312.347206	-66.469935	300.41598527	-43.56211574	204.2035	55875.0768055556	2011-11-10 01:50:36	55875.6182291667	2011-11-10 14:50:15	706030080	19.8598	18	19.8881	19.8961	0	19.8598	2	2	0	1	1	0	0	19.2508	19.2508	46.772	0	PROCESSED	57603.7203587963	2016-08-03 17:17:19	56260	2012-11-29 00:00:00	55890.6941203704	2011-11-25 16:39:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030080/	Quick Look
116	SMC X-1	19.2681	-73.4483	18.936643	-73.711469	312.329443	-66.472676	300.41718915	-43.55456404	342.3682	56005.2598611111	2012-03-19 06:14:12	56005.8452546296	2012-03-19 20:17:10	706030100	18.5821	18	18.6263	18.6343	0	18.5821	2	2	0	1	1	0	0	20.3061	20.3061	50.5719	0	PROCESSED	57604.9618055556	2016-08-04 23:05:00	56399	2013-04-17 00:00:00	56022.2021296296	2012-04-05 04:51:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030100/	Quick Look
117	III ZW 2	2.6244	10.9839	1.981573	10.705729	6.801457	9.029508	106.97577765	-50.61513425	67.4163	55726.9877893518	2011-06-14 23:42:25	55728.9792708333	2011-06-16 23:30:09	706031010	81.466	80	81.466	81.466	0	81.466	2	2	0	2	1	0	0	74.3629	74.3629	172.0397	3	PROCESSED	57602.3450925926	2016-08-02 08:16:56	56127	2012-07-19 00:00:00	55757.7040046296	2011-07-15 16:53:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061411	Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASAAKI HAYASHIDA		USA	6	AO6	SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706031010/	Quick Look
118	ESO 323-G077	196.6073	-40.4236	195.900559	-40.156267	212.090645	-30.55227	306.0162391	22.35835315	295.8925	55762.647337963	2011-07-20 15:32:10	55763.4168287037	2011-07-21 10:00:14	706033010	44.1222	40	44.1222	44.1222	0	44.1222	2	2	0	2	1	0	0	40.9258	40.9258	66.4819	0	PROCESSED	57602.6188310185	2016-08-02 14:51:07	56212	2012-10-12 00:00:00	55845.2395949074	2011-10-11 05:45:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061411	Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects.	EXTRAGALACTIC COMPACT SOURCES	7	B	MASAAKI HAYASHIDA		USA	6	AO6	SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706033010/	Quick Look
119	3C120	68.2984	5.3496	67.633882	5.245152	67.432526	-16.407924	190.37864439	-27.39774516	260.9996	55966.4234143518	2012-02-09 10:09:43	55970.8752083333	2012-02-13 21:00:18	706042010	183.0015	300	183.0255	183.0015	0	183.0255	3	2	0	2	1	0	0	158.0306	158.0306	384.5957	3	PROCESSED	57604.7163310185	2016-08-04 17:11:31	55652	2011-04-01 00:00:00	55992.4178819444	2012-03-06 10:01:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066003	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	6	AO6-KP	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706042010/	Quick Look
120	3C120	68.2996	5.3511	67.635075	5.246657	67.433996	-16.406625	190.37800916	-27.39591229	261.0003	55971.7483564815	2012-02-14 17:57:38	55974.8819907407	2012-02-17 21:10:04	706042020	118.0689	120	118.0689	118.0689	0	118.0689	2	2	0	2	1	0	0	103.5365	103.5365	270.7359	2	PROCESSED	57604.7019791667	2016-08-04 16:50:51	55652	2011-04-01 00:00:00	55992.3150694444	2012-03-06 07:33:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	066003	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	6	AO6-KP	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706042020/	Quick Look
121	1622-297	246.5282	-29.8629	245.741591	-29.750241	249.573082	-8.070344	348.81494865	13.309894	287.0011	55828.8879166667	2011-09-24 21:18:36	55829.1800810185	2011-09-25 04:19:19	706044010	8.7781	10	8.7781	8.7781	0	8.7781	2	2	0	2	1	0	0	8.7513	8.7513	25.198	0	PROCESSED	57603.2321064815	2016-08-03 05:34:14	56236	2012-11-05 00:00:00	55868.9351851852	2011-11-03 22:26:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061601	We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	6	AO6	EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706044010/	Quick Look
122	4C38.41	248.824	38.1186	248.386993	38.220121	236.373082	59.10929	61.06470824	42.32788618	255.0463	55829.1891666667	2011-09-25 04:32:24	55829.4148032407	2011-09-25 09:57:19	706045010	8.9239	10	8.9319	8.9319	0	8.9239	1	1	0	1	1	0	0	9.5353	9.5353	19.4719	0	PROCESSED	57603.2349305556	2016-08-03 05:38:18	56225	2012-10-25 00:00:00	55875.6235185185	2011-11-10 14:57:52	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061601	We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	6	AO6	EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706045010/	Quick Look
123	3C 236 WEST LOBE	151.329	34.9949	150.593371	35.23826	140.67974	21.703249	189.91194492	53.83302535	299.9981	56053.9465740741	2012-05-06 22:43:04	56055.7862384259	2012-05-08 18:52:11	707005010	83.9935	80	83.9935	83.9935	0	83.9935	2	2	0	2	1	0	0	80.4248	80.4248	158.9318	2	PROCESSED	57605.4100925926	2016-08-05 09:50:32	56436	2013-05-24 00:00:00	56070.2690856482	2012-05-23 06:27:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070014	Through the Suzaku observations of giant radio galaxies, of which the size is larger than about 1 Mpc, we are going to reveal a picture that the jets in radio galaxies become inactive as they evolve from 500 kpc to 1 Mpc. However, the current Suzaku sample of the giant radio galaxies is far from being satisfactory to make a definite conclusion. Therefore, we propose a Suzaku observation of 3C 236, one of the most giant radio galaxy in the Universe.	EXTRAGALACTIC COMPACT SOURCES	7	A	NAOKI ISOBE		JAP	7	AO7	INVESTIGATION INTO EVOLUTION OF THE JET ENERGETICS, THROUGH THE SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 236	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707005010/	Quick Look
124	2FGL J0037.8+1238	9.4591	12.6426	8.808625	12.367737	13.671851	7.875917	117.75617703	-50.09241086	67.2998	56108.005787037	2012-06-30 00:08:20	56108.9432523148	2012-06-30 22:38:17	707010010	28.6039	30	28.6039	28.6039	0	28.6039	2	2	0	2	1	0	0	30.0977	30.0977	80.972	1	PROCESSED	57606.5224768518	2016-08-06 12:32:22	56493	2013-07-20 00:00:00	56127.1415625	2012-07-19 03:23:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070034	We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN).	EXTRAGALACTIC COMPACT SOURCES	7	B	JUN KATAOKA		JAP	7	AO7	FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707010010/	Quick Look
125	NGC1365	53.4072	-36.1471	52.929884	-36.314043	36.805891	-53.04754	237.96723255	-54.59318142	57.2979	56125.3876273148	2012-07-17 09:18:11	56125.896087963	2012-07-17 21:30:22	707017030	26.7672	30	26.7672	26.7672	0	26.7672	2	2	0	2	1	0	0	25.2112	25.2112	43.9239	1	PROCESSED	57606.6299537037	2016-08-06 15:07:08	56582	2013-10-17 00:00:00	56212.7663194444	2012-10-12 18:23:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070095	NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. }	EXTRAGALACTIC COMPACT SOURCES	7	B	YASUSHI FUKAZAWA		JAP	7	AO7	MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017030/	Quick Look
126	HOLMBERG IX X-1	149.4435	69.0486	148.425456	69.287009	119.776016	51.672601	141.95726659	41.07139178	311.5635	56030.7575810185	2012-04-13 18:10:55	56034.6807175926	2012-04-17 16:20:14	707019010	182.5274	500	182.5274	182.5274	0	182.5274	2	2	0	2	1	0	0	208.6236	208.6236	338.9339	3	PROCESSED	57605.2861342593	2016-08-05 06:52:02	56018	2012-04-01 00:00:00	56044.4614699074	2012-04-27 11:04:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071251	Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy.	EXTRAGALACTIC COMPACT SOURCES	7	A	JON MILLER		USA	7	AO7	A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019010/	Quick Look
127	HOLMBERG IX X-1	149.4877	69.0751	148.469613	69.31362	119.77363	51.703415	141.9165022	41.0686989	124.501	56221.770162037	2012-10-21 18:29:02	56224.1252083333	2012-10-24 03:00:18	707019020	107.4958	320	107.4958	107.4958	0	107.4958	2	2	0	2	1	0	0	106.8673	106.8673	203.4479	1	PROCESSED	57607.8555324074	2016-08-07 20:31:58	56018	2012-04-01 00:00:00	56330.5864930556	2013-02-07 14:04:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071251	Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy.	EXTRAGALACTIC COMPACT SOURCES	7	A	JON MILLER		USA	7	AO7	A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019020/	Quick Look
128	HOLMBERG IX X-1	149.4867	69.0744	148.468616	69.312918	119.773774	51.702635	141.91753226	41.06881922	124.4999	56226.4169097222	2012-10-26 10:00:21	56228.7717708333	2012-10-28 18:31:21	707019040	110.0175	500	110.0383	110.0175	0	110.0175	3	2	0	2	1	0	0	105.7961	105.7961	203.426	2	PROCESSED	57607.8756018518	2016-08-07 21:00:52	56018	2012-04-01 00:00:00	56240.5502430556	2012-11-09 13:12:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071251	Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy.	EXTRAGALACTIC COMPACT SOURCES	7	A	JON MILLER		USA	7	AO7	A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019040/	Quick Look
129	NGC 4151	182.642	39.4132	182.010684	39.69131	164.095796	36.629182	155.04475012	75.06022062	134.3454	56242.8428472222	2012-11-11 20:13:42	56245.9599537037	2012-11-14 23:02:20	707024010	150.2669	150	150.2829	150.2669	0	150.2829	2	2	0	2	1	0	0	150.5465	150.5465	269.2897	4	PROCESSED	57608.0679861111	2016-08-08 01:37:54	56702	2014-02-14 00:00:00	56330.6348032407	2013-02-07 15:14:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071417	We propose simultaneous NuSTAR/Suzaku observations of NGC 4151 and IC 4329A. These pointings will achieve three goals: (1) They will provide the best-ever broad-band X-ray spectra of two of the brightest Seyfert galaxies in the 0.5-80 keV band; (2) They will enable broad-band, time-resolved X-ray spectroscopy of these fascinating and variable sources; (3) They will serve as invaluable calibration targets for the two observatories. The spectral coverage and sensitivity will enable the continuum, absorption and reflection components of each spectrum to be conclusively disentangled, allowing us to determine whether inner disk reflection signatures are present. We will also be able to break the degeneracy between the coronal temperature and optical depth in both AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	LAURA BRENNEMAN		USA	7	AO7	SHEDDING NEW LIGHT ON THE BROAD-BAND X-RAY SPECTRA OF NGC 4151 AND IC 4329A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707024010/	Quick Look
130	NGC 5252	204.5663	4.5481	203.934961	4.801923	201.032031	13.744519	331.30380316	64.80829028	117.6998	56287.8794791667	2012-12-26 21:06:27	56289.0952777778	2012-12-28 02:17:12	707028010	50.2701	45	50.2701	50.2921	0	50.2766	2	2	0	2	1	0	0	43.3367	43.3367	105.0278	0	PROCESSED	57608.3760300926	2016-08-08 09:01:29	56687	2014-01-30 00:00:00	56321.5462268518	2013-01-29 13:06:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071424	A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN.	EXTRAGALACTIC COMPACT SOURCES	7	C	TRACEY TURNER		USA	7	AO7	INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707028010/	Quick Look
131	PDS 456	262.0802	-14.261	261.369515	-14.22093	262.220782	8.966234	10.39487872	11.16781955	96.2511	56344.8907407407	2013-02-21 21:22:40	56349.993912037	2013-02-26 23:51:14	707035010	182.299	450	182.299	182.299	0	182.299	2	2	0	2	1	0	0	160.3071	160.3071	440.8752	4	PROCESSED	57610.7549768518	2016-08-10 18:07:10	56018	2012-04-01 00:00:00	56363.6993981482	2013-03-12 16:47:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071431	PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456.	EXTRAGALACTIC COMPACT SOURCES	7	B	JAMES REEVES		USA	7	AO7	VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707035010/	Quick Look
132	PDS 456	262.0805	-14.2617	261.369811	-14.221632	262.221115	8.965551	10.39443055	11.16720212	96.2512	56354.8215972222	2013-03-03 19:43:06	56359.5001388889	2013-03-08 12:00:12	707035020	164.8107	450	164.8267	164.8107	0	164.8291	2	2	0	2	1	0	0	147.4496	147.4496	404.1815	2	PROCESSED	57610.8342824074	2016-08-10 20:01:22	56018	2012-04-01 00:00:00	56373.6804166667	2013-03-22 16:19:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071431	PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456.	EXTRAGALACTIC COMPACT SOURCES	7	B	JAMES REEVES		USA	7	AO7	VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707035020/	Quick Look
133	PKS 0548-322	87.6707	-32.2739	87.20583	-32.286363	86.511257	-55.687672	237.56869078	-26.144265	287.028	56023.6105555556	2012-04-06 14:39:12	56026.3891435185	2012-04-09 09:20:22	707040010	102.6567	100	102.6567	102.6567	0	102.6567	2	2	0	2	1	0	0	91.5237	91.5237	240.0558	3	PROCESSED	57605.1844907407	2016-08-05 04:25:40	56415	2013-05-03 00:00:00	56044.314525463	2012-04-27 07:32:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072006	We propose Suzaku observations of the two brightest extreme BL Lac objects, PKS 0548-322 and RGB J0710+591 (100 ksec each), whose synchrotron bump peaks in the medium-hard X-ray band. The requested observations, never performed by Suzaku on this two sources, will permit to measure their continuum in the 0.6-70 keV range, fully exploiting the unique capabilities of the Suzaku satellite. With its wide energy coverage and good response, Suzaku will allow us to determine with unprecedented precision the spectral properties of the sources in the hard, medium and soft X-ray ranges, allowing us to measure the physical properties of the emitting relativistic electrons and, complemented by data at other frequencies, to infer the physical conditions in the emitting region.	EXTRAGALACTIC COMPACT SOURCES	7	A	FABRIZIO TAVECCHIO		EUR	7	AO7	REVEALING THE HIGH-ENERGY SYNCHROTRON PEAK OF EXTREME BL LACS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707040010/	Quick Look
134	0836+710	130.3582	70.9091	129.096	71.086996	109.311372	50.162038	143.52368034	34.42368753	111.9979	56213.6030787037	2012-10-13 14:28:26	56213.8223726852	2012-10-13 19:44:13	707042010	10.613	10	10.613	10.613	0	10.613	1	1	0	1	1	0	0	8.866	8.866	18.9279	0	PROCESSED	57607.7537615741	2016-08-07 18:05:25	56598	2013-11-02 00:00:00	56232.4320717593	2012-11-01 10:22:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071601	We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	7	AO7	MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707042010/	Quick Look
135	BL LAC	330.6707	42.2941	330.154473	42.052039	354.261979	49.60384	92.59387966	-10.42383814	77.7587	56431.6193981482	2013-05-19 14:51:56	56431.8724884259	2013-05-19 20:56:23	707044010	12.7426	10	12.7506	12.7426	0	12.7506	1	1	0	1	1	0	0	13.144	13.144	21.8319	0	PROCESSED	57611.320625	2016-08-11 07:41:42	56826	2014-06-18 00:00:00	56455.7300231482	2013-06-12 17:31:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071601	We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	7	AO7	MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707044010/	Quick Look
136	MARKARIAN 1040	37.056	31.3166	36.314628	31.093376	44.885956	15.789444	146.10796909	-27.16282444	69.5695	56515.9165740741	2013-08-11 21:59:52	56519.1681597222	2013-08-15 04:02:09	707046010	137.4353	135	137.4353	137.4353	0	137.4353	2	2	0	2	1	0	0	136.328	136.328	280.9053	1	PROCESSED	57612.3140625	2016-08-12 07:32:15	56955	2014-10-25 00:00:00	56587.9502662037	2013-10-22 22:48:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072025	Mrk 1040 is a nearby type-1 Seyfert galaxy where a recent XMM observation revealed the presence of a deep soft X-ray warm absorber. However the current data are unable to resolve the components of the absorber so very little is known about its properties. We propose to obtain a 200 ks definitive Chandra HETG observation of Mrk 1040 from 0.5-9.0 keV where we will resolve the lines for the first time enabling a detailed analysis of the kinematics and energetics to be made. We will also obtain the first high-resolution spectrum > 2 keV in this source allowing us to resolve the narrow Fe K alpha core. Furthermore, through a 125 ks Suzaku observation we will also study the Fe K complex in unprecedented detail while simultaneously determining the origin of the hard excess.	EXTRAGALACTIC COMPACT SOURCES	7	S	ANDREW LOBBAN		EUR	7	AO7	A HIGH-RESOLUTION VIEW OF THE WARM ABSORBER AND IRON LINE IN MRK 1040	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707046010/	Quick Look
137	NGC 3516	166.6556	72.561	165.802341	72.831319	123.361761	57.969661	133.25565935	42.40250412	335.7404	56391.9675925926	2013-04-09 23:13:20	56393.0460185185	2013-04-11 01:06:16	708006010	51.386	50	51.402	51.386	0	51.402	2	2	0	2	1	0	0	49.1015	49.1015	93.1638	1	PROCESSED	57611.0515856482	2016-08-11 01:14:17	56383	2013-04-01 00:00:00	56421.6947106482	2013-05-09 16:40:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080066	We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	8	AO8	THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006010/	Quick Look
138	NGC 3516	166.6684	72.5566	165.815394	72.826934	123.372761	57.969452	133.25443095	42.40827092	314.5458	56409.0119560185	2013-04-27 00:17:13	56409.446087963	2013-04-27 10:42:22	708006020	19.103	50	19.119	19.103	0	19.119	3	2	0	2	1	0	0	20.2121	20.2121	30.7239	0	PROCESSED	57611.1744907407	2016-08-11 04:11:16	56383	2013-04-01 00:00:00	56457.6034375	2013-06-14 14:28:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080066	We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	8	AO8	THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006020/	Quick Look
139	NGC 3516	166.6764	72.5574	165.823506	72.827743	123.374751	57.971749	133.25110438	42.40886909	307.603	56424.0155555556	2013-05-12 00:22:24	56425.1044328704	2013-05-13 02:30:23	708006030	50.4283	50	50.4283	50.4283	0	50.4283	1	1	0	1	1	0	0	57.2275	57.2275	94.076	0	PROCESSED	57611.3108680556	2016-08-11 07:27:39	56383	2013-04-01 00:00:00	56436.6511805556	2013-05-24 15:37:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080066	We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	8	AO8	THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006030/	Quick Look
140	NGC6552	270.0757	66.6036	270.078264	66.603205	60.706525	89.950181	96.43339546	29.78135373	217.6129	56610.8399884259	2013-11-14 20:09:35	56613.0126851852	2013-11-17 00:18:16	708014010	105.7767	100	105.7767	105.7767	0	105.7767	2	2	0	2	1	0	0	102.2797	102.2797	187.7079	1	PROCESSED	57613.3907060185	2016-08-13 09:22:37	57019	2014-12-28 00:00:00	56653.7413078704	2013-12-27 17:47:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080092	We propose to observe the interesting Seyfert 2 galaxy NGC6552, which has multi fluorescence lines in the X-ray band. There ara only three objects, including NGC6552, which has multi fluorescence lines in the X-ray band. We aim to detect emission lines finely and study the chemical evolution of the galaxy. We also aim measurements of hard X-ray continuum to constrain the reflection component and other nonthermal emission asscciated with jet or starburst activity.	EXTRAGALACTIC COMPACT SOURCES	7	C	TAKAFUMI KAWANO		JAP	8	AO8	OBSERVATION OF THE MULTI EMISSION LINES FROM SEYFERT 2 GALAXY: NGC6552	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708014010/	Quick Look
141	MKN 335	1.5767	20.2085	0.933785	19.930185	9.740922	17.859652	108.75946317	-41.41793251	71.5257	56454.1494907407	2013-06-11 03:35:16	56457.9792824074	2013-06-14 23:30:10	708016010	143.995	300	144.027	143.995	0	144.027	2	2	0	2	1	0	0	129.5529	129.5529	330.8674	3	PROCESSED	57611.6156828704	2016-08-11 14:46:35	56383	2013-04-01 00:00:00	56470.7662037037	2013-06-27 18:23:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081411	The idea of this proposal is trigger a 300ks observation with Suzaku of the Narrow Line Seyfert 1 Galaxy Mkn 335 during one of its low X-ray flux states. The goal here is to measure its underlying broad-band continuum with Suzaku during a low state and compare it with the 2006 high-state observations. Mkn 335 is one of the best examples of an AGN that went into a deep minimum X-ray flux state. Two competing models can explain these extreme low states: reflection models and partial covering absorber models. Both models still require a variable underlying intrinsic continuum. The science driver is to find out what is causing these low X-ray flux states that have been observed in several NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	A	DIRK GRUPE		USA	8	AO8-TOO	INTRINSIC LOW-STATE X-RAY LUMINOSITY OF THE NLS1 MKN 335	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708016010/	Quick Look
142	MCG-5-23-16	146.9232	-30.945	146.373955	-30.712416	162.623211	-41.142672	262.74537578	17.2400137	295.4404	56444.9213194444	2013-06-01 22:06:42	56448.2467361111	2013-06-05 05:55:18	708021010	159.5262	300	159.5582	159.5262	0	159.5582	2	2	0	2	1	0	0	155.1267	155.1267	287.3018	1	PROCESSED	57611.525787037	2016-08-11 12:37:08	56383	2013-04-01 00:00:00	56461.789537037	2013-06-18 18:56:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081416	Significant recent developments in probing environments around AGN black holes has been achieved using X-ray reverberation. They were initially detected in the soft excess of several NLS1s, then recently, the first Fe K reverberation was also seen. In addition to measuring x-rays reverberating a few r_g from the event horizon, short/long delays from different radii have been separated for the first time in NGC4151. Here we propose to observe MCG-5-23-1 for 300 ks in order to study its iron K reverberation. It is optimally one of the brightest and most variable AGN in X-rays. Archival data already show very exciting signatures of Fe K reverberation. With new observations we aim to constrain the emitting region size and study the emission originating at different distances from of the hole.	EXTRAGALACTIC COMPACT SOURCES	7	A	ABDERAHMEN ZOGHBI		USA	8	AO8	IRON K REVERBERATION IN MCG 5-23-16	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708021010/	Quick Look
143	NGC 235A	10.7176	-23.5378	10.098982	-23.81167	359.839777	-25.738096	94.13393297	-85.9211578	213.1719	56636.0921759259	2013-12-10 02:12:44	56636.4792939815	2013-12-10 11:30:11	708026010	19.8251	20	19.8331	19.8251	0	19.8409	2	2	0	2	1	0	0	18.2251	18.2251	33.4439	1	PROCESSED	57613.5511921296	2016-08-13 13:13:43	56383	2013-04-01 00:00:00	56646.6871412037	2013-12-20 16:29:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081419	The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come.	EXTRAGALACTIC COMPACT SOURCES	7	C	TAHIR YAQOOB		USA	8	AO8	ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708026010/	Quick Look
144	CENTAURUS A	201.3699	-43.0194	200.636516	-42.759434	217.141069	-31.326977	309.51956362	19.416494	303.7255	56519.1824305556	2013-08-15 04:22:42	56519.4264930556	2013-08-15 10:14:09	708036010	10.6751	10	10.6751	10.6751	0	10.6911	1	1	0	1	1	0	0	10.0647	10.0647	21.0799	0	PROCESSED	57612.2554050926	2016-08-12 06:07:47	56954	2014-10-24 00:00:00	56587.7389351852	2013-10-22 17:44:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081433	We request observations of the nucleus of the radio galaxy Centaurus A to study time variability of its broadband spectral energy distribution (SED) and constrain jet emission models of radio-loud AGN. Due to its proximity, Cen A can be studied in unique detail. Although frequently observed, no time-dependent, simultaneous SEDs covering the spectrum from radio to gamma-rays have been obtained for Cen A so far. Since AGN are highly variable, only quasi-contemporaneous SEDs allow us to constrain parameters of jet emission models. Combining our TANAMI radio Very Long Baseline Interferometry monitoring campaign and Fermi observations with simultaneous Suzaku spectra will fill the gap in energy and address the time-dependent behavior of jet emission and torus absorption with high accuracy.	EXTRAGALACTIC COMPACT SOURCES	7	B	ROOPESH OJHA		USA	8	AO8	SIMULTANEOUS SUZAKU AND MULTIWAVELENGTH OBSERVATIONS OF THE NUCLEUS OF CENTAURUS A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708036010/	Quick Look
145	CENTAURUS A	201.3033	-43.0014	200.570255	-42.741318	217.080563	-31.331883	309.47108059	19.44109405	111.5377	56663.4710763889	2014-01-06 11:18:21	56663.6613888889	2014-01-06 15:52:24	708036020	7.3652	10	7.3652	7.3732	0	7.3732	1	1	0	1	1	0	0	6.5444	6.5444	16.4399	0	PROCESSED	57613.7500462963	2016-08-13 18:00:04	57086	2015-03-05 00:00:00	56719.7206944444	2014-03-03 17:17:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081433	We request observations of the nucleus of the radio galaxy Centaurus A to study time variability of its broadband spectral energy distribution (SED) and constrain jet emission models of radio-loud AGN. Due to its proximity, Cen A can be studied in unique detail. Although frequently observed, no time-dependent, simultaneous SEDs covering the spectrum from radio to gamma-rays have been obtained for Cen A so far. Since AGN are highly variable, only quasi-contemporaneous SEDs allow us to constrain parameters of jet emission models. Combining our TANAMI radio Very Long Baseline Interferometry monitoring campaign and Fermi observations with simultaneous Suzaku spectra will fill the gap in energy and address the time-dependent behavior of jet emission and torus absorption with high accuracy.	EXTRAGALACTIC COMPACT SOURCES	7	B	ROOPESH OJHA		USA	8	AO8	SIMULTANEOUS SUZAKU AND MULTIWAVELENGTH OBSERVATIONS OF THE NUCLEUS OF CENTAURUS A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708036020/	Quick Look
146	ABELL 998	156.5862	67.9284	155.666008	68.182911	124.296815	52.261797	140.87284378	43.80315875	119.4303	56601.7924768518	2013-11-05 19:01:10	56602.9584722222	2013-11-06 23:00:12	708041010	60.2402	60	60.2402	60.2404	0	60.2562	3	2	0	2	1	0	0	51.856	51.856	100.7319	2	PROCESSED	57613.2563657407	2016-08-13 06:09:10	56980	2014-11-19 00:00:00	56614.6831944444	2013-11-18 16:23:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081533	We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters.	EXTRAGALACTIC COMPACT SOURCES	7	C	LAURENCE DAVID		USA	8	AO8	MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708041010/	Quick Look
147	FAIRALL 51	281.2231	-62.3584	280.059194	-62.409813	276.677853	-39.177664	333.20555808	-23.08834808	251.8035	56542.816087963	2013-09-07 19:35:10	56543.4286689815	2013-09-08 10:17:17	708046030	23.9301	30	23.9381	23.9439	0	23.9301	1	1	0	1	1	0	0	35.6507	35.6507	52.9199	0	PROCESSED	57612.5525694445	2016-08-12 13:15:42	56990	2014-11-29 00:00:00	56625.6038078704	2013-11-29 14:29:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082016	Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures.	EXTRAGALACTIC COMPACT SOURCES	7	A	JIRI SVOBODA		EUR	8	AO8	STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708046030/	Quick Look
148	SN 2006JD	120.5317	0.8109	119.887421	0.950976	122.551734	-19.245465	220.45479917	16.05743863	101.8795	56954.8286458333	2014-10-24 19:53:15	56958.31125	2014-10-28 07:28:12	709001010	144.4894	150	144.4894	151.0361	0	151.0521	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7014351852	2016-08-16 16:50:04	57435	2016-02-17 00:00:00	57066.4298032407	2015-02-13 10:18:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090005	We propose a 150 ks observation of a supernova (SN) 2006jd, a bright SN IIn discovered on October 12, 2006. It is a rare SN that remains bright in X-rays over several years, hence provides us with a rare opportunity to study the dense medium that was ejected by the progenitor star before the SN explosion. Our analysis of archival data taken by Suzaku in 2008 and XMM-Newton in 2009 has indicated interesting spectral evolution, i.e., spectral softening and an increasing centroid of Fe-K lines complex. Our proposed observation will show much clearer spectral variation than that seen in the previous Suzaku and XMM-Newton data, allowing us to understand the details of spectral evolution. The dataset will become a reference for the study of late-time X-ray spectroscopy of SN IIn.	EXTRAGALACTIC COMPACT SOURCES	7	B	SATORU KATSUDA		JAP	9	AO9	PROBING LATE-TIME X-RAY SPECTRUM OF SN 2006JD	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709001010/	Quick Look
149	NGC 2655	133.9038	78.2094	132.281402	78.399558	105.125039	57.091904	134.93858201	32.69360092	275.5561	56789.4281828704	2014-05-12 10:16:35	56791.0731712963	2014-05-14 01:45:22	709003010	76.8371	80	76.8371	76.8371	0	76.8371	2	2	0	2	0	0	0	0	0	2.1539	0	PROCESSED	57615.0904398148	2016-08-15 02:10:14	57173	2015-05-31 00:00:00	56807.6198726852	2014-05-30 14:52:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090017	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	9	AO9	BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709003010/	Quick Look
150	ARP318	32.3792	-10.1586	31.765368	-10.394539	26.44249	-21.810803	173.95964772	-64.97329044	75.9989	56873.8890509259	2014-08-04 21:20:14	56875.8252662037	2014-08-06 19:48:23	709009010	80.2195	80	80.2195	80.2195	0	80.222	2	2	0	2	1	0	0	15.3811	15.3811	43.076	0	PROCESSED	57616.4808217593	2016-08-16 11:32:23	57267	2015-09-02 00:00:00	56898.4603703704	2014-08-29 11:02:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090037	We propose Suzaku/XIS and PIN observations of nearby two radio-quiet AGNs with very weak mid-infrared emission, which might represent a new class of hot dust free AGNs. We found hot dust free AGN candidates by combining the Swift/BAT hard X-ray all-sky AGN catalog with mid-infrared (MIR) all-sky surveys. Three out of 503 sources are not detected in their MIR bands, even in the high sensitivity of WISE. One source is radio-loud AGNs and the other two radio-quiet sources are also observed in 2-10 keV band with Swift/XRT, and no significant Fe Ka line emission is detected. The scientific goal of this proposal is to obtain the first Fe Ka detection or strong constraints of the emission, which will give us a direct evidence that these sources have very small amount or even lack of torus.	EXTRAGALACTIC COMPACT SOURCES	7	B	KOHEI ICHIKAWA		JAP	9	AO9	THE FIRST BROADBAND X-RAY OBSERVATIONS OF HOT DUST FREE AGNS IN THE LOCAL UNIVERSE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709009010/	Quick Look
151	HOLMBERG IX X-1	149.4663	69.0509	148.44846	69.289367	119.784926	51.679022	141.94846823	41.07666025	284.4995	57158.2357291667	2015-05-16 05:39:27	57159.0827546296	2015-05-17 01:59:10	709015040	34.12	30	34.12	34.128	0	34.128	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.6575347222	2016-08-18 15:46:51	57536	2016-05-28 00:00:00	57168.6253935185	2015-05-26 15:00:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091251	Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs.	EXTRAGALACTIC COMPACT SOURCES	7	A	DOMINIC WALTON		USA	9	AO9	MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015040/	Quick Look
152	HE0512-3329	78.5445	-33.4308	78.084109	-33.487216	72.678048	-56.186874	236.61833373	-33.85137764	251.0519	57071.9701388889	2015-02-18 23:17:00	57072.4937847222	2015-02-19 11:51:03	709020030	25.0955	26	25.0955	25.0955	0	25.0955	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6171296296	2016-08-17 14:48:40	57457	2016-03-10 00:00:00	57087.4623726852	2015-03-06 11:05:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091431	The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission.	EXTRAGALACTIC COMPACT SOURCES	7	B	BIN CHEN		USA	9	AO9	CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709020030/	Quick Look
153	MARKARIAN 3	93.8812	71.0496	92.43086	71.064939	91.873944	47.634543	143.28137914	22.71605454	71.2169	56953.1510532407	2014-10-23 03:37:31	56953.6731828704	2014-10-23 16:09:23	709022030	22.7461	20	22.7541	22.7541	0	22.7461	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.6616087963	2016-08-16 15:52:43	57376	2015-12-20 00:00:00	57010.3833217593	2014-12-19 09:11:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092008	We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each.	EXTRAGALACTIC COMPACT SOURCES	7	A	MATTEO GUAINAZZI		EUR	9	AO9	MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022030/	Quick Look
154	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
155	SMC X-1	19.2661	-73.446	18.934565	-73.709172	312.334379	-66.471359	300.41753301	-43.55692043	64.0051	55740.5953819444	2011-06-28 14:17:21	55741.0960069444	2011-06-29 02:18:15	706030060	18.6682	18	18.7129	18.7049	0	18.6682	2	2	0	1	1	0	0	20.6764	20.6764	43.2479	0	PROCESSED	57602.4222800926	2016-08-02 10:08:05	56163	2012-08-24 00:00:00	55775.167974537	2011-08-02 04:01:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030060/	Quick Look
156	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
157	1H 0707-495	107.1586	-49.5558	106.829982	-49.474426	125.752559	-70.871973	260.16951247	-17.68246857	144.7199	53707.1759143518	2005-12-03 04:13:19	53710.0974537037	2005-12-06 02:20:20	700008010	97.2291	100	97.8529	100.3891	97.2291	97.8149	4	2	4	4	1	0	0	91.8008	91.8008	252.3688	4	PROCESSED	57532.4288194444	2016-05-24 10:17:30	54247	2007-05-27 00:00:00	54059.7078472222	2006-11-20 16:59:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001040	We propose a 100 ks observation of the NLS1 1H 0707--495 in order to understand its remarkable and puzzling spectral and variability properties. The Suzaku data will help us to disentangle between the two interpretations adopted so far, namely partial covering and relativistically blurred reflection.	EXTRAGALACTIC COMPACT SOURCES	7	A	GIOVANNI MINIUTTI		JAP	0	SWG	THE EXTREME PROPERTIES OF THE NLS1 GALAXY 1H 0707-495	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700008010/	Quick Look
158	MRK 501	253.4335	39.8281	253.015349	39.90842	242.48193	61.693142	63.68387876	38.89139128	70.9919	54913.7775347222	2009-03-23 18:39:39	54915.3328587963	2009-03-25 07:59:19	703046010	72.3342	65	72.3342	72.3342	0	72.3342	2	2	0	2	1	0	0	64.8365	64.8365	134.3581	1	PROCESSED	57545.930462963	2016-06-06 22:19:52	55329	2010-05-13 00:00:00	54924.366724537	2009-04-03 08:48:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031343	We propose to observe two bright TeV blazars with Suzaku, in coordination with VERITAS and MAGIC at TeV energies. The primary objective is to make use of the recently available observational capabilities in collecting the much needed simultaneous X-ray and TeV data on these intriguing sources. The data will be essential for addressing a number of unresolved issues in the study of TeV blazars, such as spectral variability, X-ray/TeV correlation and associated time lags, spectral hysteresis, etc. The results will likely provide insights into the properties of the emitting particles, as well as those of the emitting regions, emission mechanism, composition of the jets, and acceleration energetics.	EXTRAGALACTIC COMPACT SOURCES	7	A	WEI CUI		USA	3	AO3	COORDINATED X-RAY/TEV OBSERVATIONS OF TEV BLAZARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703046010/	Quick Look
159	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
160	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
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	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
163	3C 111	64.5741	38.0889	63.737568	37.967565	69.370671	16.452489	161.62276278	-8.7838332	81.5451	54700.4141898148	2008-08-22 09:56:26	54703.1836111111	2008-08-25 04:24:24	703034010	122.378	120	122.386	122.378	0	122.378	2	2	0	2	1	0	0	109.7067	109.7067	239.2517	1	PROCESSED	57543.4018287037	2016-06-04 09:38:38	55084	2009-09-10 00:00:00	54713.6361226852	2008-09-04 15:16:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031332	The origin of the high-energy emission from Broad-Line Radio Galaxies is still an open issue. A plausible scenario is reprocessed emission from a cold medium (disk) diluted by variable, non-thermal jet flux. To test this scenario we propose Suzaku observations of the BLRG 3C 111, which exhibits flux variability above 10 keV from available data, suggesting a jet contribution. Moreover, 3C 111 was previously detected with EGRET at GeV energies, and synergy with GLAST will thus be exploited in the proposed program. The coupled timing and spectral information provided by Suzaku are key to disentangle the disk and jet contributions, and determine their respective role for the source energy budget.	EXTRAGALACTIC COMPACT SOURCES	7	A	RITA SAMBRUNA		USA	3	AO3	SUZAKU OBSERVATIONS OF 3C 111: UNCOVERING THE JET WITHIN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703034010/	Quick Look
164	3C 326	238.0402	20.0989	237.485976	20.247377	230.081092	39.212111	33.27596058	48.22956027	119.5805	54484.6775	2008-01-19 16:15:36	54486.215462963	2008-01-21 05:10:16	702006010	61.7381	60	61.7381	61.7381	0	61.7381	2	2	0	2	1	0	0	53.4126	53.4126	132.8598	1	PROCESSED	57541.3565162037	2016-06-02 08:33:23	54888	2009-02-26 00:00:00	54515.0338078704	2008-02-19 00:48:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020014	Suzaku observations of two giant radio galaxies, 3C 326 and 3C 35, are proposed. In 60 ks exposure on the individual targets, inverse Component X-ray emission from their lobes is detected with high signal statistics. As a result, the energy densities of electrons and magnetic fields in these lobesare precisely deteremined. The size of these radio galaxies are significantly larger than that of the previous sample. Therefore, the size dependence of energetics in the lobes will be investigated.	EXTRAGALACTIC COMPACT SOURCES	7	C	NAOKI ISOBE		JAP	2	AO2	SUZAKU OBSERVATIONS OF LOBES OF GIANT RADIO GALAXIES, 3C 326 AND 3C 35	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702006010/	Quick Look
165	SDSS J1723+5553	260.8912	55.8942	260.65651	55.938805	243.54174	78.493359	83.89291292	34.34970174	8.0654	54986.3677777778	2009-06-04 08:49:36	54986.8148032407	2009-06-04 19:33:19	704051010	35.9368	30	35.9448	35.9368	0	35.9528	1	1	0	1	1	0	0	29.0393	29.0393	38.6159	0	PROCESSED	57547.4618865741	2016-06-08 11:05:07	55364	2010-06-17 00:00:00	54998.1759722222	2009-06-16 04:13:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041422	BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction.	EXTRAGALACTIC COMPACT SOURCES	7	A	XINYU DAI		USA	4	AO4	X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704051010/	Quick Look
166	PBC J0839.7-1214	129.9392	-12.3029	129.345024	-12.125278	136.15221	-29.568931	237.21342575	17.37856511	291.8979	55324.6892824074	2010-05-08 16:32:34	55326.4896990741	2010-05-10 11:45:10	705007010	80.5643	80	80.5643	80.5643	0	80.5643	2	2	0	2	1	0	0	70.7418	70.7418	155.5358	1	PROCESSED	57551.4721759259	2016-06-12 11:19:56	55707	2011-05-26 00:00:00	55341.5690856482	2010-05-25 13:39:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050024	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	5	AO5	BROAD BAND SPECTRA OF SWIFT/BAT SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705007010/	Quick Look
167	NGC 3147	154.2433	73.3869	153.186306	73.636446	117.480978	56.071635	136.29780832	39.47682975	262.9224	55340.8248611111	2010-05-24 19:47:48	55343.2925231482	2010-05-27 07:01:14	705054010	150.0476	150	150.0476	150.0556	0	150.0556	2	2	0	2	1	0	0	132.9136	132.9136	213.1818	2	PROCESSED	57553.0649074074	2016-06-14 01:33:28	55765	2011-07-23 00:00:00	55393.4710648148	2010-07-16 11:18:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052013	NGC3147 is the best candidate to be a true Seyfert 2, i.e., with no BLR. We propose a 150 ks observation with Suzaku to study the Fe line profile which in the short XMM-Newton observation shows some structure. If the iron line will turn out to be originated from the accretion disc, the lack of the BLR cannot be attributed to the lack of ionizing photons; if originated from the torus, this would put constraints on models assuming a common origin for the torus and the BLR; if the presence of an ionized iron line is confirmed, a BLR might exist but so highly ionized to be invisible at optical/UV wavelengths. An important added value of this observation is to confirm NGC3147 as a true Seyfert 2 by ruling out a Compton-thick nature, which only Suzaku can do thanks to its hard X-ray coverage.	EXTRAGALACTIC COMPACT SOURCES	7	B	GIORGIO MATT		EUR	5	AO5	SUZAKU OBSERVATION OF THE BEST ``TRUE SEYFERT 2'' GALAXY CANDIDATE, NGC 3147	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705054010/	Quick Look
168	NGC 7603	349.73	0.2557	349.089402	-0.017972	350.656446	4.302592	80.07171077	-54.72674929	67.5296	56080.5080208333	2012-06-02 12:11:33	56082.6598726852	2012-06-04 15:50:13	707003010	101.2567	100	101.2602	101.2657	0	101.2567	2	2	0	2	1	0	0	96.0023	96.0023	185.9037	2	PROCESSED	57605.6196875	2016-08-05 14:52:21	56464	2013-06-21 00:00:00	56096.2688541667	2012-06-18 06:27:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070010	X-ray spectra from Seyfert galaxies often consist of various emission components such as from an accretion disk and dusty torus. Because of this complexity, interpretation of reprocessed feature (Fe lines and reflection continuum) in X-ray spectra is often ambiguous. We selected a Seyfert 1 with very weak mid infrared emission from the putative torus relative to X-rays from an accretin disk bu using AKARI IR and XMM X-ray catalogs. We will measure a ``pure'' accretion disk spectrum without contamination of reprocessed emission from the torus, and castrain extent of an accretion disk, which is expected to depend on an Eddington ratio, from the reprocessed X-ray emission.	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	7	AO7	PURE ACCRETION DISK SPECTRUM OF THE SEYFERT 1 NGC 7603	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707003010/	Quick Look
169	LMC X-4	83.1804	-66.3624	83.172059	-66.39551	0.975905	-87.276392	276.32693529	-32.54034863	209.1491	54480.3607175926	2008-01-15 08:39:26	54480.7919560185	2008-01-15 19:00:25	702038010	21.6579	20	21.6726	21.6579	0	21.6726	2	2	0	2	1	0	0	22.8837	22.8837	37.252	0	PROCESSED	57541.3108796296	2016-06-02 07:27:40	54860	2009-01-29 00:00:00	54490.3089236111	2008-01-25 07:24:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021127	We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects.	EXTRAGALACTIC COMPACT SOURCES	7	A	RYAN HICKOX		USA	2	AO2	SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702038010/	Quick Look
170	NGC5548	214.4969	25.1266	213.929993	25.356783	201.998856	36.406453	31.93001973	70.4949274	285.8791	54310.1810648148	2007-07-29 04:20:44	54311.0209953704	2007-07-30 00:30:14	702042070	31.8099	30	31.8099	31.8099	0	31.8099	1	1	0	1	1	0	0	29.503	29.503	72.5279	1	PROCESSED	57539.3547569444	2016-05-31 08:30:51	54706	2008-08-28 00:00:00	54339.4245486111	2007-08-27 10:11:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021307	We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	2	AO2	NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042070/	Quick Look
171	NGC 1365	53.3968	-36.1347	52.919388	-36.301683	36.801187	-53.032832	237.94662462	-54.6022242	221.6565	54486.2300578704	2008-01-21 05:31:17	54490.0002083333	2008-01-25 00:00:18	702047010	160.5057	150	160.5057	160.5137	0	160.5137	2	2	0	2	1	0	0	146.8139	146.8139	325.6768	4	PROCESSED	57541.4786342593	2016-06-02 11:29:14	54883	2009-02-21 00:00:00	54515.5847800926	2008-02-19 14:02:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021314	We propose a 150 ksec observation of the Seyfert Galaxy NGC 1365. This galaxy have a unique set of properties: FeXXV and FeXXVI Kalpha and Kbeta absorption lines (the highest S/N detection so far among AGNs), rapidly varying cold absorber (nH variations of ~10^23/cm^2 in a few hours, changes from Compton-thick to Compton-thin in two days), a relativistic iron emission line. This new long observation will use at best the unique capabilities of Suzaku to constrain the dimensions of the absorbers, and, for the first time, will investigate the dynamics and physical conditions of the hot absorber responsible of the iron absorption lines. It is likely that an occultation will occur during the observation. This occultation would directly set the dimension of the X-ray source.	EXTRAGALACTIC COMPACT SOURCES	7	C	GUIDO RISALITI		USA	2	AO2	BLACK HOLE OCCULTATION AND OUTFLOW VARIABILITY IN NGC 1365	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702047010/	Quick Look
172	NGC 6300	259.2549	-62.8185	258.083078	-62.76377	263.641528	-39.613132	328.49505458	-14.05378352	296.7285	54390.5141087963	2007-10-17 12:20:19	54392.375162037	2007-10-19 09:00:14	702049010	82.577	80	82.577	82.577	0	82.577	2	2	0	2	1	0	0	105.5127	105.5127	160.7798	1	PROCESSED	57540.3276041667	2016-06-01 07:51:45	54770	2008-10-31 00:00:00	54403.3802083333	2007-10-30 09:07:30	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021331	Recent X-ray observations of Seyfert 2 galaxies have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by AGN Unified Schemes. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (60 ksec each) of four local bright Compton-thin Seyfert2s, selected from the Swift/BAT survey with a hard X-ray flux exceeding 1e-10 cgs to form a flux-limited sample. The unprecedented broad bandpass of Suzaku offers a unique tool to investigate the X-ray emission, placing strong constraints on the geometry and location of the reprocessing matter.	EXTRAGALACTIC COMPACT SOURCES	7	B	JAMES REEVES		USA	2	AO2	REVEALING THE REPROCESSING MATTER IN SEYFERT 2 GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702049010/	Quick Look
173	PKS1127-145	172.5274	-14.8245	171.896651	-14.548647	179.186436	-16.542663	275.2785401	43.63731171	115.9184	54799.7571180556	2008-11-29 18:10:15	54800.9523611111	2008-11-30 22:51:24	703004010	55.5451	40	55.5511	55.5451	0	55.5511	2	2	0	2	1	0	0	31.0123	31.0123	103.2488	0	PROCESSED	57544.5555208333	2016-06-05 13:19:57	54557	2008-04-01 00:00:00	54809.1987152778	2008-12-09 04:46:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030004	We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	3	AO3	REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703004010/	Quick Look
174	ESO 506-G027	189.6943	-27.3584	189.030338	-27.083667	200.074921	-21.229266	299.48164005	35.42851647	302.0467	54314.0460300926	2007-08-02 01:06:17	54315.2572222222	2007-08-03 06:10:24	702080010	41.7453	40	41.7533	41.7613	0	41.7453	1	1	0	1	1	0	0	38.2828	38.2828	104.6399	2	PROCESSED	57539.3906134259	2016-05-31 09:22:29	54710	2008-09-01 00:00:00	54340.5553125	2007-08-28 13:19:39	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021374	Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702080010/	Quick Look
175	NGC 788	30.262	-6.7593	29.638132	-7.000547	25.672425	-17.884233	165.15039638	-63.76864601	77.358	54660.0353819444	2008-07-13 00:50:57	54661.0516666667	2008-07-14 01:14:24	703032010	45.9073	40	45.9153	45.9073	0	45.9153	1	1	0	1	1	0	0	39.594	39.594	87.7999	0	PROCESSED	57543.0405902778	2016-06-04 00:58:27	55048	2009-08-05 00:00:00	54682.1458564815	2008-08-04 03:30:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031323	The classical unified model predicts only one type of Seyfert II (Sy2). Recent observations of SWIFT BAT-detected AGN found at least 4 classes of Sy2s: (1) objects with high column density and scattered soft x-rays, (2) Compton thick objects, (3) `hidden' AGN (Ueda et al. 2007), and (4) the `changing look' objects (Risaliti et al. 2006). The nature of these sources can only be revealed with high quality broad-band X-ray spectra from Suzaku. Thus, we are proposing 40ks observations for 2 of the brightest BAT AGN without high quality data, NGC 788, a type (3) object showing polarized optical broad lines, and NGC 3281, a classified (2) object. Such observations are necessary to build a reasonably large sample of high-quality, broad-band Sy2 spectra covering the range of X-ray/optical types.	EXTRAGALACTIC COMPACT SOURCES	7	A	RICHARD MUSHOTZKY		USA	3	AO3	SUZAKU OBSERVATIONS OF X-RAY BRIGHT TYPE II AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703032010/	Quick Look
176	Q0122-380	21.0759	-37.7461	20.512127	-38.006435	1.342949	-42.439189	271.91657466	-77.33125236	48.7944	54615.4511921296	2008-05-29 10:49:43	54616.2009722222	2008-05-30 04:49:24	703035010	28.481	25	28.481	28.489	0	28.497	2	2	0	2	1	0	0	26.8107	26.8107	64.7699	1	PROCESSED	57542.6524421296	2016-06-03 15:39:31	54999	2009-06-17 00:00:00	54633.6971759259	2008-06-16 16:43:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031334	Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates.	EXTRAGALACTIC COMPACT SOURCES	7	B	GEORGE CHARTAS		USA	3	AO3	A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703035010/	Quick Look
177	Q0551-3637	88.2026	-36.6158	87.768837	-36.625605	87.11791	-60.039805	242.36930247	-26.91846995	296.4731	54575.4385763889	2008-04-19 10:31:33	54575.6251041667	2008-04-19 15:00:09	703036010	3.8954	22	3.8954	3.8954	0	3.8954	1	1	0	1	1	0	0	3.773	3.773	16.0959	0	PROCESSED	57542.3345601852	2016-06-03 08:01:46	54979	2009-05-28 00:00:00	54588.1227314815	2008-05-02 02:56:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031334	Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	3	AO3	A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703036010/	Quick Look
178	Q0109-3518	17.9376	-35.0527	17.356449	-35.318066	0.204002	-38.849268	275.45528409	-80.96443984	40.3411	54606.0677199074	2008-05-20 01:37:31	54606.6772453704	2008-05-20 16:15:14	703037010	29.9585	18	29.9665	29.9585	0	29.9665	1	1	0	1	1	0	0	22.8339	22.8339	52.6559	1	PROCESSED	57542.5808101852	2016-06-03 13:56:22	54982	2009-05-31 00:00:00	54616.3810300926	2008-05-30 09:08:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031334	Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	3	AO3	A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703037010/	Quick Look
179	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
180	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
181	IC1586	11.9805	22.3783	11.316843	22.105657	19.903516	15.841027	121.86323541	-40.48615304	70.9045	55006.4686458333	2009-06-24 11:14:51	55007.0280555556	2009-06-25 00:40:24	704005010	23.5306	20	23.5306	24.3466	0	24.3546	2	2	0	2	1	0	0	22.2778	22.2778	48.3259	0	PROCESSED	57547.6510648148	2016-06-08 15:37:32	55385	2010-07-08 00:00:00	55019.1259259259	2009-07-07 03:01:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040049	We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	4	AO4	SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704005010/	Quick Look
182	3C120	68.2984	5.3555	67.633855	5.251051	67.433469	-16.402094	190.37315865	-27.39441526	237.4585	53775.1527199074	2006-02-09 03:39:55	53776.2433217593	2006-02-10 05:50:23	700001010	41.9321	160	41.9321	41.9321	41.9321	41.9321	2	2	2	2	1	0	0	34.0941	34.0941	94.2219	1	PROCESSED	57532.9769791667	2016-05-24 23:26:51	54247	2007-05-27 00:00:00	53906.2470601852	2006-06-20 05:55:46	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001003	Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	0	SWG	BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001010/	Quick Look
183	PKS2155-304	329.7191	-30.2247	328.99529	-30.464273	321.189186	-16.770975	17.73226544	-52.24760927	254.1358	53704.7749884259	2005-11-30 18:35:59	53706.3613888889	2005-12-02 08:40:24	700012010	63.9114	80	63.9194	63.9114	63.9194	63.9166	2	2	2	2	1	0	0	58.0114	58.0114	137.0498	3	PROCESSED	57532.3797685185	2016-05-24 09:06:52	54247	2007-05-27 00:00:00	54038.8920138889	2006-10-30 21:24:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001100	Jets in blazars are believed to be a powerful site of particle acceleration. TeV emitting blazars are very important, because we can study very end of electron distribution near the maximum energy by using X-ray spectrum, because X-ray emission is believed to be due to synchrotron emission from the higher energy electron. Comparison of spectral index between X-ray and TeV gives us a crucial information on these source, because this is very sensitive to the particle injection and rapid cooling. In order to maximize the capability of sensitive hard X-ray observations of Suzaku, we propose reserved TOO observations for the next six months of PV phase from the TeV emitting blazars established by HESS, selected from five candidates.	EXTRAGALACTIC COMPACT SOURCES	7	A	TADAYUKI TAKAHASHI		JAP	0	SWG-TOO	RESERVED TOO OBSERVATIONS OF SELECTED TEV-BRIGHT BLAZARS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700012010/	Quick Look
184	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
185	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
186	ESO 428-G014	109.1256	-29.3248	108.632746	-29.234716	116.992827	-50.987581	241.87528565	-7.96864273	123.1273	55516.1372569445	2010-11-16 03:17:39	55518.5508680556	2010-11-18 13:13:15	705008010	82.8873	80	82.9033	82.8873	0	82.9033	2	2	0	2	1	0	0	68.4518	68.4518	208.5016	2	PROCESSED	57554.1967361111	2016-06-15 04:43:18	55898	2011-12-03 00:00:00	55530.4256597222	2010-11-30 10:12:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050031	Non-Hidden Broad Line Region Seyfert 2 galaxies (NHBLR Sey2s) are classified as Seyfert 2 galaxies without broad Balmer lines even in the polarized light. One possible interpretation for the absence of broad lines is that NHBLR Sey2s are viewed from an extreme edge-on direction, so that the scattered light is obscured by the accretion torus. Hence observation of NHBLR Sey2s provides us the unique opportunity to investigate the densest region of the torus. We, therefore, propose 80 ksec observation of NHBLR Sey2 ESO 428-G014. High sensitivity throughout the 0.5-70 keV wide energy band of Suzaku allows us to strictly constrain the intrinsic X-ray luminosity and column density of the obscuring material. From our observation, we expect to derive more complete unified picture of AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	C	YOSHITO HABA		JAP	5	AO5	SUZAKU VIEW OF NON-HIDDEN BROAD LINE REGION SEYFERT 2 GALAXY ESO 428-G014	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705008010/	Quick Look
187	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
188	IRAS 01250+2832	21.9819	28.787	21.285155	28.528242	31.216552	18.139977	132.5132824	-33.40495941	250.843	55571.3211805556	2011-01-10 07:42:30	55572.5926388889	2011-01-11 14:13:24	705024010	57.5829	50	57.5829	57.5829	0	57.5829	2	2	0	2	1	0	0	54.8082	54.8082	109.8299	1	PROCESSED	57600.6088194444	2016-07-31 14:36:42	55962	2012-02-05 00:00:00	55595.2272569444	2011-02-03 05:27:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050074	We propose Suzaku XIS and HXD/PIN observations of two buried Active Galactic Nuclei(AGNs) at z=0.04 which are discovered by the AKARI mid-infrared all-sky survey. Both objects only show AGN features in AKARI near- and mid-infrared obsevations, while there are no clues of AGN presence in previous X-ray survey of ROSAT, radio 20cm, near-infrared photometries of 2MASS and detail optical spectroscopic data. These results indicate that a central engine of the AGN is completely buried and the nature of this population of AGNs is only poorly understood. Therefore, the hard X-ray observations is needed in order to confirm the AGN presence as well as to estimate the amount of absorption component and the AGN energy.	EXTRAGALACTIC COMPACT SOURCES	7	B	SHINKI OYABU		JAP	5	AO5	SUZAKU SEARCH FOR DIRECT EVIDENCE OF SUPER MASSIVE BLACK HOLES IN BURIED ACTIVE GALACTIC NUCLEI DISCOVERED BY AKARI	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705024010/	Quick Look
189	IRAS 00521-7054	13.5029	-70.6421	13.04558	-70.91316	316.631077	-63.690795	302.62218098	-46.48460341	40.2116	56431.8840740741	2013-05-19 21:13:04	56434.2543287037	2013-05-22 06:06:14	708005010	103.045	100	103.053	103.045	0	103.053	2	2	0	2	1	0	0	87.3405	87.3405	204.7697	1	PROCESSED	57611.3837152778	2016-08-11 09:12:33	56809	2014-06-01 00:00:00	56443.6034259259	2013-05-31 14:28:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080036	The existence of a broad iron line in AGN is still very debated. Amongst the several claims of detection of broad iron lines performed in the last decade, that of IRAS 00521-7054 is one of the most surprising. This type-2 object appears to show in fact an extremely broadened iron line, which would require a maximally rotating supermassive black hole and the presence of light bending. However, due to the lack of high-quality broadband studies, alternative explanations, as a clumpy-absorbers scenario, cannot be ruled out. The aim of this proposal is to perform a 100ks observation of IRAS 00521-7054. Thanks to its large band coverage and its good sensitivity in the iron-line region, Suzaku will allow us to clearly understand the origin of the intriguing spectral features of IRAS 00521-7054.	EXTRAGALACTIC COMPACT SOURCES	7	B	CLAUDIO RICCI		JAP	8	AO8	UNDERSTANDING THE ORIGIN OF THE PECULIAR X-RAY SPECTRAL FEATURES OF THE SEYFERT 2 IRAS 00521-7054	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708005010/	Quick Look
190	NGC 526A	20.9794	-35.0729	20.408158	-35.333404	3.010528	-40.076485	263.77547728	-79.45131683	257.0195	55578.7592939815	2011-01-17 18:13:23	55580.6404050926	2011-01-19 15:22:11	705044010	72.9346	70	72.9346	72.9346	0	72.9346	2	2	0	2	1	0	0	63.1372	63.1372	162.4977	2	PROCESSED	57600.6980324074	2016-07-31 16:45:10	55961	2012-02-04 00:00:00	55595.4905671296	2011-02-03 11:46:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051434	The Compton-thin NELG NGC 526a has large hard X-ray variability and likely an abnormally flat photon index, Gamma near 1.6. We request two observations of 70 ks each, spaced six months apart, to accurately constrain Compton reflection and obtain geometrical constraints on the accreting material to test Seyfert unification schemes, as well as constrain coronal power law parameters. Importantly, we will track long-term spectral variability to constrain the location and nature of the reflecting material. We also will resolve the moderately broad Fe K alpha line, which may indicate the presence of a truncated accretion disk, and thus constrain the amount of reflection off an accretion disk versus that from a torus.	EXTRAGALACTIC COMPACT SOURCES	7	C	ALEX MARKOWITZ		USA	5	AO5	COMPTON REFLECTION AND LONG-TERM SPECTRAL VARIABILITY IN THE SEYFERT AGN NGC 526A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705044010/	Quick Look
191	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
192	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
193	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
194	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
195	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
196	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
197	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
198	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
199	NGC5135	201.4174	-29.8897	200.719488	-29.629866	211.188294	-19.343803	311.72101463	32.39717213	286.1252	54284.2497800926	2007-07-03 05:59:41	54285.3057175926	2007-07-04 07:20:14	702005010	52.4964	50	52.4964	52.4964	0	52.4964	2	2	0	2	1	0	0	49.7837	49.7837	91.2209	2	PROCESSED	57539.1022222222	2016-05-31 02:27:12	54696	2008-08-18 00:00:00	54328.4497453704	2007-08-16 10:47:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020005	Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei.	EXTRAGALACTIC COMPACT SOURCES	7	A	HISAMITSU AWAKI		JAP	2	AO2	REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702005010/	Quick Look
200	NGC5643	218.1422	-44.2268	217.336243	-44.006582	230.485298	-27.635672	321.40267054	14.9878026	293.4229	54331.8795023148	2007-08-19 21:06:29	54332.9724421296	2007-08-20 23:20:19	702010010	42.8823	50	42.8903	42.8903	0	42.8823	2	2	0	2	1	0	0	40.8685	40.8685	94.386	2	PROCESSED	57539.6330902778	2016-05-31 15:11:39	54770	2008-10-31 00:00:00	54402.2016782407	2007-10-29 04:50:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020034	Seyfert 2 galaxies often have an nucleus obscured by thick matter. Risaliti et al. found that Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy s population by studying the distribution of absorbing column densities among Seyfert 2 galaxies. This result is important to discuss on the structure and evolution of active galactic nuclei. However, it is difficult to classify Seyfert 2 galaxies into Compton thick and thin objects only by using their X-ray spectra below 10 keV. Therefore, there may be Compton thin objects among Risaliti s Compton thick sample. In order to make the distribuion of the column density more reliable, we propose the Suzaku observations of heavily obscured AGNs with NH >1E25cm-2.	EXTRAGALACTIC COMPACT SOURCES	7	B	HISAMITSU AWAKI		JAP	2	AO2	SUZAKU OBSERVATIONS OF THE HEAVILY OBSCURED AGNS WITH NH>1E25 CM-2	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702010010/	Quick Look
201	NGC 7314	338.9055	-25.9984	338.214858	-26.257583	330.662233	-15.873025	27.22535085	-59.7013223	59.6979	54215.4316319444	2007-04-25 10:21:33	54217.9516666667	2007-04-27 22:50:24	702015010	109.0198	100	109.0198	109.0198	0	109.0198	2	2	0	2	1	0	0	92.2408	92.2408	217.7139	2	PROCESSED	57538.5280439815	2016-05-30 12:40:23	54744	2008-10-05 00:00:00	54230.4096527778	2007-05-10 09:49:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020037	We propose a Suzaku observation of the highly variable Seyfert 1.9 NGC 7314. The Fe K line in this object varies on a very short time scale (<10 keV) in contrast to Seyferts observed with Suzaku in the SWG time. The data will be used to search for a weak broad Fe K line to constrain the inner radius of an optically thick disk and to study the spectral variation on short time scales to elucidate the fundamental processes producing X-rays in the vicinity of the central black hole.	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	2	AO2	RAPID SPECTRAL X-RAY VARIABILITY IN THE SEYFERT GALAXY NGC 7314: UNDERSTANDING ENERGY RELEASE PROCESSES IN AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702015010/	Quick Look
202	IGR J21247+5058	321.1969	51.0428	320.772046	50.826527	353.918258	60.483587	93.38215801	0.42876214	108.8126	54206.5871759259	2007-04-16 14:05:32	54208.4613888889	2007-04-18 11:04:24	702027010	85.0319	80	85.0319	85.0399	0	85.0479	2	2	0	2	1	0	0	70.9709	70.9709	161.8949	2	PROCESSED	57538.4530671296	2016-05-30 10:52:25	54744	2008-10-05 00:00:00	54214.1071412037	2007-04-24 02:34:17	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020097	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	2	AO2	BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702027010/	Quick Look
203	MRK 1239	148.0816	-1.6118	147.44487	-1.376316	150.825441	-13.652204	239.27134701	38.21950621	286.5242	54226.0919907407	2007-05-06 02:12:28	54227.5973726852	2007-05-07 14:20:13	702031010	63.128	80	63.128	63.128	0	63.128	2	2	0	2	1	0	0	53.5944	53.5944	130.0619	2	PROCESSED	57615.5991435185	2016-08-15 14:22:46	54744	2008-10-05 00:00:00	54235.4602662037	2007-05-15 11:02:47	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020127	X-ray observations of "Hidden" narrow-line Seyfert 1 galaxies (NLS1s) have never been performed effectively, in spite of the fact that both obscuring material and nucleus of NLS1s are thought to be a crucial key to understand the fueling and accretion mechanisms, which may be directly related to the evolution of supermassive black holes and host galaxies. Hence,we propose 80 ksec observation of the candidates of hidden NLS1s Mrk 1239. Large effective area and unprecedented wide energy band of Suzaku allows us to strictly constrain the column density and covering fraction of obscuring matter, intrinsic power law slope, and its luminosity. From these observations, we expect to derive more complete unified picture of AGNs	EXTRAGALACTIC COMPACT SOURCES	7	B	YOSHITO HABA		JAP	2	AO2	SUZAKU VIEW OF "HIDDEN" NARROW-LINE SEYFERT 1 GALAXY MRK 1239	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702031010/	Quick Look
204	NGC 4593	189.9131	-5.3426	189.268208	-5.068085	191.201579	-0.987759	297.48049807	57.40434975	112.24	54449.1962384259	2007-12-15 04:42:35	54451.972349537	2007-12-17 23:20:11	702040010	118.8415	107	118.8415	118.8415	0	118.8415	2	2	0	2	1	0	0	108.976	108.976	239.7899	6	PROCESSED	57540.92	2016-06-01 22:04:48	54829	2008-12-29 00:00:00	54462.4425462963	2007-12-28 10:37:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021302	We propose a 80 ksec observation of the bright Seyfert 1 NGC 4593 to resolve the moderately relativistic Fe K line, and test for a truncated or ionized accretion disk. To achieve accurate modeling of the broad Fe line, Suzaku's broad bandpass is required to deconvolve the broadband emitting component and accurately constrain the continuum. NGC 4593 is one of the few Seyferts to also show evidence for Fe XXVI emission at 6.9 keV; we will use the XIS to confirm the line and constrain its origin. If the thin accretion disk is truncated or transitions to an ADAF, it would reveal NGC 4593 to be an analogue of low/hard-state X-ray Binaries.	EXTRAGALACTIC COMPACT SOURCES	7	C	ALEX MARKOWITZ		USA	2	AO2	DOES THE SEYFERT AGN NGC 4593 HAVE A TRUNCATED OR IONIZED ACCRETION DISK?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702040010/	Quick Look
205	NGC7582	349.5472	-42.3304	348.858747	-42.603943	331.723267	-34.368393	348.20905034	-65.68466064	49.5845	54221.7937384259	2007-05-01 19:02:59	54222.3176273148	2007-05-02 07:37:23	702052010	23.9412	25	23.9572	23.9412	0	23.9572	2	2	0	2	1	0	0	21.5816	21.5816	45.256	0	PROCESSED	57538.5368402778	2016-05-30 12:53:03	54695	2008-08-17 00:00:00	54228.073275463	2007-05-08 01:45:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021332	We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARCO CHIABERGE		USA	2	AO2	MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052010/	Quick Look
206	NGC7582	349.6446	-42.4137	348.956435	-42.687331	331.752163	-34.475865	347.94526846	-65.70277041	233.1822	54413.9093981482	2007-11-09 21:49:32	54414.6459490741	2007-11-10 15:30:10	702052030	29.3538	25	29.3538	29.3538	0	29.3538	2	2	0	2	1	0	0	24.4331	24.4331	63.6319	1	PROCESSED	57540.4723842593	2016-06-01 11:20:14	54790	2008-11-20 00:00:00	54423.1929398148	2007-11-19 04:37:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021332	We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARCO CHIABERGE		USA	2	AO2	MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052030/	Quick Look
207	NGC7582	349.6411	-42.4153	348.952917	-42.688928	331.748482	-34.476047	347.94523476	-65.69973119	236.7954	54420.0722337963	2007-11-16 01:44:01	54420.8960532407	2007-11-16 21:30:19	702052040	31.8955	25	31.8955	31.8955	0	31.8955	2	2	0	2	1	0	0	25.7806	25.7806	71.1719	0	PROCESSED	57540.5407060185	2016-06-01 12:58:37	54797	2008-11-27 00:00:00	54430.3041203704	2007-11-26 07:17:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021332	We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARCO CHIABERGE		USA	2	AO2	MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052040/	Quick Look
208	3C 33	17.2445	13.2796	16.584921	13.013252	20.958615	5.507742	129.4936436	-49.368548	249.2604	54460.3029282407	2007-12-26 07:16:13	54463.6390509259	2007-12-29 15:20:14	702059010	127.3677	100	127.3757	127.3757	0	127.3677	2	2	0	2	1	0	0	106.5885	106.5885	288.2036	7	PROCESSED	57541.0545833333	2016-06-02 01:18:36	54854	2009-01-23 00:00:00	54483.4886458333	2008-01-18 11:43:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021356	We propose a 100 ks Suzaku observation of the nucleus of the nearby (z=0.0597) FRII radio galaxy 3C 33, to constrain the nature of its Compton reflection component, and make an accurate measurement of its Fe Ka emission line. 3C 33 (awarded category-C time in Suzaku AO-1, not observed) is the only radio-loud AGN with evidence of Compton reflection in its low-energy (< 10 keV) spectrum, and so offers a unique opportunity to study both the soft- and hard-band properties of reflection. The HXD will allow us, for the first time, to constrain the nature of the Compton reflection component in 3C 33 and, when combined with the superb sensitivity of the XIS, will enable us to determine the line-of-sight geometry and structure of the reflecting region.	EXTRAGALACTIC COMPACT SOURCES	7	B	DANIEL EVANS		USA	2	AO2	CONSTRAINING THE REFLECTION PROPERTIES OF THE NARROW-LINE RADIO GALAXY 3C 33	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702059010/	Quick Look
209	Q1017+1055	155.041	10.671	154.377707	10.922699	152.99156	0.282434	230.36219873	50.83483368	121.1263	54431.9135185185	2007-11-27 21:55:28	54432.4376851852	2007-11-28 10:30:16	702064010	18.0486	20	18.0486	18.0486	0	18.0486	2	2	0	2	1	0	0	15.0316	15.0316	45.2819	0	PROCESSED	57540.6059606482	2016-06-01 14:32:35	54805	2008-12-05 00:00:00	54438.285150463	2007-12-04 06:50:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021361	The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars.	EXTRAGALACTIC COMPACT SOURCES	7	C	GEORGE CHARTAS		USA	2	AO2	AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702064010/	Quick Look
210	3C 273	187.2559	1.9961	186.616492	2.272457	185.868054	4.712799	289.92713501	64.30042167	293.1671	54281.0022569444	2007-06-30 00:03:15	54282.2661342593	2007-07-01 06:23:14	702070010	54.8927	67	54.8927	54.8927	0	54.8927	2	2	0	2	1	0	0	51.2592	51.2592	109.1439	1	PROCESSED	57539.0801388889	2016-05-31 01:55:24	54695	2008-08-17 00:00:00	54322.4904166667	2007-08-10 11:46:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021364	We propose a Suzaku campaign on the bright z=0.158 quasar 3C 273. The source exhibits a Seyfert-like X-ray spectrum when the luminosity is low but is dominated by emission from the jet in a high state. Suzaku will be able to measure the broadband spectrum, especially X-ray reprocessed features, with greater sensitivity than ever before. Decoupling and monitoring of the disk and jet components will enable detailed spectroscopy to help understand the disk-jet connection and the wider implications for AGN physics in general. The target is bright and well-suited because for most AGN either the disk or jet component dominates. For this pilot study we propose two 50 ks observations, one in each visibility window. The science goals cannot be achieved with existing data or other missions.	EXTRAGALACTIC COMPACT SOURCES	7	C	TAHIR YAQOOB		USA	2	AO2	EXPLORING THE ACCRETION DISK AND JET CONNECTION IN 3C 273 WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702070010/	Quick Look
211	SWIFT J0318.7+6828	49.4315	68.5395	48.26024	68.35635	69.167768	48.016071	135.6962435	9.37350025	42.3301	54365.4488078704	2007-09-22 10:46:17	54367.125162037	2007-09-24 03:00:14	702075010	77.1156	53	77.1396	77.1156	0	77.1396	2	2	0	2	1	0	0	70.6855	70.6855	144.7978	1	PROCESSED	57540.0779513889	2016-06-01 01:52:15	54770	2008-10-31 00:00:00	54403.1984490741	2007-10-30 04:45:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021372	The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702075010/	Quick Look
212	PHOENIX GALAXY	120.9921	5.0644	120.329999	5.206365	122.073674	-14.991802	216.72692126	18.43029643	304.6737	54222.3296296296	2007-05-02 07:54:40	54223.9585069445	2007-05-03 23:00:15	702111010	58.8677	50	58.8677	58.8677	0	58.8677	2	2	0	2	1	0	0	49.6978	49.6978	140.7239	5	PROCESSED	57538.5788078704	2016-05-30 13:53:29	54744	2008-10-05 00:00:00	54230.3771527778	2007-05-10 09:03:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022002	We propose a 50 ks Suzaku observation of the Seyfert galaxy UGC4203 (a.k.a. Mrk 1210), the ``Phoenix Galaxy''. It is one of the sources which have been discovered to change from Compton-thin to reflection-dominated states. The aim of the proposal is to understand the origin of this variation (i.e. as either due to flux or to NH variations) by measuring its column density and compare it to previous observations. Suzaku is unique for this task, because thanks to its broad band it may probe column densities up to several times 10^24 cm^-2 in this source, which has never been observed above 10 keV.	EXTRAGALACTIC COMPACT SOURCES	7	B	GIORGIO MATT		EUR	2	AO2	THE NATURE OF THE VARIATIONS OF STATE IN THE PHOENIX GALAXY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702111010/	Quick Look
213	IC4329A	207.3329	-30.3099	206.618741	-30.061746	216.345977	-17.776956	317.49868436	30.91898994	293.8517	54318.0289930556	2007-08-06 00:41:45	54318.8786226852	2007-08-06 21:05:13	702113020	30.6233	25	30.6233	30.6233	0	30.6233	2	2	0	2	1	0	0	25.7461	25.7461	73.384	3	PROCESSED	57539.4343287037	2016-05-31 10:25:26	54730	2008-09-21 00:00:00	54347.5971180556	2007-09-04 14:19:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022009	IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASSIMO CAPPI		EUR	2	AO2	SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113020/	Quick Look
214	IRAS18325-5926	279.2243	-59.4565	278.116624	-59.498471	275.782962	-36.20075	335.92469241	-21.3483138	281.9669	54399.3814699074	2007-10-26 09:09:19	54401.4169444444	2007-10-28 10:00:24	702118010	78.4348	80	78.4348	78.4428	0	78.4428	2	2	0	2	1	0	0	74.2917	74.2917	175.8357	0	PROCESSED	57540.4011458333	2016-06-01 09:37:39	54777	2008-11-07 00:00:00	54409.305474537	2007-11-05 07:19:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022025	We propose a 80 ks observation of the Seyfert galaxy IRAS 18325-5926. Previous observations show evidence for reflection from highly ionized matter, absorption features in the 8-10 keV band, and a possible roll-over of the continuum spectrum at around 30 keV. The observation goal is to elucidate the continuum roll-over and to investigate variability of the spectral features, which would have many important implications for the physical condition and the geometry of the accretion disc and the illuminating source. This study will provide crucial keys to understand the geometry of primary X-ray source and immediate surroundings. The broad-band coverage and the high sensitivity at the hard X-ray band provided by Suzaku are ideally suited to study this unique AGN.	EXTRAGALACTIC COMPACT SOURCES	7	C	KAZUTAMI MISAKI		EUR	2	AO2	HARD X-RAY SPECTRUM OF IRAS 18325-5926: REFLECTION FROM AN IONIZED DISC AND CONTINUUM ROLL-OVER	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702118010/	Quick Look
215	PKS0208-512	32.6864	-51.0102	32.231145	-51.245187	0.269734	-58.029766	276.09849974	-61.78596913	230.2146	54814.3149074074	2008-12-14 07:33:28	54815.4793171296	2008-12-15 11:30:13	703002010	51.9594	40	51.9834	51.9594	0	51.9834	2	2	0	2	1	0	0	42.559	42.559	100.5999	0	PROCESSED	57544.9648032407	2016-06-05 23:09:19	54557	2008-04-01 00:00:00	54826.3087268518	2008-12-26 07:24:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030004	We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	3	AO3	REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703002010/	Quick Look
216	4C73.08	147.4414	73.2521	146.291521	73.485172	114.906674	54.77086	138.04435007	38.07252036	100.3847	54786.9238888889	2008-11-16 22:10:24	54788.4946643518	2008-11-18 11:52:19	703018010	81.3752	80	81.3752	81.3752	0	81.3752	2	2	0	2	1	0	0	72.4533	72.4533	135.692	0	PROCESSED	57544.4300694444	2016-06-05 10:19:18	55164	2009-11-29 00:00:00	54798.0487152778	2008-11-28 01:10:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030063	Suzaku observation of two giant radio galaxies, 4C 73.08 and 3C 35, are proposed. In 80 ks exposure on the individual target, inverse Compton X-ray emission from their lobes is detected with high signal statistics. As a result, the energy densities of electrons and magnetic field in these lobesare precisely determined. The size of these radio galaxies are significantly lager than that of the previous sample. Therefore, the size dependence of energetics in the lobes will be investigated	EXTRAGALACTIC COMPACT SOURCES	7	C	YUICHI YAJI		JAP	3	AO3	SUZAKU OBSERVATION OF LOBES OF GIANT RADIO GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703018010/	Quick Look
217	NGC 4051	180.7952	44.5393	180.156844	44.817625	159.255387	40.346248	148.86124636	70.08047443	126.4079	54793.7	2008-11-23 16:48:00	54795.572025463	2008-11-25 13:43:43	703023020	78.3855	70	78.3935	78.3855	0	78.3939	1	1	0	1	1	0	0	62.7604	62.7604	161.7358	0	PROCESSED	57544.5729513889	2016-06-05 13:45:03	54557	2008-04-01 00:00:00	54811.74875	2008-12-11 17:58:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031014	The powerful combination of Principal Components Analysis with time-resolved X-ray spectroscopy of Seyfert AGN has shown strong evidence that changes in a complex absorber are the origin of much of observed AGN spectral and flux variability. Large column, high ionization layers of gas may arise in a disk wind, representing a significant new, and possibly dominant, component, responsible for shaping the X-ray spectrum of AGN. The broad bandpass of Suzaku gives us a unique opportunity to model primary and reflected continua and the effects of variable absorbing zones, and test wind and other models. We propose a long 340 ks exposure on the NLSy1 NGC 4051 whose large amplitude of variability and well-studied complex absorption will test those models to the limit	EXTRAGALACTIC COMPACT SOURCES	7	A	TRACEY TURNER		USA	3	AO3	DECONSTRUCTING SEYFERT SPECTRA - TIME FOR A PARADIGM SHIFT?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703023020/	Quick Look
218	SMC X-1	19.2829	-73.4465	18.951639	-73.709645	312.337269	-66.476032	300.41108523	-43.55576838	356.8796	55658.8646759259	2011-04-07 20:45:08	55659.2447106482	2011-04-08 05:52:23	706030010	18.4662	18	18.4662	18.55	0	18.5448	1	1	0	1	1	0	0	15.5577	15.5577	32.8239	0	PROCESSED	57601.4235185185	2016-08-01 10:09:52	56040	2012-04-23 00:00:00	55673.2343055556	2011-04-22 05:37:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030010/	Quick Look
219	SMC X-1	19.2476	-73.446	18.915775	-73.709202	312.329896	-66.466401	300.42473809	-43.55764171	6.4299	55669.2561805556	2011-04-18 06:08:54	55669.705775463	2011-04-18 16:56:19	706030020	17.2769	18	17.2769	17.2849	0	17.4844	2	2	0	1	1	0	0	17.6646	17.6646	38.8159	0	PROCESSED	57601.5313657407	2016-08-01 12:45:10	56058	2012-05-11 00:00:00	55691.1543171296	2011-05-10 03:42:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030020/	Quick Look
220	NGC 7172	330.5062	-31.8708	329.778877	-32.112297	321.223494	-18.549637	15.12698367	-53.06449716	59.7356	54611.0658680556	2008-05-25 01:34:51	54612.8558217593	2008-05-26 20:32:23	703030010	82.2797	80	82.2797	82.2877	0	82.2877	2	2	0	2	1	0	0	71.7465	71.7465	154.6338	0	PROCESSED	57542.6661805556	2016-06-03 15:59:18	54999	2009-06-17 00:00:00	54633.7016203704	2008-06-16 16:50:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031322	X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s.	EXTRAGALACTIC COMPACT SOURCES	7	A	VALENTINA BRAITO		USA	3	AO3	THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703030010/	Quick Look
221	NGC 3281	157.9591	-34.9074	157.391937	-34.649823	175.881528	-40.345828	273.03211125	19.73409342	278.2413	54607.8508449074	2008-05-21 20:25:13	54609.2287615741	2008-05-23 05:29:25	703033010	46.234	40	46.242	46.25	0	46.234	2	2	0	2	1	0	0	41.4549	41.4549	119.038	0	PROCESSED	57542.6257175926	2016-06-03 15:01:02	54988	2009-06-06 00:00:00	54620.2890162037	2008-06-03 06:56:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031323	The classical unified model predicts only one type of Seyfert II (Sy2). Recent observations of SWIFT BAT-detected AGN found at least 4 classes of Sy2s: (1) objects with high column density and scattered soft x-rays, (2) Compton thick objects, (3) `hidden' AGN (Ueda et al. 2007), and (4) the `changing look' objects (Risaliti et al. 2006). The nature of these sources can only be revealed with high quality broad-band X-ray spectra from Suzaku. Thus, we are proposing 40ks observations for 2 of the brightest BAT AGN without high quality data, NGC 788, a type (3) object showing polarized optical broad lines, and NGC 3281, a classified (2) object. Such observations are necessary to build a reasonably large sample of high-quality, broad-band Sy2 spectra covering the range of X-ray/optical types.	EXTRAGALACTIC COMPACT SOURCES	7	A	RICHARD MUSHOTZKY		USA	3	AO3	SUZAKU OBSERVATIONS OF X-RAY BRIGHT TYPE II AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703033010/	Quick Look
222	3C279	194.0699	-5.7328	193.422743	-5.462367	195.164566	0.26232	305.15066173	57.11808922	113.6425	54854.8772222222	2009-01-23 21:03:12	54856.125162037	2009-01-25 03:00:14	703049020	56.937	200	56.937	56.937	0	56.937	2	2	0	2	1	0	0	12.6263	12.6263	107.7799	2	PROCESSED	57545.3327777778	2016-06-06 07:59:12	55328	2010-05-12 00:00:00	54880.5584259259	2009-02-18 13:24:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031346	We propose a 200 ks observation of 3C279, the archetypal EGRET blazar to be conducted simultaneously with GLAST as well as many other facilities, with the goal of obtaining broadband spectra and light-curves. The flux in all observable bands is known to be rapidly variable, but the information regarding the correlation between the time history of flux in various bands is limited, and the proposed observations are designed to remedy this shortcoming. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles.	EXTRAGALACTIC COMPACT SOURCES	7	A	GRZEGORZ MADEJSKI		USA	3	AO3	SUZAKU AND GLAST OBSERVATIONS OF 3C279	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703049020/	Quick Look
223	PKS1549-79	239.2836	-79.2302	237.405254	-79.084019	259.929288	-56.865354	311.18735019	-19.47008602	310.7048	54752.6495833333	2008-10-13 15:35:24	54754.9009375	2008-10-15 21:37:21	703059010	82.1755	80	82.197	82.1835	0	82.1755	2	2	0	2	1	0	0	79.9736	79.9736	194.4977	2	PROCESSED	57544.1654398148	2016-06-05 03:58:14	55148	2009-11-13 00:00:00	54780.6256597222	2008-11-10 15:00:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032005	Galaxy merger models predict rapid black hole growth and strong outflows late in the merger as the accretion rate increases. PKS1549-79 is a powerful, low redshift, high accretion rate active galaxy which has undergone a recent merger. It is therefore an ideal object to test our understanding of galaxy activity and mergers and for studying feedback between AGN and their host galaxies. We propose an 80 ksec Suzaku observation to: (i) determine the amount and ionisation state of the nuclear obscuring material in PKS1549-79 and hence confirm its status as a local proto-quasar; (ii) search for the massive, probably highly ionised, outflowing wind predicted by galaxy evolution models and hence complete a census of outflow components in this object; and (iii) quantify the high energy spectrum.	EXTRAGALACTIC COMPACT SOURCES	7	B	PAUL O'BRIEN		EUR	3	AO3	UNVEILING PKS 1549-79 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703059010/	Quick Look
224	MRK 573	26.0161	2.2904	25.370891	2.039517	24.959775	-7.914401	148.3199793	-57.9636564	249.71	55217.5861226852	2010-01-21 14:04:01	55219.0328587963	2010-01-23 00:47:19	704002010	64.3118	60	64.3118	64.3118	0	64.3118	2	2	0	2	1	0	0	53.7471	53.7471	124.992	0	PROCESSED	57550.3256944445	2016-06-11 07:49:00	55612	2011-02-20 00:00:00	55245.753599537	2010-02-18 18:05:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040017	Monte Carlo simulation is one of the best tools to study the complex spectra of Compton-thick AGNs and to figure out the relation between their nuclear structures and X-ray spectra. We have simulated X-ray spectra of Compton-thick AGNs obscured by an accretion torus, and found that observed spectra of Compton thick objects, Mrk 3 and NGC 2273 are well reproduced by the simulated X-ray spectra. Furthermore, our simulation predicts that there are many obscured AGNs with a heavily absorbed reflection component. Their spectra are similar to that predicted from synthesis modeling of the Cosmic X-ray Background. We propose Suzaku observations of candidates of the Compton thick AGNs, Mrk 573 and Mrk 78.	EXTRAGALACTIC COMPACT SOURCES	7	C	HISAMITSU AWAKI		JAP	4	AO4	SEARCH FOR COMPTON THICK AGNS WITH A HEAVILY ABSORBED REFLECTION COMPONENT	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704002010/	Quick Look
225	SWIFT J2248.8+1725	342.1903	17.444	341.576565	17.179413	350.711211	23.025613	85.72592105	-36.41328844	248.2402	56997.6938888889	2014-12-06 16:39:12	56999.668287037	2014-12-08 16:02:20	709004010	78.0938	80	78.0938	78.0938	0	78.0938	2	2	0	2	1	0	0	68.8266	68.8266	170.56	1	PROCESSED	57617.5240046296	2016-08-17 12:34:34	57460	2016-03-13 00:00:00	57092.3224652778	2015-03-11 07:44:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090018	We propose to observe two hard X-ray bright Seyfert galaxies with a highly accreting small BH. This class of objects is of importance in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be fundamental pieces of information to better understand accretion physics and ``feedback'' processes in galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	C	YUICHI TERASHIMA		JAP	9	AO9	ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED LOW-MASS SEYFERTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709004010/	Quick Look
226	1216-015	184.787	-1.8118	184.145709	-1.534245	185.108736	0.239101	286.61259693	60.03288042	293.8466	55010.1063773148	2009-06-28 02:33:11	55010.6043287037	2009-06-28 14:30:14	704006010	20.7779	20	20.7779	20.7859	0	20.7859	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57547.6897337963	2016-06-08 16:33:13	55388	2010-07-11 00:00:00	55020.3653009259	2009-07-08 08:46:02	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040049	We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	4	AO4	SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704006010/	Quick Look
227	UGC 12741	355.4449	30.6414	354.81812	30.364038	9.270542	29.65828	105.65559107	-29.88276227	64.429	54989.5219560185	2009-06-07 12:31:37	54990.6711111111	2009-06-08 16:06:24	704014010	47.9458	40	47.9538	47.9458	0	47.9458	1	1	0	1	1	0	0	41.5244	41.5244	99.2799	0	PROCESSED	57547.5132060185	2016-06-08 12:19:01	55367	2010-06-20 00:00:00	55001.0091435185	2009-06-19 00:13:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040060	Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe three Compton thick AGN candidates in the 22 months BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	4	AO4	DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704014010/	Quick Look
228	NGC985	38.6279	-8.738	38.014145	-8.956444	33.218289	-22.635173	180.72422437	-59.4803664	62.3866	55027.6174884259	2009-07-15 14:49:11	55028.5925231482	2009-07-16 14:13:14	704042010	31.9969	30	31.9969	32.0063	0	32.0063	2	2	0	2	1	0	0	25.7241	25.7241	84.2379	1	PROCESSED	57547.8515856482	2016-06-08 20:26:17	55406	2010-07-29 00:00:00	55040.2752430556	2009-07-28 06:36:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041414	We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc.	EXTRAGALACTIC COMPACT SOURCES	7	B	EZEQUIEL TREISTER		USA	4	AO4	THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704042010/	Quick Look
229	NGC 3431	162.8114	-17.015	162.196181	-16.749458	171.110311	-22.386386	266.03803779	37.10135134	298.5009	56089.5660648148	2012-06-11 13:35:08	56091.5571412037	2012-06-13 13:22:17	707012010	65.6756	70	65.6756	65.6756	0	65.6756	2	2	0	2	1	0	0	59.8819	59.8819	171.9959	2	PROCESSED	57605.6909259259	2016-08-05 16:34:56	56473	2013-06-30 00:00:00	56106.3662384259	2012-06-28 08:47:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070067	The nature of the hard X-ray emission of many AGN remains ill-understood. Using the latest 70 month Swift/BAT sky survey, we have selected optically-classified Seyfert 2s with a very hard BAT photon index (Gamma<1.4). The BAT energy range is not strongly affected by obscuration unless the column is Compton-thick. The selected sources are radio-quiet, arguing against jet-dominated non-thermal spectra. The cause of a low Gamma is unknown, but may include high or atypical obscuration, non-thermal X-ray emission without associated radio/optical jets or the presence of electron coronae with temperatures or optical depths higher than average. Our aim is to observe two of the hardest Seyfert 2s (neither of which has prior pointed observations below 10 keV) with Suzaku to elucidate their nature.	EXTRAGALACTIC COMPACT SOURCES	7	A	POSHAK GANDHI		JAP	7	AO7	WHAT IS THE NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707012010/	Quick Look
230	NGC4102	181.5322	52.6534	180.899339	52.931664	153.57589	47.373492	138.20676485	63.11040703	305.2196	54981.0678009259	2009-05-30 01:37:38	54983.4203009259	2009-06-01 10:05:14	704057010	105.5579	100	105.5819	105.5579	0	105.5659	2	2	0	2	1	0	0	97.2802	97.2802	203.2139	2	PROCESSED	57547.4983912037	2016-06-08 11:57:41	55363	2010-06-16 00:00:00	54994.4413541667	2009-06-12 10:35:33	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042014	The nature of Low Ionization Nuclear Emission-line Region (LINER) galaxies has been the subject of a strong controversy. The distinction between LINER nuclei and other families of Active Galactic Nuclei (AGN) can be due to different amounts and/or properties of the obscuring material. A high population of LINERs are Compton-thick candidates. However the Equivalent Width (EW) of the FeKa emission line are lower than those measured for Compton-thick AGN. We propose to use the unprecedented sensitivity of HXD and XIS on board Suzaku to study NGC4102, one of the brightest LINER in the 36-month Swift/BAT survey. NGC4102 is a Compton-thick LINER candidate with EW(FeKa)<500keV, it is therefore an ideal case to investigate the properties of absorption and the FeKa emission line.	EXTRAGALACTIC COMPACT SOURCES	7	B	OMAIRA GONZALEZ-MARTIN		EUR	4	AO4	PROBING COMPTON-THICK OBSCURATION AND LOW EW(FEKA) OF LINERS: THE CASE OF NGC4102	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704057010/	Quick Look
231	NGC3516	166.8656	72.6213	166.014761	72.891861	123.359499	58.056735	133.14023939	42.38468378	135.8338	55132.2328125	2009-10-28 05:35:15	55137.5272453704	2009-11-02 12:39:14	704062010	251.3555	250	251.3795	251.3715	0	251.3555	2	2	0	2	1	0	0	190.8372	190.8372	333.01	5	PROCESSED	57549.2037268518	2016-06-10 04:53:22	54922	2009-04-01 00:00:00	55152.2729398148	2009-11-17 06:33:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	046003	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	4	AO4	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704062010/	Quick Look
232	ARK 347	181.0952	20.2476	180.45595	20.52594	172.634722	18.942585	243.01628342	77.22827936	294.4295	55377.99625	2010-06-30 23:54:36	55378.8668171296	2010-07-01 20:48:13	705002010	38.9726	40	38.9886	38.9726	0	38.9886	2	2	0	2	1	0	0	35.9876	35.9876	75.2099	0	PROCESSED	57552.4401851852	2016-06-13 10:33:52	55772	2011-07-30 00:00:00	55404.2387268518	2010-07-27 05:43:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050003	We propose to observe two Swift/BAT selected obscured AGNs with significant scattered emission, Mrk 18 and Ark 347. Hard X-ray selected AGNs show some peculiar characteristics compared to optically selected ones such as weak scattering emission from the opening part of the putative torus and weak plasma emission in the soft X-ray band. The targets are Swift/BAT selected AND show significant scattered emission, which are poorly explored with Suzaku so far. Our aims are to constrain the geometrical structure of the obscuring matter based on broad-band X-ray spectra and compare them with other hard X-ray or optically selected obscured AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	5	AO5	THE STRUCTURE OF COMPTON-THIN AGNS WITH SIGNIFICANT SCATTERED EMISSION SELECTED BY SWIFT/BAT	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705002010/	Quick Look
233	EMS0873	200.796	29.7234	200.211284	29.984115	186.018841	35.27496	55.1881509	82.55574598	136.0743	55527.7704976852	2010-11-27 18:29:31	55528.2800231482	2010-11-28 06:43:14	705029010	22.7849	20	22.7849	22.7849	0	22.7849	1	1	0	1	1	0	0	20.8106	20.8106	44.0079	2	PROCESSED	57554.227974537	2016-06-15 05:28:17	55903	2011-12-08 00:00:00	55536.9832523148	2010-12-06 23:35:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050126	Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects.	EXTRAGALACTIC COMPACT SOURCES	7	C	YASUYUKI TANAKA		JAP	5	AO5	SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705029010/	Quick Look
234	CEN A S LOBE NO. 4	196.751	-45.1436	196.031726	-44.876448	214.740849	-34.712794	305.81117883	17.64110832	288.0039	55421.3479282407	2010-08-13 08:21:01	55421.67375	2010-08-13 16:10:12	705035010	20.642	20	20.642	20.65	0	20.658	1	1	0	1	1	0	0	18.9643	18.9643	28.1439	0	PROCESSED	57552.9465277778	2016-06-13 22:43:00	55803	2011-08-30 00:00:00	55435.1577314815	2010-08-27 03:47:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051401	We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays).	EXTRAGALACTIC COMPACT SOURCES	7	B	GRZEGORZ MADEJSKI		USA	5	AO5	SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705035010/	Quick Look
235	IRAS 00397-1312	10.5707	-12.9503	9.941553	-13.224287	4.464578	-16.066781	113.89016485	-75.66108211	246.4295	55558.1361342593	2010-12-28 03:16:02	55560.2501388889	2010-12-30 06:00:12	705046010	83.7928	90	83.7928	83.7928	0	83.7928	2	2	0	2	1	0	0	71.9314	71.9314	182.6317	1	PROCESSED	57632.5965856482	2016-09-01 14:19:05	56040	2012-04-23 00:00:00	55670.3615046296	2011-04-19 08:40:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051441	We propose two Suzaku-HXD observations of two ULIRGs hosting a deeply buried AGN. These two objects are expected to host a powerful AGN in the luminosity range of quasars, based on solid evidence from mid-IR Spitzer spectroscopy. However, these sources are completely buried behind a screen of dust with column density in excess of 10^24 cm^-2, so not only the primary emission below 10 keV is obscured, but the reflected emission, usually ascribed to a circumnuclear "torus", is also absent. This suggests a complete spherical coverage of the X-ray source along all directions. The unique capabilities of Suzaku at high energies will allow to confirm the existence of these objects, representing the most extreme examples of buried AGNs, both in terms of obscuration and of intrinsic luminosity.	EXTRAGALACTIC COMPACT SOURCES	7	C	GUIDO RISALITI		USA	5	AO5	BURIED QUASAR 2S INSIDE ULIRGS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705046010/	Quick Look
236	NGC 4945	196.3415	-49.5274	195.611435	-49.259681	217.040288	-38.699914	305.25336122	13.28155854	286.7821	55386.9936226852	2010-07-09 23:50:49	55388.2626388889	2010-07-11 06:18:12	705047020	44.1517	40	44.1517	44.1597	0	44.1517	2	2	0	2	1	0	0	40.1612	40.1612	109.434	0	PROCESSED	57552.6167824074	2016-06-13 14:48:10	55777	2011-08-04 00:00:00	55411.4916898148	2010-08-03 11:48:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051442	We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval.	EXTRAGALACTIC COMPACT SOURCES	7	B	GUIDO RISALITI		USA	5	AO5	HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047020/	Quick Look
237	NGC 4945	196.2918	-49.5144	195.562046	-49.246615	216.996084	-38.704359	305.2209968	13.29631795	319.7988	55438.8990277778	2010-08-30 21:34:36	55439.9896990741	2010-08-31 23:45:10	705047040	39.3859	40	39.3859	39.3859	0	39.3859	2	2	0	2	1	0	0	35.7823	35.7823	94.2239	0	PROCESSED	57553.267962963	2016-06-14 06:25:52	55815	2011-09-11 00:00:00	55449.2596296296	2010-09-10 06:13:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051442	We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval.	EXTRAGALACTIC COMPACT SOURCES	7	B	GUIDO RISALITI		USA	5	AO5	HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047040/	Quick Look
238	ESP 39607	11.5922	-40.0968	10.997666	-40.369881	351.254657	-40.701682	307.24150307	-76.98900447	243.1952	55549.7680208333	2010-12-19 18:25:57	55551.3175810185	2010-12-21 07:37:19	705048010	60.6687	60	60.6927	60.6687	0	60.6847	2	2	0	2	1	0	0	48.9555	48.9555	133.8399	3	PROCESSED	57554.5018402778	2016-06-15 12:02:39	55960	2012-02-03 00:00:00	55593.2278472222	2011-02-01 05:28:06	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051443	We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec.	EXTRAGALACTIC COMPACT SOURCES	7	C	WAYNE BAUMGARTNER		USA	5	AO5	SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705048010/	Quick Look
239	3C 433	320.9422	25.055	320.383545	24.83969	333.197862	37.998992	74.46917661	-17.70913692	252.1178	55506.5663310185	2010-11-06 13:35:31	55508.0953472222	2010-11-08 02:17:18	705050010	62.5009	60	62.54	62.5009	0	62.54	2	2	0	2	1	0	0	44.4271	44.4271	132.0698	0	PROCESSED	57554.0198958333	2016-06-15 00:28:39	55890	2011-11-25 00:00:00	55524.1485416667	2010-11-24 03:33:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051443	We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec.	EXTRAGALACTIC COMPACT SOURCES	7	C	WAYNE BAUMGARTNER		USA	5	AO5	SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705050010/	Quick Look
240	4U 1344-60	206.8966	-60.619	206.036622	-60.369696	231.500761	-45.327278	309.76861534	1.50528265	97.6008	55572.7924189815	2011-01-11 19:01:05	55575.4751273148	2011-01-14 11:24:11	705058010	93.8773	100	93.9013	93.8933	0	93.8773	2	2	0	2	1	0	0	79.5617	79.5617	231.7537	3	PROCESSED	57600.6768865741	2016-07-31 16:14:43	55975	2012-02-18 00:00:00	55607.6933333333	2011-02-15 16:38:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052018	We propose a 100 ks Suzaku observation of 4U 1344-60, a poorly studied (because at low Galactic latitude) but bright (about 2 millicrabs) AGN which showed, in an XMM-Newton observation, a strong relativistic disk iron line. The main aim of the proposal is to determine in detail the parameters of the disk, which is possible only with a high quality broad band observation which permits to control the continuum beneath the line. Presently, only Suzaku has the right combination of sensitivity, energy resolution and broad band coverage to achieve this objective.	EXTRAGALACTIC COMPACT SOURCES	7	C	JIRI SVOBODA		EUR	5	AO5	4U 1344-60: A BRIGHT AGN WITH A STRONG RELATIVISTIC IRON LINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705058010/	Quick Look
241	MRK 205	185.2459	75.2485	184.69782	75.525765	124.91832	63.698525	125.52269394	41.72619699	309.3435	55338.764849537	2010-05-22 18:21:23	55340.8203125	2010-05-24 19:41:15	705062010	100.9605	126	100.9685	100.9605	0	100.9685	2	2	0	2	1	0	0	91.9525	91.9525	177.5778	0	PROCESSED	57551.6334606482	2016-06-12 15:12:11	55723	2011-06-11 00:00:00	55355.4313773148	2010-06-08 10:21:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052026	Mrk 205 (z=0.071) is a ``bare'' radio-quiet quasar, showing a peculiar continuum and FeK complex. From our analysis of past XMM-Newton observations, it shows a prominent and variable soft excess down to a two-day timescale. In 2000, an unusual FeK profile was found with an unresolved narrow line at 6.4keV and a broadened line centered at 6.7keV; while in 2006 a broad line has been observed near 6.4keV with a visible energy shift to 6.5keV occurring when the source flux increased. Our aims are to: (i) determine the FeK origin from its profile, and its possible variability on sub-orbital time-scales, (ii) to obtain an unprecedented simultaneous measurement of the Compton hump which is critical for modelling the true FeK profile (iii) and hence to infer a global picture of this object.	EXTRAGALACTIC COMPACT SOURCES	7	B	DELPHINE PORQUET		EUR	5	AO5	PROBING THE ORIGIN OF THE FEK COMPLEX IN THE ``BARE'' NUCLEUS OF MRK205.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705062010/	Quick Look
242	WISE J1819+4532	274.9137	45.5584	274.555701	45.535406	279.54226	68.836144	73.38480627	24.31157427	77.6532	56020.3333333333	2012-04-03 08:00:00	56021.0070833333	2012-04-04 00:10:12	707038010	30.8819	30	30.8819	30.8819	0	30.8819	2	2	0	2	1	0	0	27.564	27.564	58.2039	0	PROCESSED	57605.0974537037	2016-08-05 02:20:20	56399	2013-04-17 00:00:00	56033.2380787037	2012-04-16 05:42:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071443	We request a 30-ks observation of WISE J1819+4532, an extreme WISE-selected AGN at z=2.031. This source stands out even amongst the rare WISE-selected sources we have been targeting: at mid-IR wavelengths, WISE J1819+4532 is ~10x brighter than similarly selected WISE sources, and more than 50x brighter than extreme Spitzer-selected sources. Assuming the local mid-IR to hard X-ray correlations, the implied intrinsic hard X-ray luminosity is L(2-10)~3e46 erg/s. WISE J1819+4532 is optically faint and the optical spectrum shows a typical obscured AGN with narrow emission lines. However, the object is infrared bright and the near-IR spectrum shows broad H-alpha emission. This implies that WISE J1819+4532 is a rare example of a an extremely luminous, semi-obscured AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	DANIEL STERN		USA	7	AO7	WISE J1819+4532: AN OBSCURED, HYPERLUMINOUS ULIRG/AGN AT Z~2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707038010/	Quick Look
243	NGC 4785	193.3693	-48.746	192.657492	-48.474679	214.374181	-38.980118	303.27856941	14.12437615	296.8629	56495.4767013889	2013-07-22 11:26:27	56496.6341782407	2013-07-23 15:13:13	708003010	79.3882	70	79.3882	79.3962	0	79.3882	2	2	0	2	1	0	0	70.777	70.777	99.994	0	PROCESSED	57611.9465972222	2016-08-11 22:43:06	56876	2014-08-07 00:00:00	56509.7469907407	2013-08-05 17:55:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080027	At faint fluxes, the Swift/BAT AGN survey is uncovering sources with very hard photon indices (Gamma) above 10 keV. The origin of a low Gamma in the hard band is ill-understood, but may include high/atypical obscuration, non-thermal X-rays without radio jets, or electron coronae with high temperatures or optical depths. In AO7, we observed two such Seyfert 2s and discovered Compton-thick obscuration in one source, and a buried AGN spectrum with no reflection or high-energy cutoff in the other. The hard BAT Gamma values thus have a variety of origins, and our strategy is very effective in selecting objects with interesting spectra. Here, we propose to observe two hardest sources (Gamma<~1) with no prior X-ray observations below 10 keV in order to shed light on the nature of this population.	EXTRAGALACTIC COMPACT SOURCES	7	A	POSHAK GANDHI		JAP	8	AO8	THE VARIED NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708003010/	Quick Look
244	1FGL J1311.7-3429	197.9423	-34.512	197.244044	-34.24657	210.304099	-24.759106	307.68226276	28.17214982	298.263	55774.7002314815	2011-08-01 16:48:20	55776.7362847222	2011-08-03 17:40:15	706001010	82.4771	80	82.4771	82.4771	0	82.4771	2	2	0	2	1	0	0	70.3737	70.3737	175.8638	2	PROCESSED	57602.7690046296	2016-08-02 18:27:22	56219	2012-10-19 00:00:00	55851.4595601852	2011-10-17 11:01:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060003	We propose Suzaku observations of "unusual" Fermi-LAT sources 1FGL J1311.7 and 1FGL J2339.7, which are extremely bright in gamma-ray (> 30 sigma detection), but are as-yet unidentified even after two-year accumulation of Fermi-LAT data. Previous Suzaku observation revealed a highly variable X-ray source at the position of 1FGL J1311.7, but both spectral and temporal features do not resemble that of blazars or the gamma-ray pulsars. Meanwhile, an X-ray counterpart of 1FGL J2339.7 shows extremely hard spectrum with its photon index 1.1, which seems to connect smoothly with a bump feature around 2GeV. We will characterize variability and spectral properties of these peculiar X-ray counterparts and firmly understand the nature/origin of "new-type" GeV gamma-ray sources.	EXTRAGALACTIC COMPACT SOURCES	7	B	JUN KATAOKA		JAP	6	AO6	SUZAKU OBSERVATIONS OF "NEW-TYPE'' GAMMA-RAY SOURCES DETECTED WITH FERMI-LAT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706001010/	Quick Look
245	1FGL J1946.7-5404	296.6052	-54.0506	295.618874	-54.173159	288.105396	-32.270844	343.89458124	-29.55670998	268.6577	55865.7799074074	2011-10-31 18:43:04	55866.783599537	2011-11-01 18:48:23	706026010	42.3959	40	42.3959	42.3988	0	42.3988	2	2	0	2	1	0	0	54.8833	54.8833	86.7079	0	PROCESSED	57603.6796990741	2016-08-03 16:18:46	56246	2012-11-15 00:00:00	55879.1861574074	2011-11-14 04:28:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060084	In this proposal, we'd like to make a suggestion of 2 "steady" unassociated Fermi-LAT gamma-ray sources with Suzaku. 2-year Fermi-LAT observation detected 2412 sources, but 1194 sources are still unassociated. Proposed objects are located at high Galactic latitude, and selected not likely to be associated with blazar(AGN) and pulsar. These lightcurves do not show the significant temporal variability. To confirm their stability, we checked Test Statistic Value of 1FGL and 2-year Fermi observation. Deep Observation with Suzaku (1FGLJ0103: 80ks, 1FGL1946:40ks) is expected to reveal the nature of these unassociated objects, or at least impose strict limits at 2-10keV. Of course, it is necessary that multi-wavelength observation. We'll plan to arrange tie-ups with other wavelength researcher.	EXTRAGALACTIC COMPACT SOURCES	7	B	KOTO MAEDA		JAP	6	AO6	SUZAKU OBSERVATION OF "STEADY" UNASSOCIATED FERMI-LAT GAMMA-RAY SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706026010/	Quick Look
246	RX J1633+4718	248.3342	47.2989	247.973952	47.402455	228.776709	67.659807	73.52584527	42.62417772	308.6809	55760.5047916667	2011-07-18 12:06:54	55761.4376388889	2011-07-19 10:30:12	706027020	37.51	40	37.51	37.51	0	37.51	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57602.5962847222	2016-08-02 14:18:39	56152	2012-08-13 00:00:00	55830.7262268518	2011-09-26 17:25:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060089	RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time.	EXTRAGALACTIC COMPACT SOURCES	7	A	KIYOSHI HAYASHIDA		JAP	6	AO6	X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027020/	Quick Look
247	ZW229-15	286.3333	42.4706	285.936982	42.393229	298.560222	64.301193	73.09172558	15.5517204	34.6696	55715.0128356482	2011-06-03 00:18:29	55719.6251736111	2011-06-07 15:00:15	706035010	167.0838	165	168.6766	167.0838	0	168.6846	2	2	0	2	1	0	0	218.1832	218.1832	398.4357	2	PROCESSED	57602.3250694445	2016-08-02 07:48:06	56127	2012-07-19 00:00:00	55757.7055671296	2011-07-15 16:56:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061414	The optical emission from AGN is though to be a combination of direct radiation from an accretion disk and reprocessed x-ray emission. Separating these components requires simultaneous high-precision x-ray/optical monitoring, which has heretofore not been achieved. We propose to gather this necessary data via simultaneous optical and x-ray monitoring of the Sy 1 galaxy Zw 229-15. Kepler is monitoring Zw 229-15 every 30 minutes with unprecedented 99% duty cycle and 0.1% repeatability. The key missing data is an appropriate x-ray campaign. We propose a 64-orbit (165 ks) Suzaku long-look combined with a series of 48 Swift visits to probe lags of 0.1-10 days. This will be the first experiment sensitive to such short lags and thus will critically test the present disc/reprocessing paradigm	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	6	AO6	SIMULTANEOUS SUZAKU/SWIFT/ KEPLER MONITORING OF ZW 229-15	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706035010/	Quick Look
248	IRAS 09104+4109	138.3378	40.9513	137.53478	41.157946	128.03448	23.67766	180.99146588	43.55010524	90.0004	55883.9878356482	2011-11-18 23:42:29	55885.7675694444	2011-11-20 18:25:18	706038010	81.3276	80	81.3356	81.3276	0	81.3356	2	2	0	2	1	0	0	76.5883	76.5883	153.73	2	PROCESSED	57603.9341203704	2016-08-03 22:25:08	56264	2012-12-03 00:00:00	55895.209849537	2011-11-30 05:02:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062009	We propose to observe IRAS 09104+4109 for 80 ks with Suzaku in order to confirm the ~3 sigma BeppoSAX PDS detection of the source and increase the detection significance with the HXD/PIN to 10 sigma in the 10--80 keV band, allowing the detailed spectral shape to be determined. IRAS 09104+4109 is a hyperluminous Type 2 quasar embedded in a central cluster galaxy at redshift 0.442. It is likely to be the hard-X-ray-brightest such object observed with Suzaku and could well be the prototype Compton-thick Type 2 quasar. The Suzaku observation, especially above 10 keV will most likely reveal one of the most luminous Compton--thick Type 2 QSO to date.	EXTRAGALACTIC COMPACT SOURCES	7	C	CHIA-YING CHIANG		EUR	6	AO6	THE TYPE 2 HYPERLUMINOUS QUASAR IRAS 09104+4109	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706038010/	Quick Look
249	0528+134	82.7323	13.541	82.025359	13.504077	82.83368	-9.719507	191.35839601	-11.00951452	89.1633	55832.6802314815	2011-09-28 16:19:32	55833.0119444444	2011-09-29 00:17:12	706043010	14.7892	10	14.7892	14.7892	0	14.7892	2	2	0	2	1	0	0	15.8659	15.8659	28.6359	0	PROCESSED	57603.2623032407	2016-08-03 06:17:43	56225	2012-10-25 00:00:00	55875.6223958333	2011-11-10 14:56:15	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061601	We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	6	AO6	EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706043010/	Quick Look
250	3C 227	146.9365	7.4245	146.275614	7.656926	146.610705	-5.546093	228.57888407	42.2858038	108.3139	56237.0794675926	2012-11-06 01:54:26	56239.0279513889	2012-11-08 00:40:15	707004010	82.5325	80	82.5405	82.5325	0	82.5405	2	2	0	2	1	0	0	71.4299	71.4299	168.3338	0	PROCESSED	57608.0036342593	2016-08-08 00:05:14	56631	2013-12-05 00:00:00	56264.6488773148	2012-12-03 15:34:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070012	Radio galaxies are a key class to understand the origin and effects of AGN feedback to the surroundings. However, the fundamental question, how the structure of the nucleus is different between AGNs with and without jets, is not resolved yet. A key parameter to understand the accretion flow is the Eddington ratio. BLRGs of 4C 50.55 and 3C 120 are rare objects having high Eddington ratio (L_bol/L_Edd~0.4) compared with Seyferts and typical BLRGs (< 0.1). Though the accretion disks in many BLRGs are known to be truncated and/or inner parts covered by corona, unified picture of accretion flows over a wide range of accretion rate is far from established. Therefore we propose observing a BLRG of 3C 227, which has the highest Eddington ratio in the hard X-ray luminous BLRGs.	EXTRAGALACTIC COMPACT SOURCES	7	C	FUMIE TAZAKI		JAP	7	AO7	STUDY OF NUCLEAR STRUCTURE OF BLRGS WITH HIGH ACCRETION RATE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707004010/	Quick Look
251	2FGL J1502.1+5548	225.5826	55.8575	225.235279	56.052883	185.603435	66.74758	92.73148616	52.90392629	345.2903	56069.912974537	2012-05-22 21:54:41	56070.8342824074	2012-05-23 20:01:22	707008010	62.8733	60	62.8813	62.8813	0	62.8733	2	2	0	2	1	0	0	56.167	56.167	79.5899	1	PROCESSED	57605.4999652778	2016-08-05 11:59:57	56449	2013-06-06 00:00:00	56083.096875	2012-06-05 02:19:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070024	We propose X-ray follow up observations of two high redshift blazar candidates in the Fermi/LAT unidentified sources. The aim of this proposal is to detect X-ray emissions from high redshift blazars (z >> 3) buried in unidentified Fermi/LAT sources and to find the most distant LAT detected blazar. Gamma-ray photons above 10 GeV are attenuated by interactions with UV photons which result in creating electron-positron pairs. Therefore, attenuation signatures are predicted to be observed in gamma-ray spectra and such attenuation of high redshift blazars with redshift up to z ~ 6 provide information about UV background out to the epoch of cosmological reionization. By utilizing the attenuation, we can investigate the UV radiation state of the early universe.	EXTRAGALACTIC COMPACT SOURCES	7	B	YOSUKE TAKAHASHI		JAP	7	AO7	SUZAKU OBSERVATIONS OF HIGH REDSHIFT BLAZAR CANDIDATES IN THE FERMI UNIDENTIFIED SOURCE SAMPLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707008010/	Quick Look
252	2FGL J0157.2-5259	29.3567	-53.0295	28.896901	-53.272777	354.834799	-58.248558	282.0695167	-61.34394411	33.9769	56075.6946064815	2012-05-28 16:40:14	56076.2565162037	2012-05-29 06:09:23	707011010	32.0753	30	32.0753	32.0753	0	32.0753	2	2	0	2	1	0	0	31.7784	31.7784	48.5239	1	PROCESSED	57605.5386458333	2016-08-05 12:55:39	56527	2013-08-23 00:00:00	56161.0508449074	2012-08-22 01:13:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070034	We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN).	EXTRAGALACTIC COMPACT SOURCES	7	B	JUN KATAOKA		JAP	7	AO7	FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707011010/	Quick Look
253	NGC1365	53.4038	-36.1454	52.926467	-36.312356	36.802809	-53.044895	237.96455345	-54.59601318	66.4692	56137.3445138889	2012-07-29 08:16:06	56138.1030208333	2012-07-30 02:28:21	707017040	31.3603	30	31.3683	31.3683	0	31.3603	1	1	0	1	1	0	0	28.2314	28.2314	65.5279	2	PROCESSED	57606.7020717593	2016-08-06 16:50:59	56528	2013-08-24 00:00:00	56162.0367361111	2012-08-23 00:52:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070095	NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. }	EXTRAGALACTIC COMPACT SOURCES	7	B	YASUSHI FUKAZAWA		JAP	7	AO7	MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017040/	Quick Look
254	SWIFT J164449.3+1573	251.1623	57.5874	250.936922	57.677768	216.812116	77.507745	86.72267547	39.46447046	15.8437	56064.7296064815	2012-05-17 17:30:38	56066.0522106482	2012-05-19 01:15:11	707018010	80.8141	80	80.8221	80.8141	0	80.8221	2	2	0	2	1	0	0	74.3379	74.3379	114.2699	0	PROCESSED	57605.4610648148	2016-08-05 11:03:56	56442	2013-05-30 00:00:00	56076.0214351852	2012-05-29 00:30:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070096	We propose a 80 ks observation of a tidal disruption event Swift J164449.3+1573451 one year after its onset. In this event, a star was presumably disrupted by a strong tidal force of a massive black hole at the center of a galaxy at z=0.35, releasing a relativistic jet that emitted intense X-rays. In this proposal, we attempt to detect the non-thermal emission from the relativistic jet and the fluorescent Fe K line from its surrounding material. With these results we study the driving mechanism of the jet and to test the tidal disruption model.	EXTRAGALACTIC COMPACT SOURCES	7	B	RYUICHI USUI		JAP	7	AO7	ONE YEAR AFTER THE TIDAL DISRUPTION OF SWIFT J164449.3+1573451	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707018010/	Quick Look
255	MCG-03-34-64	200.5996	-16.727	199.930176	-16.465808	205.288367	-7.470033	313.53711237	45.50625694	110.133	56296.8837384259	2013-01-04 21:12:35	56301.1737384259	2013-01-09 04:10:11	707027010	155.7127	150	155.7367	155.7127	0	155.7287	2	2	0	2	1	0	0	135.0516	135.0516	370.6038	4	PROCESSED	57608.5292824074	2016-08-08 12:42:10	56018	2012-04-01 00:00:00	56336.6958680556	2013-02-13 16:42:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071423	Analysis of Suzaku observations selected from the BAT 58-month catalog has shown extreme hard X-ray excesses to exist in ~70% of type 1 AGN, and these can be modeled by partial-covering of Compton-thick gas. This new result shows the importance of broad X-ray coverage, currently available only with Suzaku. The most extreme of the sample sources, MCG-03-34-64 and NGC 1194, show significant spectral and flux variability above 10 keV, likely attributable to changes in the Compton-thick absorber. We request new observations of MCG-03-34-64 (150 ks) and NGC 1194 (200 ks) to study the X-ray reprocessor in these extreme systems, confirm the high-energy spectral variability and constrain the nature and location of the Compton-thick absorber.	EXTRAGALACTIC COMPACT SOURCES	7	C	TRACEY TURNER		USA	7	AO7	THE CASE FOR VARIATIONS IN COMPTON-THICK ABSORPTION: MCG-03-34-64 AND NGC 1194	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707027010/	Quick Look
256	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
257	H1821+643	275.4669	64.3595	275.403094	64.333117	318.334051	86.844268	94.01942058	27.4280098	65.0004	56402.5419444444	2013-04-20 13:00:24	56404.6925462963	2013-04-22 16:37:16	708037020	128.2485	400	128.2703	128.2485	0	128.2485	2	2	0	2	1	0	0	132.8215	132.8215	185.8058	2	PROCESSED	57611.1374884259	2016-08-11 03:17:59	56383	2013-04-01 00:00:00	56425.6256712963	2013-05-13 15:00:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081436	H1821+643 (z=0.297) is not "just another quasar". This luminous active galactic nucleus (AGN) is an extremely rare example of a powerful quasar at the center of a rich, cooling-core cluster of galaxies. As such, it may represent a key evolutionary stage in the complex interplay between AGN and the core regions of the intracluster medium (ICM). Our analysis of archival XMM-Newton data has found evidence for a relativistically broad iron line. Here, we build on this request deep (400ks) Suzaku spectroscopy of H1821+643 to (1) measure the spin of this supermassive black hole and (2) search for powerful highly ionized outflows. In addition to measuring spin in the most luminous and distant object yet, this will enable us to test key predictions of recent models for AGN feedback.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	8	AO8	THE BLACK HOLE SPIN AND IONIZED OUTFLOWS IN THE COOLING-FLOW QUASAR H1821+643	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708037020/	Quick Look
258	IRAS F11119+3257	168.6582	32.6829	167.981225	32.955487	156.042952	25.438757	192.21056175	68.35212615	301.5808	56425.1110185185	2013-05-13 02:39:52	56431.3329050926	2013-05-19 07:59:23	708038010	252.2992	250	252.3232	252.2992	0	252.3232	2	2	0	2	1	0	0	220.3036	220.3036	400.8599	10	PROCESSED	57611.4720717593	2016-08-11 11:19:47	56858	2014-07-20 00:00:00	56491.9181828704	2013-07-18 22:02:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081441	Recent Herschel observations provided a breakthrough in identifying powerful, large-scale molecular outflows in ULIRGs, indicating that AGN feedback can indeed have a strong impact on star formation and galaxy evolution, in accordance with theoretical models. However, observational evidence for the connection between the putative fast nuclear AGN winds required for the formation of these large-scale outflows is missing. X-ray observations of blue-shifted Fe K absorption lines directly probe ultra-fast outflows (UFOs) ejected from the AGN accretion disk with v>10,000km/s. A 250ks Suzaku exposure of the ULIRG F11119+3257 with observed extreme molecular/neutral/ionized outflows would allow to characterize the expected UFO, providing the "smoking gun" evidence for feedback driven by AGN winds.	EXTRAGALACTIC COMPACT SOURCES	7	A	FRANCESCO TOMBESI		USA	8	AO8	IRAS F11119+3257: THE "SMOKING GUN" EVIDENCE FOR AGN FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708038010/	Quick Look
259	UGC 03142	70.9469	28.9681	70.161272	28.87543	73.291585	6.626144	172.09277202	-10.99747628	264.8107	56335.692349537	2013-02-12 16:36:59	56336.9946296296	2013-02-13 23:52:16	707032010	51.2847	50	51.2847	51.2927	0	51.3007	2	2	0	2	1	0	0	47.5632	47.5632	112.51	1	PROCESSED	57610.6216898148	2016-08-10 14:55:14	56721	2014-03-05 00:00:00	56349.5963541667	2013-02-26 14:18:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071424	A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN.	EXTRAGALACTIC COMPACT SOURCES	7	C	TRACEY TURNER		USA	7	AO7	INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707032010/	Quick Look
260	FAIRALL 51	281.2285	-62.3615	280.064534	-62.412939	276.680669	-39.180999	333.20299178	-23.09155943	253.9697	56548.4894444445	2013-09-13 11:44:48	56549.3146990741	2013-09-14 07:33:10	708046040	30.1926	30	30.2006	30.1926	0	30.1926	2	2	0	2	1	0	0	37.1812	37.1812	71.2679	1	PROCESSED	57612.6129050926	2016-08-12 14:42:35	56990	2014-11-29 00:00:00	56625.6172337963	2013-11-29 14:48:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082016	Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures.	EXTRAGALACTIC COMPACT SOURCES	7	A	JIRI SVOBODA		EUR	8	AO8	STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708046040/	Quick Look
261	MCG -5-23-16	146.9445	-30.9023	146.395049	-30.669659	162.619875	-41.096298	262.72964912	17.28396386	118.3849	53711.9526388889	2005-12-07 22:51:48	53714.4939699074	2005-12-10 11:51:19	700002010	95.6774	100	95.6774	95.7174	95.7174	95.6854	2	2	2	2	1	0	0	85.5647	85.5647	219.5251	3	PROCESSED	57532.4508680556	2016-05-24 10:49:15	54247	2007-05-27 00:00:00	54039.1988310185	2006-10-31 04:46:19	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001006	We request a 100ks Suzaku observation of the bright Seyfert galaxy, MCG -5-23-16 simultaneously with approved XMM-Newton and Chandra HETG observations in December 2005. MCG -5-23-16 has one of the best known examples of a relativistically broadened iron K line. With a Swift-BAT flux of 1.6e-10 cgs (15-100 keV), it is one of the brightest AGN above 10 keV. The simultaneous observations will allow us to determine the shape of the broad relativistic Fe line after subtracting the narrow line components measured by HETG. Importantly, Suzaku's wide bandpass will accurately measure the broad-band continuum and reflection component of MCG -5-23-16, essential for constraining the broad iron line. These observations will also allow us to determine the temperature of the high energy cut-off.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		JAP	0	SWG	PROBING THE BROAD IRON LINE AND HIGH ENERGY CONTINUUM OF MCG -5-23-16 SIMULTANEOUSLY WITH SUZAKU, XMM-NEWTON AND CHANDRA	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700002010/	Quick Look
262	IRAS 12127-1412	183.8305	-14.4966	183.185484	-14.2187	189.338442	-11.765951	289.94461652	47.46236248	294.8513	56113.7580671296	2012-07-05 18:11:37	56115.2862615741	2012-07-07 06:52:13	707037010	63.6095	60	63.6095	63.6095	0	63.6095	2	2	0	2	1	0	0	57.584	57.584	132.012	2	PROCESSED	57606.6111342593	2016-08-06 14:40:02	56508	2013-08-04 00:00:00	56142.1406018518	2012-08-03 03:22:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071441	We propose to observe with the Hard X-ray Detector onboard Suzaku the two Ultraluminous Infrared Galaxies IRAS 00182-7112 and IRAS 12127-1412, both of which are known to harbour very luminous and highly obscured active galactic nuclei (AGN). An AGN reflection component arising from ionized gas is clearly identified at 2 10 keV: the detection of the direct AGN emission above 10 keV and the measure of the reflection efficiency would provide fundamental information on both the physical structure of Compton-thick AGN embedded in a nuclear starburst and their feedback on the surrounding environment.	EXTRAGALACTIC COMPACT SOURCES	7	B	EMANUELE NARDINI		USA	7	AO7	THE PHYSICAL STRUCTURE OF COMPTON-THICK AGN/ULIRGS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707037010/	Quick Look
263	PG 1211+143	183.6045	14.1097	182.967898	14.387617	177.569786	14.352789	267.53559231	74.37841457	120.7913	53698.7348263889	2005-11-24 17:38:09	53701.3397453704	2005-11-27 08:09:14	700009010	96.3241	100	96.59	97.5802	96.3241	96.3241	3	2	3	3	1	0	0	84.0087	84.0087	225.0438	2	PROCESSED	57528.1616203704	2016-05-20 03:52:44	54247	2007-05-27 00:00:00	54038.7422106482	2006-10-30 17:48:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001041	A 100ks Suzaku observation of the NLS1, PG 1211+143 is proposed. Previous XMM-Newton and Chandra observation claimed both blue-shifted (0.1c) and redshifted (0.26c-0.40c) iron Kalpha absorption lines. The redshifted iron K lines may originate from matter falling onto the supermassive black hole. The high effective area and low background of Suzaku XIS above 5 keV will enable us to measure these relativistically shifted iron lines in PG 1211+143 with great accuracy. Constraining the time variability of the lines will allow us to determine the physical origins of the absorption, e.g. failed jet/outflow or gravitational redshift from a Kerr black hole. The excellent broadband capabilities of Suzaku will accurately determine the continuum, essential for modeling the iron K band.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		JAP	0	SWG	EXPLORING THE RELATIVISTICALLY SHIFTED IRON LINES IN PG 1211+143	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700009010/	Quick Look
264	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
265	3C345	250.7487	39.7945	250.326948	39.887223	238.332578	61.133151	63.43440525	40.94504508	267.732	56181.2697453704	2012-09-11 06:28:26	56181.4772337963	2012-09-11 11:27:13	707043010	12.7008	10	12.7088	12.7168	0	12.7008	1	1	0	1	1	0	0	10.7314	10.7314	17.9199	0	PROCESSED	57606.986412037	2016-08-06 23:40:26	56582	2013-10-17 00:00:00	56212.7656712963	2012-10-12 18:22:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071601	We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	7	AO7	MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707043010/	Quick Look
266	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
267	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
268	NGC 5273	205.535	35.6446	204.979886	35.89633	186.960858	42.373618	74.3162813	76.25118024	278.9999	56489.1929976852	2013-07-16 04:37:55	56491.0543171296	2013-07-18 01:18:13	708001010	81.7709	80	81.7709	81.7949	0	81.7789	2	2	0	2	1	0	0	79.0981	79.0981	160.8018	3	PROCESSED	57612.0002546296	2016-08-12 00:00:22	56890	2014-08-21 00:00:00	56523.6749537037	2013-08-19 16:11:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080015	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	8	AO8	BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708001010/	Quick Look
269	NGC 3516	166.6694	72.5588	165.816381	72.829135	123.37012	57.971175	133.25250212	42.40656753	323.9054	56754.7044675926	2014-04-07 16:54:26	56755.5002777778	2014-04-08 12:00:24	708006080	51.539	50	51.539	51.547	0	51.555	2	2	0	2	1	0	0	46.0472	46.0472	68.752	1	PROCESSED	57614.1922800926	2016-08-14 04:36:53	56383	2013-04-01 00:00:00	56817.774849537	2014-06-09 18:35:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080066	We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	8	AO8	THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006080/	Quick Look
270	HOLMBERG II X-1	124.8874	70.7162	123.586257	70.872801	106.845907	49.308193	144.27230635	32.72696637	127.9069	56552.1954398148	2013-09-17 04:41:26	56553.2994212963	2013-09-18 07:11:10	708015010	52.19	50	52.19	52.19	0	52.19	2	2	0	2	1	0	0	48.9852	48.9852	95.376	0	PROCESSED	57612.6731481482	2016-08-12 16:09:20	56954	2014-10-24 00:00:00	56588.6670717593	2013-10-23 16:00:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081251	Recent X-ray observations have produced evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in an unusual super-Eddington state. Current data are unable to deliver a clear answer, as attempts to model the 0.5-10keV spectra have been plagued by degeneracies resulting from the limited bandpass, owing to the previous lack of focusing hard X-ray telescopes. Combined, Suzaku and NuSTAR will obtain high-quality spectra covering 0.5-30keV, providing powerful probes for understanding the accretion modes and nature of the central BHs. A definitive statement on the existence of either 100-1000Msun black holes or extreme accretion states will be an important legacy of both missions.	EXTRAGALACTIC COMPACT SOURCES	7	A	DOMINIC WALTON		USA	8	AO8	COORDINATED SUZAKU AND NUSTAR OBSERVATIONS OF HOLMBERG II X-1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708015010/	Quick Look
271	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
272	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
273	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
274	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
275	MKN 335	1.5763	20.2091	0.933386	19.930785	9.740827	17.860354	108.75916207	-41.41726175	71.5255	56457.9792939815	2013-06-14 23:30:11	56461.868287037	2013-06-18 20:50:20	708016020	154.8168	300	154.8648	154.8168	0	154.8568	2	2	0	2	1	0	0	141.5908	141.5908	335.8944	3	PROCESSED	57611.6590162037	2016-08-11 15:48:59	56383	2013-04-01 00:00:00	56512.7189467593	2013-08-08 17:15:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081411	The idea of this proposal is trigger a 300ks observation with Suzaku of the Narrow Line Seyfert 1 Galaxy Mkn 335 during one of its low X-ray flux states. The goal here is to measure its underlying broad-band continuum with Suzaku during a low state and compare it with the 2006 high-state observations. Mkn 335 is one of the best examples of an AGN that went into a deep minimum X-ray flux state. Two competing models can explain these extreme low states: reflection models and partial covering absorber models. Both models still require a variable underlying intrinsic continuum. The science driver is to find out what is causing these low X-ray flux states that have been observed in several NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	A	DIRK GRUPE		USA	8	AO8-TOO	INTRINSIC LOW-STATE X-RAY LUMINOSITY OF THE NLS1 MKN 335	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708016020/	Quick Look
276	NGC5929	231.5229	41.6989	231.07632	41.872918	210.309469	57.436696	67.89643134	55.30533508	120.4869	56651.8033217593	2013-12-25 19:16:47	56652.6042824074	2013-12-26 14:30:10	708022010	24.649	30	24.649	24.6689	0	24.6565	2	2	0	2	1	0	0	25.1767	25.1767	69.1919	0	PROCESSED	57613.6825925926	2016-08-13 16:22:56	56383	2013-04-01 00:00:00	56700.6301388889	2014-02-12 15:07:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081418	Using Suzaku's sensitivity in the 2-50keV range, we propose to obtain broad-band spectral fits to the X-ray emission from five Seyfert galaxies which have nuclei that are likely to be Compton-thick. We will thereby derive estimates of their absorbing column densities (hitherto unknown), Fe line widths and equivalent widths, absorption-corrected nuclear X-ray emission and the reprocessed components. With these new estimates we will have complete measurements for a rigorously selected sample of 20 Seyferts that are matched in orientation-independent parameters. The sample selection enables us to account for orientation effects which dominate in them, and investigate the AGN evolution, AGN-star burst connection, and host galaxy evolution.	EXTRAGALACTIC COMPACT SOURCES	7	C	PRAJVAL SHASTRI		USA	8	AO8	COMPTON-THICK SEYFERT NUCLEI AND SEYFERT UNIFICATION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708022010/	Quick Look
277	MRK533	351.9889	8.7759	351.354325	8.500435	356.155514	11.232339	90.62800693	-48.78900326	248.1747	56634.8830671296	2013-12-08 21:11:37	56636.0847569444	2013-12-10 02:02:03	708023010	52.194	50	52.194	52.194	0	52.194	2	2	0	2	1	0	0	48.5617	48.5617	103.8059	0	PROCESSED	57613.5724421296	2016-08-13 13:44:19	56383	2013-04-01 00:00:00	56646.7358449074	2013-12-20 17:39:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081418	Using Suzaku's sensitivity in the 2-50keV range, we propose to obtain broad-band spectral fits to the X-ray emission from five Seyfert galaxies which have nuclei that are likely to be Compton-thick. We will thereby derive estimates of their absorbing column densities (hitherto unknown), Fe line widths and equivalent widths, absorption-corrected nuclear X-ray emission and the reprocessed components. With these new estimates we will have complete measurements for a rigorously selected sample of 20 Seyferts that are matched in orientation-independent parameters. The sample selection enables us to account for orientation effects which dominate in them, and investigate the AGN evolution, AGN-star burst connection, and host galaxy evolution.	EXTRAGALACTIC COMPACT SOURCES	7	C	PRAJVAL SHASTRI		USA	8	AO8	COMPTON-THICK SEYFERT NUCLEI AND SEYFERT UNIFICATION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708023010/	Quick Look
278	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
279	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
280	ABELL 1005	156.925	68.2013	156.004708	68.456472	124.194907	52.556114	140.47803773	43.70739533	119.4313	56609.4953819444	2013-11-13 11:53:21	56610.8334490741	2013-11-14 20:00:10	708042010	61.3496	60	61.3496	61.3496	0	61.3496	2	2	0	2	1	0	0	58.9645	58.9645	115.5998	2	PROCESSED	57613.3284722222	2016-08-13 07:53:00	56994	2014-12-03 00:00:00	56625.7198611111	2013-11-29 17:16:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081533	We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters.	EXTRAGALACTIC COMPACT SOURCES	7	C	LAURENCE DAVID		USA	8	AO8	MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708042010/	Quick Look
281	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
282	NGC 2788A	135.6754	-68.2181	135.519975	-68.019146	206.346244	-72.761691	284.17134554	-14.14937336	282.2863	57157.0478819444	2015-05-15 01:08:57	57158.2230324074	2015-05-16 05:21:10	710007010	42.2339	40	42.2339	42.2339	0	42.2339	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.6656828704	2016-08-18 15:58:35	57591	2016-07-22 00:00:00	57224.447650463	2015-07-21 10:44:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	100009	Swift/BAT extragalactic survey above E >15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe four Compton thick AGN candidates in the 70 month BAT catalog with Suzaku. Since their spectra below 10 keV are likely reflection dominated, joint analysis of Suzaku/XIS and Swift/BAT can constrain the absorption and intrinsic luminosity without being much affected by time variability. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep survey.	EXTRAGALACTIC COMPACT SOURCES	7	B	YOSHIHIRO UEDA		JAP	10	AO10	DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710007010/	Quick Look
283	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
284	NGC 4395	186.4111	33.4884	185.79012	33.76517	170.810459	32.904029	162.54122992	81.55189464	303.1476	54253.6042013889	2007-06-02 14:30:03	54256.2981944444	2007-06-05 07:09:24	702001010	101.5075	100	101.5155	101.5075	0	101.5155	2	2	0	2	1	0	0	101.9292	101.9292	232.7198	4	PROCESSED	57538.8900694444	2016-05-30 21:21:42	54745	2008-10-06 00:00:00	54263.5438194445	2007-06-12 13:03:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020001	We propose a 100 ks observation of the intermediate mass black hole (IMBH) active nucleus in the dwarf Seyfert galaxy NGC 4395. Utilising the high-energy sensitivity of Suzaku will enable us to determine the shape of the intrinsic continuum, which is significantly absorbed below 10 keV. Constraining the shape of the continuum will allow us to investigate the more general problem of the relationship between AGN flux and apparent spectral slope. In addition, with a firm grasp of the intrinsic continuum properties, we can accurately determine the physical conditions of the warm absorber in NGC 4395.	EXTRAGALACTIC COMPACT SOURCES	7	A	YASUO TANAKA		JAP	2	AO2	UNCOVERING THE IMBH ACTIVE NUCLEUS IN THE DWARF SEYFERT GALAXY NGC 4395	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702001010/	Quick Look
285	M33 X8	23.4834	30.5892	22.778431	30.333215	33.223542	19.296261	133.64723816	-31.39681198	258.5185	55207.0743865741	2010-01-11 01:47:07	55209.5626157407	2010-01-13 13:30:10	704016010	106.1036	100	106.1036	106.1061	0	106.1061	2	2	0	2	1	0	0	6.1053	6.1053	214.9577	1	PROCESSED	57550.3046412037	2016-06-11 07:18:41	55587	2011-01-26 00:00:00	55218.6414930556	2010-01-22 15:23:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040067	The nature of ultraluminous X-ray sources (ULXs) is one of the important unresolved issues in the modern astrophysics. In order to solve the problem, it is of crucial importance to observe X-ray spectra above 10 keV from ULXs, which enables us to determine precisely their spectral states. Therefore, Suzaku observations of two bright ULX, M33 X8 and IC 342 X2, are proposed.	EXTRAGALACTIC COMPACT SOURCES	7	C	NAOKI ISOBE		JAP	4	AO4	HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704016010/	Quick Look
286	ARK 564	340.6583	29.7351	340.07073	29.472916	355.35057	34.71587	92.13955378	-25.32593551	75.7895	57167.0898842593	2015-05-25 02:09:26	57168.4029282407	2015-05-26 09:40:13	710018010	52.5104	50	52.5104	53.9344	0	53.9344	2	2	0	2	1	0	0	27.9802	27.9802	100.9477	2	PROCESSED	57618.7636921296	2016-08-18 18:19:43	57548	2016-06-09 00:00:00	57178.248587963	2015-06-05 05:57:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	102721	A NuSTAR legacy is emerging through long observations of bare Seyfert galaxies that reveal an unprecedented look at relativistic reflection off an ionized accretion disc. We propose now to look at the Seyfert galaxy Ark 564 for 200 ks with NuSTAR and 50 ks with Suzaku in order to understand the reflection in this bright source. Ark 564 has been well-studied in the soft band, revealing a steep spectrum, strong soft excess, broad iron K emission line and dramatic variability on the order of hours. It is very akin to two other well-known bare Seyferts, 1H0707-405 and IRAS 13224-3809, except it is an order of magnitude brighter. With this 200 ks observation, we will probe the geometry of the corona, through a complete spectral and timing analysis.	EXTRAGALACTIC COMPACT SOURCES	7	B	ERIN KARA		EUR	10	AO10	UNDERSTANDING REFLECTION IN THE BARE SEYFERT I ARK 564	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710018010/	Quick Look
287	B2 1023+25	156.5986	25.7113	155.903697	25.966089	148.79406	14.812793	207.05661505	57.60744793	288.3095	56442.6428125	2013-05-30 15:25:39	56444.9133449074	2013-06-01 21:55:13	708044010	100.8874	100	100.8954	100.8874	0	100.8954	2	2	0	2	1	0	0	96.5787	96.5787	196.1298	2	PROCESSED	57611.461099537	2016-08-11 11:03:59	56821	2014-06-13 00:00:00	56455.8205324074	2013-06-12 19:41:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082005	We propose a deep (100 ksec) Suzaku observation of the recently discovered high redshift blazar candidate B2 1023+25 (z=5.3). A very hard (Gamma <2) spectrum would confirm its blazar nature, allowing to study the physical properties of the relativistic jet in this extremely powerful and very high redshift source. The proposed observation will yield an X-ray spectrum of sufficient quality to determine the X-ray shape. The confirmation of a second blazar at this redshift has profound cosmological implications, placing stronger constraints on the number density of high mass BH at high z	EXTRAGALACTIC COMPACT SOURCES	7	A	VALENTINA BRAITO		EUR	8	AO8	THE HIGH-REDSHIFT BLAZAR CANDIDATE B2 1023+25	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708044010/	Quick Look
288	OJ 287 QUIESCENT	133.689	20.0482	132.974133	20.239223	130.506959	2.538802	206.87650629	35.78772906	283.9125	54200.8243055556	2007-04-10 19:47:00	54203.4654976852	2007-04-13 11:10:19	702009010	102.8441	100	102.8441	102.8441	0	102.8441	2	2	0	2	1	0	0	93.6244	93.6244	228.1859	12	PROCESSED	57538.2031018518	2016-05-30 04:52:28	54744	2008-10-05 00:00:00	54210.7303587963	2007-04-20 17:31:43	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020024	OJ 287 is a promissing candidate of a suppermassive binary black hole, based on its periodic flare with a cycle of about 12 years. The next flare is predicted to take place on the fall, 2007. Therefore, two Suzaku exposures on OJ 287 is proposed, coordinated with radio, optical and very high energy gamma-ray observations. The first observation is on the spring to obtained the multi-wavelength spectrum of the target in its quiescent phase. The second is planned to be in a form of ToO observation on the fall, which will be triggered by an optical flare. The nature of the flare will be extensively investigated in these observatsions.	EXTRAGALACTIC COMPACT SOURCES	7	A	NAOKI ISOBE		JAP	2	AO2-TOO	MULTI-WAVELENGTH OBSERVATION OF PREDICTED FLARE OF SUPERMASSIVE BINARY BLACK HOLE CANDIDATE, OJ 287	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702009010/	Quick Look
289	SWIFT J0714.2+3518	108.5168	35.2792	107.688726	35.365694	105.421903	12.82422	182.49455345	19.57130625	283.6115	57116.9939814815	2015-04-04 23:51:20	57118.9043634259	2015-04-06 21:42:17	709007010	79.2471	80	79.2471	79.2471	0	79.2471	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.9309027778	2016-08-17 22:20:30	57565	2016-06-26 00:00:00	57198.4724074074	2015-06-25 11:20:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090019	Swift/BAT extragalactic survey above E >15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe two Compton thick AGN candidates in the 70 month BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	9	AO9	DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709007010/	Quick Look
290	KUV 00311-1938	8.3907	-19.361	7.763877	-19.636683	359.653009	-21.03622	94.15504043	-81.21658968	60.8243	56821.2581481482	2014-06-13 06:11:44	56822.2384606482	2014-06-14 05:43:23	709013010	41.8926	40	41.8926	41.9006	0	41.9006	2	2	0	2	1	0	0	35.9853	35.9853	84.6858	0	PROCESSED	57615.2401851852	2016-08-15 05:45:52	57200	2015-06-27 00:00:00	56833.588900463	2014-06-25 14:08:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090088	Extreme HBL objects are BL Lac objects characterized by their hard TeV gamma-ray spectra, by which the sources are considered as excellent targets to study secondary cascade gamma-ray emission induced by very-high-energy photons or protons from the sources. We propose Suzaku observations of 1ES 0347-121 and KUV 00311-1938 for 60 ks and 40 ks, respectively. The observations can reveal detailed spectral structure around synchrotron peak in the extreme HBLs, which are essential to derive physical parameters such as electron spectrum, magnetic filed strength in the jet. The results will help understating gamma-ray components of both intrinsic jet emission and the secondary cascade emission.	EXTRAGALACTIC COMPACT SOURCES	7	C	MASAAKI HAYASHIDA		JAP	9	AO9	SUZAKU OBSERVATIONS OF EXTREME HIGH-FREQUENCY PEAKED BL LAC OBJECTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709013010/	Quick Look
291	NGC 4593	189.9133	-5.3412	189.268409	-5.066685	191.201213	-0.986393	297.4806457	57.40576161	111.8999	57017.6624421296	2014-12-26 15:53:55	57021.7640740741	2014-12-30 18:20:16	709014040	130.3584	30	130.3904	130.3584	0	130.3824	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.5950810185	2016-08-17 14:16:55	57415	2016-01-28 00:00:00	57049.4551851852	2015-01-27 10:55:28	3.0.22.44	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090097	In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	9	AO9	X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014040/	Quick Look
292	LMC X-4	83.221	-66.3591	83.212611	-66.392014	1.088478	-87.292124	276.32094979	-32.52452295	284.2438	54561.5523842593	2008-04-05 13:15:26	54562.3058333333	2008-04-06 07:20:24	702036020	25.3397	20	25.3425	25.3425	0	25.3397	2	2	0	2	1	0	0	24.502	24.502	65.07	0	PROCESSED	57542.2490046296	2016-06-03 05:58:34	54943	2009-04-22 00:00:00	54574.4237152778	2008-04-18 10:10:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021127	We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects.	EXTRAGALACTIC COMPACT SOURCES	7	A	RYAN HICKOX		USA	2	AO2	SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702036020/	Quick Look
293	NGC5548	214.4955	25.1272	213.928592	25.357387	201.997114	36.406484	31.93108614	70.4962838	289.7815	54303.4447337963	2007-07-22 10:40:25	54304.2711111111	2007-07-23 06:30:24	702042060	28.9178	30	28.9258	28.9258	0	28.9178	1	1	0	1	1	0	0	24.8181	24.8181	71.3839	1	PROCESSED	57539.29125	2016-05-31 06:59:24	54706	2008-08-28 00:00:00	54339.5363310185	2007-08-27 12:52:19	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021307	We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	2	AO2	NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042060/	Quick Look
294	NGC 4507	188.8987	-39.9119	188.223538	-39.636542	205.656728	-32.779926	299.63576127	22.85843053	109.5879	54454.5145717593	2007-12-20 12:20:59	54456.5835532407	2007-12-22 14:00:19	702048010	103.626	80	103.634	103.626	0	103.634	2	2	0	2	1	0	0	110.9021	110.9021	178.7279	0	PROCESSED	57540.963900463	2016-06-01 23:08:01	54829	2008-12-29 00:00:00	54462.288287037	2007-12-28 06:55:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021331	Recent X-ray observations of Seyfert 2 galaxies have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by AGN Unified Schemes. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (60 ksec each) of four local bright Compton-thin Seyfert2s, selected from the Swift/BAT survey with a hard X-ray flux exceeding 1e-10 cgs to form a flux-limited sample. The unprecedented broad bandpass of Suzaku offers a unique tool to investigate the X-ray emission, placing strong constraints on the geometry and location of the reprocessing matter.	EXTRAGALACTIC COMPACT SOURCES	7	B	JAMES REEVES		USA	2	AO2	REVEALING THE REPROCESSING MATTER IN SEYFERT 2 GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702048010/	Quick Look
295	HOLMBERG IX X-1	149.4756	69.0751	148.45738	69.31359	119.76782	51.701026	141.91985765	41.06519535	104.8942	56976.7425347222	2014-11-15 17:49:15	56977.5230787037	2014-11-16 12:33:14	709015020	34.1281	30	34.1281	34.1281	0	34.1281	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7878240741	2016-08-16 18:54:28	57359	2015-12-03 00:00:00	56993.4304513889	2014-12-02 10:19:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091251	Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs.	EXTRAGALACTIC COMPACT SOURCES	7	A	DOMINIC WALTON		USA	9	AO9	MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015020/	Quick Look
296	I ZW 18	143.5064	55.23	142.623877	55.452479	125.705805	38.222173	160.54065348	44.84408453	279.2158	56792.4911111111	2014-05-15 11:47:12	56792.8568402778	2014-05-15 20:33:51	709021010	17.2612	100	17.2612	17.2612	0	17.2612	1	1	0	1	1	0	0	16.549	16.549	31.1279	0	PROCESSED	57615.102650463	2016-08-15 02:27:49	57358	2015-12-02 00:00:00	56818.6775347222	2014-06-10 16:15:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091441	The source of energetic photons that reionized and heated the early universe remains uncertain. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectrum with the Suzaku XIS. These observations are important to our understanding of the heating of the universe during the epoch of reionization.	EXTRAGALACTIC COMPACT SOURCES	7	A	PHILIP KAARET		USA	9	AO9	X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709021010/	Quick Look
297	MARKARIAN 3	93.8907	71.0457	92.440546	71.061085	91.87875	47.630769	143.28642165	22.71781378	80.3638	56937.8059953704	2014-10-07 19:20:38	56938.0751967593	2014-10-08 01:48:17	709022020	17.7277	20	17.7357	17.7357	0	17.7277	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.6163078704	2016-08-16 14:47:29	57358	2015-12-02 00:00:00	56992.4094560185	2014-12-01 09:49:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092008	We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each.	EXTRAGALACTIC COMPACT SOURCES	7	A	MATTEO GUAINAZZI		EUR	9	AO9	MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022020/	Quick Look
298	QSO 1222+216	186.2289	21.3877	185.599556	21.664582	176.758894	22.007996	255.04256268	81.66684682	123.6039	56989.2953356482	2014-11-28 07:05:17	56989.4064583333	2014-11-28 09:45:18	709025020	0.5272	15	0.5352	0.5272	0	0.8088	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.4022222222	2016-08-17 09:39:12	57368	2015-12-12 00:00:00	57002.4417361111	2014-12-11 10:36:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092023		EXTRAGALACTIC COMPACT SOURCES	7	C	MARCUS LANGEJAHN		EUR	9	AO9	false	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709025020/	Quick Look
299	XBONGBLUE1	217.1061	32.8569	216.573655	33.079659	200.393656	44.372245	54.10325006	68.28811801	132.8525	54453.8528587963	2007-12-19 20:28:07	54454.166875	2007-12-20 04:00:18	702082010	15.1725	13	15.1725	15.1725	0	15.1725	2	2	0	2	1	0	0	15.6996	15.6996	27.1259	0	PROCESSED	57540.9008217593	2016-06-01 21:37:11	54828	2008-12-28 00:00:00	54461.0450231482	2007-12-27 01:04:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021376	We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs.	EXTRAGALACTIC COMPACT SOURCES	7	C	CHRISTINE JONES		USA	2	AO2	OBSCURED AGN AND XBONGS IN BOOTES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702082010/	Quick Look
300	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
301	IGR J12391-1612	189.807	-16.1292	189.153193	-15.854578	195.389743	-10.939243	298.65896251	46.64122293	122.9437	54818.9051273148	2008-12-18 21:43:23	54822.2910648148	2008-12-22 06:59:08	703007010	130.274	120	130.274	130.274	0	130.274	2	2	0	2	1	0	0	111.0893	111.0893	292.4838	2	PROCESSED	57545.0634953704	2016-06-06 01:31:26	55206	2010-01-10 00:00:00	54840.5288425926	2009-01-09 12:41:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030012	We propose a Suzaku observation of a Compton thick candidate, IGR J12391-1612. This source is a bright Seyfert 2 galaxy in the INTEGRAL AGN catalog by Beckman et al. 2006. By a follow-up observation in the optical band, this source was classified as an X-ray luminous type 2 Seyfert galaxy. A Chandra follow-up observation was also performed, but the shape of the X-ray spectrum was not well determined due to a short exposure of 3.5ks. Thank to the wide-band spectroscopy of Suzaku, we can obtain an X-ray spectrum in the 0.5-100 keV band. We will reveal the nature of this Compton thick Seyfert in a spectral analysis.	EXTRAGALACTIC COMPACT SOURCES	7	A	HISAMITSU AWAKI		JAP	3	AO3	X-RAY OBSERVATION OF A COMPTON THICK CANDIDATE, IGR J12391-1612	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703007010/	Quick Look
302	NGC 1313	49.5565	-66.5364	49.405687	-66.717354	341.391654	-74.190914	283.40259478	-44.62074971	201.281	54805.9606828704	2008-12-05 23:03:23	54808.2814699074	2008-12-08 06:45:19	703010010	91.4661	100	91.4981	91.4661	0	91.4981	2	2	0	2	1	0	0	78.7593	78.7593	200.4937	1	PROCESSED	57544.7004861111	2016-06-05 16:48:42	55188	2009-12-23 00:00:00	54822.6519328704	2008-12-22 15:38:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030038	The nature of ultra luminous X-ray sources (ULX) is one of the most important unresolved issue in the modern astrophysics. We propose a 100 ks observation of an famous ULX, NGC 1313 X1, in order to search for Fe-K absorption lines, which are important spectral feature of Galactic black holes. Through the absorption feature, we will examine the nature of the ULX.	EXTRAGALACTIC COMPACT SOURCES	7	C	KEN OHSUGA		JAP	3	AO3	EXPLORING FE K-LINE ABSORPTION FEATURES FROM AN ULTRALUMINOUS X-RAY SOURCE, NGC 1313 X1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703010010/	Quick Look
303	NGC 454	18.511	-55.3853	17.99732	-55.649778	343.260726	-55.777074	296.21074431	-61.44696878	18.3891	54950.2291782407	2009-04-29 05:30:01	54953.4023032407	2009-05-02 09:39:19	704009010	128.9562	120	128.9562	128.9562	0	128.9562	2	2	0	2	1	0	0	114.5969	114.5969	274.1296	0	PROCESSED	57546.5592361111	2016-06-07 13:25:18	55342	2010-05-26 00:00:00	54973.5148842593	2009-05-22 12:21:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040050	Seyfert galaxies with a low-mass central black hole are a key class of objects to study the growth phase of supermassive black holes. We propose to observe the hard X-ray brightest and low-mass (1.6e6 Msolar) Seyfert 2 galaxy NGC 454 selected from the Swift BAT survey. The data will be used (1) to measure broad-band X-ray spectrum and its variability, (2) to compare them with properties of known Seyferts, and (3) to search for variation of absorption to constrain the structure and origin of obscuring matter.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	4	AO4	X-RAY SPECTRAL VARIABILITY OF THE HARD X-RAY BRIGHTEST LOW-MASS SEYFERT 2 NGC 454	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704009010/	Quick Look
304	MRK 18	135.5092	60.0703	134.525486	60.267174	118.140543	40.9961	155.86471567	39.40052697	266.8203	55330.5025810185	2010-05-14 12:03:43	55331.3772106482	2010-05-15 09:03:11	705001010	37.9667	40	37.9747	37.9747	0	37.9667	2	2	0	2	1	0	0	34.667	34.667	75.5539	1	PROCESSED	57551.5224074074	2016-06-12 12:32:16	55769	2011-07-27 00:00:00	55403.0749768518	2010-07-26 01:47:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050003	We propose to observe two Swift/BAT selected obscured AGNs with significant scattered emission, Mrk 18 and Ark 347. Hard X-ray selected AGNs show some peculiar characteristics compared to optically selected ones such as weak scattering emission from the opening part of the putative torus and weak plasma emission in the soft X-ray band. The targets are Swift/BAT selected AND show significant scattered emission, which are poorly explored with Suzaku so far. Our aims are to constrain the geometrical structure of the obscuring matter based on broad-band X-ray spectra and compare them with other hard X-ray or optically selected obscured AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	5	AO5	THE STRUCTURE OF COMPTON-THIN AGNS WITH SIGNIFICANT SCATTERED EMISSION SELECTED BY SWIFT/BAT	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705001010/	Quick Look
305	NGC3227	155.8772	19.8684	155.194638	20.121777	150.38806	9.142968	216.98573476	55.44624837	110.6974	54797.8953703704	2008-11-27 21:29:20	54799.750162037	2008-11-29 18:00:14	703022050	79.4298	50	79.4298	79.4339	0	79.4378	2	2	0	2	1	0	0	39.8439	39.8439	160.2418	1	PROCESSED	57544.6203819444	2016-06-05 14:53:21	54557	2008-04-01 00:00:00	54809.8059490741	2008-12-09 19:20:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031013	We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	3	AO3	NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022050/	Quick Look
306	CENTAURUS_A	201.3411	-43.072	200.607667	-42.811983	217.145584	-31.383496	309.48969514	19.36734145	290.0008	55032.3718634259	2009-07-20 08:55:29	55033.7683333333	2009-07-21 18:26:24	704018010	62.4328	50	62.4328	62.6888	0	62.7076	3	2	0	2	1	0	0	55.45	55.45	120.6499	3	PROCESSED	57547.9397569444	2016-06-08 22:33:15	55415	2010-08-07 00:00:00	55048.3403356482	2009-08-05 08:10:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040085	We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku.	EXTRAGALACTIC COMPACT SOURCES	7	A	YASUSHI FUKAZAWA		JAP	4	AO4	SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704018010/	Quick Look
307	MKN 279	208.2253	69.3021	207.933654	69.547649	144.919228	67.626916	115.05735618	46.87522986	345.4595	54965.2632407407	2009-05-14 06:19:04	54968.6668287037	2009-05-17 16:00:14	704031010	160.3514	150	160.3594	160.3514	0	160.3594	2	2	0	2	1	0	0	150.386	150.386	293.9979	3	PROCESSED	57546.636099537	2016-06-07 15:15:59	55345	2010-05-29 00:00:00	54978.3987152778	2009-05-27 09:34:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041403	We aim to test if the high-luminosity Seyfert 1.5 Mkn 279 contains an ionized inner accretion disk by using Suzaku to spectroscopically separate the ionized and neutral reflectors. This source is relatively unobscured, allowing clear modeling of the shape of the strong soft excess; we will also test for a Fe K diskline component, which may be missing if the disk is ionized or truncated. Only a broadband X-ray spectrum, including simultaneous > 10 keV coverage to constrain Compton reflection, will allow us to thoroughly test blurred, ionized disk reflection models and constrain the nature of the reflector(s).	EXTRAGALACTIC COMPACT SOURCES	7	A	ALEX MARKOWITZ		USA	4	AO4	DOES THE LOW-OBSCURATION, LOW-REFLECTION, HIGH-LUMINOSITY SEYFERT MKN279 CONTAIN AN IONIZED OR TRUNCATED ACCRETION DISK?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704031010/	Quick Look
308	NGC1194	45.9522	-1.1044	45.31576	-1.299082	43.150403	-17.672733	179.17914291	-48.96176874	76.9913	55044.6911689815	2009-08-01 16:35:17	55045.8141087963	2009-08-02 19:32:19	704046010	50.3161	50	50.3161	50.5961	0	50.5961	2	2	0	2	1	0	0	48.4268	48.4268	97.0038	1	PROCESSED	57548.0499074074	2016-06-09 01:11:52	55427	2010-08-19 00:00:00	55061.5275115741	2009-08-18 12:39:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041414	We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc.	EXTRAGALACTIC COMPACT SOURCES	7	B	EZEQUIEL TREISTER		USA	4	AO4	THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704046010/	Quick Look
309	IC 2497	145.222	34.6799	144.47003	34.907483	135.80747	19.598067	190.267728	48.8163504	306.2341	54939.6906365741	2009-04-18 16:34:31	54941.5550810185	2009-04-20 13:19:19	704053010	76.4837	75	76.4837	76.4837	0	76.4837	2	2	0	2	1	0	0	63.948	63.948	161.0478	2	PROCESSED	57546.2140046296	2016-06-07 05:08:10	55318	2010-05-02 00:00:00	54952.1320717593	2009-05-01 03:10:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041432	The discovery of `Hanny's Voorwerp' near IC 2497 opens an unprecedented window into the time evolution of a single AGN on timescales up to 100,000 years. Based on its properties, the Voorwerp was illuminated by a luminous AGN ~100,000 years ago, but the AGN host galaxy - IC 2497 - does not seem to host a sufficiently luminous AGN. Thus, IC 2497 either hosts a highly obscured AGN only detectable in hard X-rays, or it has dropped in luminosity by a factor of 10-1000. We propose to observe IC 2497 with Suzaku for 75 ksec to determine the hard X-ray luminosity and spectrum to measure the amount of obscuration and the current intrinsic luminosity of its AGN. Only with hard X-ray observations can we break the degeneracy between obscuration and decrease in luminosity.	EXTRAGALACTIC COMPACT SOURCES	7	A	KEVIN SCHAWINSKI		USA	4	AO4	HOW FAST CAN AN AGN SHUT DOWN? - SUZAKU OBSERVATION OF IC 2497 AND `HANNY'S VOORWERP'	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704053010/	Quick Look
310	IC 342 X2	56.516	68.1498	55.302778	67.99381	72.573568	46.727351	138.08335694	10.57829767	91.9969	55415.9786689815	2010-08-07 23:29:17	55417.3765625	2010-08-09 09:02:15	705009010	74.379	80	74.379	74.379	0	74.379	2	2	0	2	1	0	0	64.1316	64.1316	120.7679	0	PROCESSED	57552.9205671296	2016-06-13 22:05:37	55794	2011-08-21 00:00:00	55428.1624537037	2010-08-20 03:53:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050041	The nature of ultraluminous X-ray sources (ULXs) is one of the important unresolved issues in the modern astrophysics. A Suzaku HXD spectrum above 10 keV and its variation, in combination with those with XIS, provide us with an unique opportunity to determine unambiguously the physical state of ULXs, which is a key information to solve their nature. Here, two 80 ks Suzaku exposures are proposed on a bright ULX IC 342 X2, one of the most promising candidates for hard X-ray detection.	EXTRAGALACTIC COMPACT SOURCES	7	A	NAOKI ISOBE		JAP	5	AO5	HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705009010/	Quick Look
311	LEDA 84274	220.5853	66.0952	220.354238	66.306919	158.410677	70.66779	106.75984756	47.40039166	359.2838	55331.3858333333	2010-05-15 09:15:36	55332.0542824074	2010-05-16 01:18:10	705023010	49.465	50	49.465	49.465	0	49.465	2	2	0	2	1	0	0	40.8385	40.8385	57.7519	1	PROCESSED	57551.5334143518	2016-06-12 12:48:07	55769	2011-07-27 00:00:00	55403.1228125	2010-07-26 02:56:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050074	We propose Suzaku XIS and HXD/PIN observations of two buried Active Galactic Nuclei(AGNs) at z=0.04 which are discovered by the AKARI mid-infrared all-sky survey. Both objects only show AGN features in AKARI near- and mid-infrared obsevations, while there are no clues of AGN presence in previous X-ray survey of ROSAT, radio 20cm, near-infrared photometries of 2MASS and detail optical spectroscopic data. These results indicate that a central engine of the AGN is completely buried and the nature of this population of AGNs is only poorly understood. Therefore, the hard X-ray observations is needed in order to confirm the AGN presence as well as to estimate the amount of absorption component and the AGN energy.	EXTRAGALACTIC COMPACT SOURCES	7	B	SHINKI OYABU		JAP	5	AO5	SUZAKU SEARCH FOR DIRECT EVIDENCE OF SUPER MASSIVE BLACK HOLES IN BURIED ACTIVE GALACTIC NUCLEI DISCOVERED BY AKARI	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705023010/	Quick Look
312	CEN A S LOBE NO. 1	200.8664	-45.1602	200.128121	-44.89936	217.870253	-33.408756	308.83796576	17.34395301	288.0039	55418.6612962963	2010-08-10 15:52:16	55419.7758101852	2010-08-11 18:37:10	705032010	75.1654	80	75.1654	75.1654	0	75.1654	2	2	0	2	1	0	0	64.2728	64.2728	96.2818	0	PROCESSED	57552.9742476852	2016-06-13 23:22:55	55803	2011-08-30 00:00:00	55428.1537152778	2010-08-20 03:41:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051401	We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays).	EXTRAGALACTIC COMPACT SOURCES	7	B	GRZEGORZ MADEJSKI		USA	5	AO5	SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705032010/	Quick Look
313	CEN A S LOBE NO. 3	205.7514	-45.1409	204.991343	-44.889287	221.546575	-31.897052	312.39292182	16.78143613	279.0007	55420.9668981482	2010-08-12 23:12:20	55421.3452777778	2010-08-13 08:17:12	705034010	20.0575	20	20.0815	20.0735	0	20.0575	3	2	0	2	1	0	0	18.9436	18.9436	32.6879	1	PROCESSED	57552.9389467593	2016-06-13 22:32:05	55803	2011-08-30 00:00:00	55435.169537037	2010-08-27 04:04:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051401	We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays).	EXTRAGALACTIC COMPACT SOURCES	7	B	GRZEGORZ MADEJSKI		USA	5	AO5	SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705034010/	Quick Look
314	IGR J19378-0617	294.4023	-6.2869	293.733278	-6.400449	295.156006	15.047751	32.53385066	-13.11752642	260.9167	55485.0705324074	2010-10-16 01:41:34	55487.3016087963	2010-10-18 07:14:19	705055010	77.8014	80	77.8174	77.8014	0	77.8174	2	2	0	2	1	0	0	70.5712	70.5712	192.7439	1	PROCESSED	57553.8036226852	2016-06-14 19:17:13	55867	2011-11-02 00:00:00	55498.2386805556	2010-10-29 05:43:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052014	We propose to observe with Suzaku three Narrow Line Seyfert 1 galaxies detected by INTEGRAL/IBIS and/or Swift/BAT with a flux in excess of 1.5e-11 cgs in the 15-50keV band (corresponding to the HXD/PIN band). The proposed observations will provide rare high quality spectra of NLS1s in the 0.5-50keV band. The good quality data above 10keV will dramatically help us removing the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM-Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources.	EXTRAGALACTIC COMPACT SOURCES	7	A	GIOVANNI MINIUTTI		EUR	5	AO5	BROADBAND X-RAY PROPERTIES OF HARD-X-RAY-BRIGHT NLS1 GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705055010/	Quick Look
315	SMC X-1	19.2337	-73.4445	18.901627	-73.707724	312.330059	-66.462167	300.42986971	-43.55966827	9.1005	55673.6490625	2011-04-22 15:34:39	55674.1112037037	2011-04-23 02:40:08	706030030	15.6526	18	15.6526	15.6526	0	15.871	2	2	0	1	1	0	0	21.2614	21.2614	39.9199	1	PROCESSED	57601.5606597222	2016-08-01 13:27:21	56067	2012-05-20 00:00:00	55692.2968634259	2011-05-11 07:07:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030030/	Quick Look
316	1ES 1927+654	291.8157	65.5862	291.743016	65.482913	3.782751	81.150517	97.0030083	20.97400385	83.4311	55667.8280092593	2011-04-16 19:52:20	55669.2425115741	2011-04-18 05:49:13	706006010	71.8889	100	71.9129	71.8889	0	71.9129	2	2	0	2	1	0	0	79.6647	79.6647	122.1919	0	PROCESSED	57601.5407986111	2016-08-01 12:58:45	56059	2012-05-12 00:00:00	55691.2683912037	2011-05-10 06:26:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060008	1ES 1927+654, an X-ray unabsorbed optically classified type-2 AGN, challenges the standard unified model. What is known about its X-ray characteristics suggest it can provide tremendous insight. It is extremely bright and will render close to 20 ct/s in the combined XIS providing sufficient data to unambiguously detect features in the Fe~K region, distinguish absorption and reflection models, and study its rapid variability. Even in the most conservative estimates a PIN detection is expected. It is persistently variable on short time scales and in combination with the long duration of Suzaku observations, the proposed observationswill yield fruitful variability studies. It has never been observed by Suzaku thus guaranteeing significant opportunity for discovery.	EXTRAGALACTIC COMPACT SOURCES	7	B	LUIGI GALLO		JAP	6	AO6	REVEALING THE NATURE OF AN X-RAY ABSORBED SEYFERT 2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706006010/	Quick Look
317	PG 1626+554	247.0224	55.3701	246.753118	55.479335	214.524979	74.372261	84.50112094	42.16849703	200.5289	55876.6090046296	2011-11-11 14:36:58	55877.9341550926	2011-11-12 22:25:11	706017010	60.8488	60	60.8488	60.8488	0	60.8488	2	2	0	2	1	0	0	56.1328	56.1328	114.4639	2	PROCESSED	57603.7696412037	2016-08-03 18:28:17	56256	2012-11-25 00:00:00	55890.6981828704	2011-11-25 16:45:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060069	Measurement of iron abundance in active galactic nuclei (AGN) relative to that of alpha-elements possesses potential of elucidating the cosmic chemical evolution, in particular, when the formation of the first stars initiated. However, it has been found that iron abundances estimated from FeII(opt) and FeII(UV) in the broad line region (BLR) do not agree and their ratio is dependent on the BLR cloud column densities. Thus, in order to derive precise AGN iron abundances, independent measurement of the BLR cloud column densities is required. Here we propose to obtain precise X-ray energy spectra of several AGNs, of which FeII(opt)/FeII(UV) values we have already measured. By combining the optical and X-ray spectra, we can estimate iron abundances of these targets more precisely than ever.	EXTRAGALACTIC COMPACT SOURCES	7	C	HIROAKI SAMESHIMA		JAP	6	AO6	X-RAY MEASUREMENTS OF COLUMN DENSITIES OF THE BROAD LINE REGION CLOUDS TO CONSTRAIN THE COSMIC CHEMICAL EVOLUTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706017010/	Quick Look
318	MRK 841	226.0091	10.4587	225.405512	10.653095	220.178836	26.612533	11.24319757	54.63999984	112.9994	55931.8646180556	2012-01-05 20:45:03	55937.1896990741	2012-01-11 04:33:10	706029010	244.3518	350	244.3518	244.3518	0	244.3598	2	2	0	2	1	0	0	229.726	229.726	419.686	4	PROCESSED	57604.4310648148	2016-08-04 10:20:44	55652	2011-04-01 00:00:00	55946.5082407407	2012-01-20 12:11:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061119	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	6	AO6-LP	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706029010/	Quick Look
319	NGC 2110	88.0457	-7.4586	87.441571	-7.469572	87.744639	-30.884812	212.92775975	-16.54787795	79.201	56170.1053009259	2012-08-31 02:31:38	56172.5412268518	2012-09-02 12:59:22	707034010	103.2595	100	103.2595	103.2595	0	103.2595	2	2	0	2	1	0	0	102.8063	102.8063	210.4361	1	PROCESSED	57607.0102199074	2016-08-07 00:14:43	56667	2014-01-10 00:00:00	56301.6411458333	2013-01-09 15:23:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071426	We request two 100 ks	EXTRAGALACTIC COMPACT SOURCES	7	B	ELIZABETH RIVERS		USA	7	AO7	TRACKING THE PARTIAL COVERING ABSORBERS IN NGC 2110: CONSTRAINTS FOR CLUMPY ABSORBER MODELS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707034010/	Quick Look
320	MRK 478	220.4959	35.3708	219.98335	35.583266	202.392109	47.875746	59.0913373	65.0766343	294.6097	55756.9652777778	2011-07-14 23:10:00	55758.8334837963	2011-07-16 20:00:13	706041010	85.3236	80	85.3316	85.3396	0	85.3236	3	2	0	2	1	0	0	77.6366	77.6366	161.3897	1	PROCESSED	57602.6370601852	2016-08-02 15:17:22	56151	2012-08-12 00:00:00	55783.7198842593	2011-08-10 17:16:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062028	The NLS1 galaxy Mrk 478 has exceptionally unusual properties. It shows up to a factor of five variability while keeping its spectral shape constant. Previous short XMM-Newton observations show that it is probably reflection-dominated, where light-bending effects are at their extreme. This is the only known object that shows such high variability while remaining in a reflection-dominated state. All other known objects show reflection-dominated spectra only when in a faint state, making their study very difficult. This object is reflection-dominated yet bright enough to study with relatively short exposures.Here we propose to observe this object for 80 ks. The goal is to detect the reflection hump using Suzaku capabilities above 10 keV and probe light-bending around this black hole.	EXTRAGALACTIC COMPACT SOURCES	7	A	ABDERAHMEN ZOGHBI		EUR	6	AO6	PROBING EXTREME RELATIVISITC LIGHT-BENDING IN MRK 478	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706041010/	Quick Look
321	1730-130	263.2641	-13.0933	262.559168	-13.058946	263.324851	10.191548	12.02258907	10.80244107	271.1606	55829.6599537037	2011-09-25 15:50:20	55830.0946643518	2011-09-26 02:16:19	706046010	11.0858	10	11.0938	11.0938	0	11.0858	1	1	0	1	1	0	0	9.8811	9.8811	37.5359	1	PROCESSED	57603.2457407407	2016-08-03 05:53:52	56225	2012-10-25 00:00:00	55875.6203703704	2011-11-10 14:53:20	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061601	We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	6	AO6	EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706046010/	Quick Look
322	ESO 565-G019	143.6802	-21.9346	143.106087	-21.711094	154.563677	-34.141633	253.87283017	21.67453181	298.0016	56067.8709259259	2012-05-20 20:54:08	56069.9022222222	2012-05-22 21:39:12	707013010	78.9239	80	78.9239	78.9319	0	78.9319	2	2	0	2	1	0	0	71.1211	71.1211	175.4878	2	PROCESSED	57605.5328935185	2016-08-05 12:47:22	56448	2013-06-05 00:00:00	56079.3396643518	2012-06-01 08:09:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070067	The nature of the hard X-ray emission of many AGN remains ill-understood. Using the latest 70 month Swift/BAT sky survey, we have selected optically-classified Seyfert 2s with a very hard BAT photon index (Gamma<1.4). The BAT energy range is not strongly affected by obscuration unless the column is Compton-thick. The selected sources are radio-quiet, arguing against jet-dominated non-thermal spectra. The cause of a low Gamma is unknown, but may include high or atypical obscuration, non-thermal X-ray emission without associated radio/optical jets or the presence of electron coronae with temperatures or optical depths higher than average. Our aim is to observe two of the hardest Seyfert 2s (neither of which has prior pointed observations below 10 keV) with Suzaku to elucidate their nature.	EXTRAGALACTIC COMPACT SOURCES	7	A	POSHAK GANDHI		JAP	7	AO7	WHAT IS THE NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707013010/	Quick Look
323	ESO 511-G030	214.8452	-26.646	214.125789	-26.416487	221.403618	-12.022581	326.22952078	32.2164843	286.9689	56130.0282407407	2012-07-22 00:40:40	56136.3340856482	2012-07-28 08:01:05	707023020	224.0255	270	224.0255	224.0255	0	224.0335	2	2	0	2	1	0	0	195.6334	195.6334	410.8958	3	PROCESSED	57606.8434606482	2016-08-06 20:14:35	56646	2013-12-20 00:00:00	56279.0046064815	2012-12-18 00:06:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071413	The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		USA	7	AO7	MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707023020/	Quick Look
324	SNR 1987A	83.833	-69.2775	83.924877	-69.307216	307.543742	-86.433259	279.71430694	-31.94790633	135.9732	56233.5143981482	2012-11-02 12:20:44	56234.854375	2012-11-03 20:30:18	707020010	81.2764	80	81.2764	81.2844	0	81.2924	2	2	0	2	1	0	0	78.5842	78.5842	115.7599	0	PROCESSED	57607.9555439815	2016-08-07 22:55:59	56611	2013-11-15 00:00:00	56245.4956365741	2012-11-14 11:53:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071331	Despite extensive observations of supernova remnant (SNR) 1987A with Chandra and XMM-Newton, the origin of the hard band (3-10 keV) X-ray emission is elusive (thermal vs nonthermal). A straightforward way to discriminate the thermal and nonthermal origins of the hard X-rays is to detect Fe K lines. The Suzaku XIS provides a uniquely efficient opportunity for a sensitive search for the Fe K lines, which is an excellent complement to the existing Chandra and XMM-Newton studies of SNR 1987A. Thus, we propose an 80 ks Suzaku observation of SNR 1987A.	EXTRAGALACTIC COMPACT SOURCES	7	C	SANGWOOK PARK		USA	7	AO7	X-RAY EMISSION FROM SUPERNOVA REMNANT 1987A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707020010/	Quick Look
325	RE J1034+396	158.663	39.6488	157.936699	39.907419	144.538164	28.290615	180.26295059	59.06449262	115.7032	56245.9648726852	2012-11-14 23:09:25	56248.0689583333	2012-11-17 01:39:18	707039010	99.9113	100	99.9193	99.9113	0	99.9193	2	2	0	2	1	0	0	93.446	93.446	181.7639	3	PROCESSED	57608.0485416667	2016-08-08 01:09:54	56640	2013-12-14 00:00:00	56274.6249884259	2012-12-13 14:59:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072005	Understanding the nature of the emission from the extreme active galaxy, RE J1034+396 can help us to unravel the properties of accretion as the Eddington limit is reached. A fleeting glimpse of the unique quasi-periodic oscillation (QPO) in this source has shown a complex timing behaviour with the emission below ~2 keV apparently crucial to its presence. Thus by understanding the origin and properties of the soft emission we can probe the physical mechanism of signals that cannot be resolved in stellar mass X-ray binaries but must be associated with the regions closest to the black hole. A new observation with Suzaku will allow a much deeper analysis of the soft emission and will shed light on how its changing properties can trigger such unique behaviour as the QPO.	EXTRAGALACTIC COMPACT SOURCES	7	C	MATTHEW MIDDLETON		EUR	7	AO7	REVEALING THE NATURE OF RE J1034+396 AND THE EXTREME SOFT EXCESS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707039010/	Quick Look
326	CTA102	338.1458	11.7401	337.526658	11.482274	344.409824	19.371456	77.43997335	-38.57166798	72.4263	56431.345462963	2013-05-19 08:17:28	56431.6134606482	2013-05-19 14:43:23	707045010	9.5626	10	9.5706	9.5626	0	9.5706	1	1	0	1	1	0	0	7.283	7.283	23.1439	0	PROCESSED	57611.3187847222	2016-08-11 07:39:03	56809	2014-06-01 00:00:00	56443.5010069444	2013-05-31 12:01:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071601	We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	7	AO7	MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707045010/	Quick Look
327	ESO 119-G008	72.2547	-57.6544	72.033322	-57.73981	38.878903	-77.915205	266.66680471	-38.87724734	324.43	56411.0111458333	2013-04-29 00:16:03	56413.2355787037	2013-05-01 05:39:14	708004010	100.5873	100	100.5953	100.5953	0	100.5873	2	2	0	2	1	0	0	103.7614	103.7614	192.1719	3	PROCESSED	57611.2384375	2016-08-11 05:43:21	56837	2014-06-29 00:00:00	56475.7648611111	2013-07-02 18:21:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080027	At faint fluxes, the Swift/BAT AGN survey is uncovering sources with very hard photon indices (Gamma) above 10 keV. The origin of a low Gamma in the hard band is ill-understood, but may include high/atypical obscuration, non-thermal X-rays without radio jets, or electron coronae with high temperatures or optical depths. In AO7, we observed two such Seyfert 2s and discovered Compton-thick obscuration in one source, and a buried AGN spectrum with no reflection or high-energy cutoff in the other. The hard BAT Gamma values thus have a variety of origins, and our strategy is very effective in selecting objects with interesting spectra. Here, we propose to observe two hardest sources (Gamma<~1) with no prior X-ray observations below 10 keV in order to shed light on the nature of this population.	EXTRAGALACTIC COMPACT SOURCES	7	A	POSHAK GANDHI		JAP	8	AO8	THE VARIED NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708004010/	Quick Look
328	NGC 3516	166.7239	72.5839	165.871383	72.854298	123.356587	58.000243	133.21571384	42.39397937	129.7498	56600.2605671296	2013-11-04 06:15:13	56601.215474537	2013-11-05 05:10:17	708006060	46.2	50	46.2	46.2	0	46.2	2	2	0	2	1	0	0	45.1764	45.1764	82.502	1	PROCESSED	57613.2009722222	2016-08-13 04:49:24	56383	2013-04-01 00:00:00	56646.7076041667	2013-12-20 16:58:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080066	We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	8	AO8	THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006060/	Quick Look
329	LEDA 168563	73.0158	49.5506	72.064208	49.467096	77.740518	26.831198	157.24701812	3.42018054	86.3166	56536.8773611111	2013-09-01 21:03:24	56539.0592708333	2013-09-04 01:25:21	708017010	100.011	100	100.035	100.011	0	100.035	3	2	0	2	1	0	0	92.947	92.947	188.5018	1	PROCESSED	57612.530162037	2016-08-12 12:43:26	56383	2013-04-01 00:00:00	56608.7327893518	2013-11-12 17:35:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081413	We propose to carry out Suzaku observations, a 100 ks each, of three Seyfert I nuclei hard X-ray selected by Swift. Our goal is to distinguish between various competing models proposed for the X-ray spectra of Seyfert I nuclei. Especially we will test, by observing these targets, the ionized relativistic reflection (hereafter IRR). We will take advantage of Suzaku s unique capability of detecting hard X-rays beyond 10 keV by its HXD-PIN, simultaneously with X-rays in lower to medium energy bands by its XIS on board. With our proposed studies we will gain deeper understanding of accretion-powered AGN in general. Since the IRR takes place close to the black hole we will test the effects of strong gravity, such as the black hole spin.	EXTRAGALACTIC COMPACT SOURCES	7	B	SACHIKO TSURUTA		USA	8	AO8	SPECTRAL STUDIES OF SOME HARD X-RAY SELECTED SEYFERT NUCLEI	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708017010/	Quick Look
330	IGR J09026-4812	135.6468	-48.2323	135.224236	-48.033912	164.675258	-60.400706	268.86967218	-1.09239209	115.8572	56622.3203356482	2013-11-26 07:41:17	56622.9521990741	2013-11-26 22:51:10	708031010	37.7924	35	37.8244	37.8164	0	37.7924	2	2	0	2	1	0	0	35.2029	35.2029	54.5859	1	PROCESSED	57613.429212963	2016-08-13 10:18:04	56383	2013-04-01 00:00:00	56632.5852777778	2013-12-06 14:02:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081419	The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come.	EXTRAGALACTIC COMPACT SOURCES	7	C	TAHIR YAQOOB		USA	8	AO8	ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708031010/	Quick Look
331	ABELL 981	156.0884	68.0988	155.16023	68.352315	123.8863	52.287736	140.87577234	43.55064218	119.4308	56601.2179398148	2013-11-05 05:13:50	56601.7917708333	2013-11-05 19:00:09	708040010	27.5945	30	27.6025	27.5945	0	27.5945	2	2	0	2	1	0	0	25.286	25.286	49.574	1	PROCESSED	57613.2182060185	2016-08-13 05:14:13	56980	2014-11-19 00:00:00	56614.6564583333	2013-11-18 15:45:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081533	We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters.	EXTRAGALACTIC COMPACT SOURCES	7	C	LAURENCE DAVID		USA	8	AO8	MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708040010/	Quick Look
332	PG 1404+226	211.5907	22.3868	211.009924	22.624644	200.393386	32.82418	21.44706338	72.36251102	287.2346	56486.8565972222	2013-07-13 20:33:30	56489.1889583333	2013-07-16 04:32:06	708045010	102.3327	100	102.3704	102.3327	0	102.3625	2	2	0	2	1	0	0	95.3407	95.3407	201.5059	2	PROCESSED	57612.0131828704	2016-08-12 00:18:59	56872	2014-08-03 00:00:00	56503.7358796296	2013-07-30 17:39:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082010	Suzaku observations reveal evidence of relativistically-broadened emission lines from the inner regions of supermassive black holes, providing a unique tool for studying accreting systems. It is understood that the X-ray source is compact at low-fluxes, and increases in size at higher fluxes. Thus variable sources are essential for probing the physics of the innermost regions. Previous studies of the low-flux 'state' have been limited by low count rates. We propose to observe PG 1404+226, which shares many properties of other AGN showing reverberation, but even at low-fluxes, it is a factor of three brighter than similar objects. This source, never before observed with Suzaku, provides a unique opportunity for probing strong-field accretion because of its high luminosity and variability.	EXTRAGALACTIC COMPACT SOURCES	7	B	ERIN KARA		EUR	8	AO8	MAPPING THE X-RAY EMISSION IN THE VICINITY OF THE BLACK HOLE PG 1404+226	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708045010/	Quick Look
333	FAIRALL 51	281.2261	-62.3592	280.062181	-62.410627	276.679536	-39.178599	333.20510197	-23.08989761	251.799	56540.8073958333	2013-09-05 19:22:39	56541.1744212963	2013-09-06 04:11:10	708046020	30.958	30	30.958	30.958	0	30.9646	1	1	0	1	1	0	0	23.2171	23.2171	31.7039	0	PROCESSED	57612.5333333333	2016-08-12 12:48:00	56956	2014-10-26 00:00:00	56588.7741319444	2013-10-23 18:34:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082016	Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures.	EXTRAGALACTIC COMPACT SOURCES	7	A	JIRI SVOBODA		EUR	8	AO8	STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708046020/	Quick Look
334	NGC 3998	179.4698	55.4443	178.823114	55.722594	149.626555	48.892783	138.19460038	60.06850959	319.2188	56780.8797569445	2014-05-03 21:06:51	56782.5966898148	2014-05-05 14:19:14	709002010	80.6754	80	80.6754	80.6754	0	80.6754	2	2	0	2	1	0	0	76.8901	76.8901	148.2858	0	PROCESSED	57615.0693981482	2016-08-15 01:39:56	57159	2015-05-17 00:00:00	56793.5775	2014-05-16 13:51:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090017	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	9	AO9	BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709002010/	Quick Look
335	NGC2110	88.0489	-7.4533	87.444745	-7.464256	87.748433	-30.879563	212.92425635	-16.54269345	269.0605	57101.7987152778	2015-03-20 19:10:09	57103.3044328704	2015-03-22 07:18:23	709011010	45.6257	50	45.6257	49.4936	0	49.5096	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8483564815	2016-08-17 20:21:38	57558	2016-06-19 00:00:00	57190.4658333333	2015-06-17 11:10:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090062	We propose to observe the Seyfert galaxy NGC2110 twice every half year, which showed a big flare by a factor of around 5 against the normal state around 2012 December. We can observe the echo history following the flare in a time scale of years, and then measure the reflection spectrum very accurately to constrain the geometry of the reflection torus.	EXTRAGALACTIC COMPACT SOURCES	7	A	YASUSHI FUKAZAWA		JAP	9	AO9	X-RAY ECHO OF THE BIG FLARE OF SEYFERT GALAXY NGC2110	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709011010/	Quick Look
336	HOLMBERG IX X-1	149.4572	69.0544	148.43919	69.292844	119.777434	51.680142	141.94722641	41.07197433	311.5038	57118.9110416667	2015-04-06 21:51:54	57119.5667708333	2015-04-07 13:36:09	709015030	31.5263	30	31.5263	31.5263	0	31.5263	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.9243402778	2016-08-17 22:11:03	57513	2016-05-05 00:00:00	57129.4193171296	2015-04-17 10:03:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091251	Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs.	EXTRAGALACTIC COMPACT SOURCES	7	A	DOMINIC WALTON		USA	9	AO9	MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015030/	Quick Look
337	OJ 287	133.705	20.1043	132.989927	20.295379	130.505973	2.596868	206.81753743	35.82068078	285.8744	57148.4467708333	2015-05-06 10:43:21	57151.4189351852	2015-05-09 10:03:16	710011020	110.2819	323	110.2819	112.3099	0	112.3099	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.1271643518	2016-08-18 03:03:07	57113	2015-04-01 00:00:00	57164.5272337963	2015-05-22 12:39:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101431	Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously.	EXTRAGALACTIC COMPACT SOURCES	7	A	RICK EDELSON		USA	10	AO10	SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011020/	Quick Look
338	OJ 287	133.7049	20.1044	132.989827	20.295479	130.505855	2.596938	206.81738245	35.82062575	285.8744	57151.4189467593	2015-05-09 10:03:17	57154.3266666667	2015-05-12 07:50:24	710011030	107.7143	323	107.7143	107.7143	0	107.7143	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.6879166667	2016-08-18 16:30:36	57113	2015-04-01 00:00:00	57164.5596527778	2015-05-22 13:25:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101431	Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously.	EXTRAGALACTIC COMPACT SOURCES	7	A	RICK EDELSON		USA	10	AO10	SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011030/	Quick Look
339	MRK421	166.1418	38.2711	165.447021	38.540933	151.207571	29.566146	179.67525089	65.03258412	111.0988	54803.7278240741	2008-12-03 17:28:04	54805.9480324074	2008-12-05 22:45:10	703020010	101.3075	100	101.3315	101.3075	0	101.3315	2	2	0	2	1	0	0	65.5148	65.5148	191.7877	3	PROCESSED	57544.7029398148	2016-06-05 16:52:14	55188	2009-12-23 00:00:00	54818.7659837963	2008-12-18 18:23:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030119	Mrk421 provides our best opportunity to understand the high-energy emission of blazar jets, because it has produced the largest observed flux. Suzaku HXD has proved that spectum upto 40 keV can be measured only with an exposure of 1 ks from Mrk 421. Hard X-ray region is very crucial to study particle acceleration in the jet, since it corresponds to high energy end of electron distribution. Cooling and Acceleration phenomena will appear in this energy band. Here we will propose to monitor Mrk 421 for 200 ks, in which we can expect at least four or five flares.	EXTRAGALACTIC COMPACT SOURCES	7	B	TADAYUKI TAKAHASHI		JAP	3	AO3	STUDY OF HARD X-RAY EVOLUTION FROM THE BRIGHTEST BLAZAR JET.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703020010/	Quick Look
340	I ZW 18	143.5151	55.2494	142.632451	55.471905	125.701519	38.241912	160.51246258	44.84288886	130.2629	56934.0191666667	2014-10-04 00:27:36	56935.6258680556	2014-10-05 15:01:15	709021020	82.0708	70	82.0708	82.0868	0	82.0868	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6143865741	2016-08-16 14:44:43	57358	2015-12-02 00:00:00	56989.5111689815	2014-11-28 12:16:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091441	The source of energetic photons that reionized and heated the early universe remains uncertain. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectrum with the Suzaku XIS. These observations are important to our understanding of the heating of the universe during the epoch of reionization.	EXTRAGALACTIC COMPACT SOURCES	7	A	PHILIP KAARET		USA	9	AO9	X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709021020/	Quick Look
341	3C279	194.0685	-5.7338	193.421343	-5.463366	195.163667	0.26086	305.14803375	57.11713803	113.6423	54850.9795833333	2009-01-19 23:30:36	54853.9391203704	2009-01-22 22:32:20	703049010	134.1106	200	134.1106	134.1106	0	134.1106	2	2	0	2	1	0	0	82.8563	82.8563	255.689	7	PROCESSED	57545.3939351852	2016-06-06 09:27:16	55328	2010-05-12 00:00:00	54880.5781365741	2009-02-18 13:52:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031346	We propose a 200 ks observation of 3C279, the archetypal EGRET blazar to be conducted simultaneously with GLAST as well as many other facilities, with the goal of obtaining broadband spectra and light-curves. The flux in all observable bands is known to be rapidly variable, but the information regarding the correlation between the time history of flux in various bands is limited, and the proposed observations are designed to remedy this shortcoming. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles.	EXTRAGALACTIC COMPACT SOURCES	7	A	GRZEGORZ MADEJSKI		USA	3	AO3	SUZAKU AND GLAST OBSERVATIONS OF 3C279	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703049010/	Quick Look
342	NGC 4258	184.7518	47.3153	184.134648	47.592794	160.376562	44.164981	138.28789039	68.83430148	139.1798	55511.1601388889	2010-11-11 03:50:36	55512.7112615741	2010-11-12 17:04:13	705051010	103.8332	100	103.8332	103.8412	0	103.837	2	2	0	2	1	0	0	86.2257	86.2257	133.9688	1	PROCESSED	57554.0812384259	2016-06-15 01:56:59	55903	2011-12-08 00:00:00	55537.1754398148	2010-12-07 04:12:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051451	We request a 100 ksec observation of the Low Luminosity AGN NGC 4258. This observation is meant to complement our existing 100 ksec Suzaku observation (Reynolds et al. 2009), and our 320 ksec Chandra-HETG observation (Murphy et al., in prep.). The goal is to further characterize the observed variability of the Fe Kalpha line and any associated changes in the continuum and/or absorption of NGC 4258. Given the unique constraints that we have on the mass, distance and accretion flow geometry in NGC 4258, as well as its role as a bridge between the most quiescent nuclei and powerful AGN, further Suzaku studies of NGC 4258 are clearly warranted.	EXTRAGALACTIC COMPACT SOURCES	7	C	MICHAEL NOWAK		USA	5	AO5	HUNTING FOR THE VARIABLE IRON LINE IN NGC 4258	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705051010/	Quick Look
343	MCG-6-30-15	203.9717	-34.2976	203.255303	-34.04246	215.173232	-22.546653	313.28966663	27.67858669	102.4356	53758.5062962963	2006-01-23 12:09:04	53761.0835648148	2006-01-26 02:00:20	700007020	98.4834	300	98.4834	98.4834	98.4834	98.4834	2	2	2	2	1	0	0	81.8922	81.8922	222.6497	3	PROCESSED	57532.8430902778	2016-05-24 20:14:03	54247	2007-05-27 00:00:00	54059.5463773148	2006-11-20 13:06:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001035	The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales .	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREW FABIAN		JAP	0	SWG	REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007020/	Quick Look
344	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
345	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
346	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
347	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
348	NGC1386	54.1629	-35.9533	53.686009	-36.117288	37.868182	-53.108166	237.58696036	-53.99184818	64.5172	54309.0884259259	2007-07-28 02:07:20	54310.1668402778	2007-07-29 04:00:15	702002010	55.5226	50	55.5226	55.5306	0	55.5306	2	2	0	2	1	0	0	47.5213	47.5213	93.1439	1	PROCESSED	57539.3619907407	2016-05-31 08:41:16	54707	2008-08-29 00:00:00	54339.0775115741	2007-08-27 01:51:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020005	Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei.	EXTRAGALACTIC COMPACT SOURCES	7	A	HISAMITSU AWAKI		JAP	2	AO2	REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702002010/	Quick Look
349	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
350	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
351	NGC3393	162.075	-25.2139	161.475136	-24.949432	174.292392	-30.103718	270.6699706	29.83420275	292.9271	54243.7827662037	2007-05-23 18:47:11	54245.1876041667	2007-05-25 04:30:09	702004010	55.227	50	55.227	55.227	0	55.227	2	2	0	2	1	0	0	48.255	48.255	121.3699	4	PROCESSED	57538.7560416667	2016-05-30 18:08:42	54745	2008-10-06 00:00:00	54255.6532986111	2007-06-04 15:40:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020005	Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei.	EXTRAGALACTIC COMPACT SOURCES	7	A	HISAMITSU AWAKI		JAP	2	AO2	REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702004010/	Quick Look
352	LMC X-4	83.1883	-66.3595	83.179882	-66.392572	1.044909	-87.279168	276.32310713	-32.53751505	226.9099	54507.0294560185	2008-02-11 00:42:25	54507.6043287037	2008-02-11 14:30:14	702037010	23.3814	20	23.3894	23.3974	0	23.3814	1	1	0	1	1	0	0	20.047	20.047	49.662	1	PROCESSED	57541.5628356482	2016-06-02 13:30:29	54883	2009-02-21 00:00:00	54515.5898842593	2008-02-19 14:09:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021127	We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects.	EXTRAGALACTIC COMPACT SOURCES	7	A	RYAN HICKOX		USA	2	AO2	SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702037010/	Quick Look
353	3C 445	335.9528	-2.0995	335.30761	-2.353112	336.949965	7.376595	61.86726076	-46.70852053	68.9567	54245.2015046296	2007-05-25 04:50:10	54248.9169444444	2007-05-28 22:00:24	702056010	139.7691	125	139.7691	139.7691	0	139.7691	2	2	0	2	1	0	0	117.2412	117.2412	320.9918	4	PROCESSED	57538.8276967593	2016-05-30 19:51:53	54702	2008-08-24 00:00:00	54256.717662037	2007-06-05 17:13:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021352	It is well known that the circum-black hole environ of Seyferts contain warm, photoionized gas responsible for complex absorption/emission at X-rays. Evidence for such components in radio-loud AGN is, instead, rare. And yet, presence of an ionized, scattering medium is postulated by unification models for these sources, and some models for jet formation. Here we tackle this problem by proposing sensitive Suzaku observations of 3C445, the only Broad-Line Radio Galaxy exhibiting soft X-ray emission lines from 0.4-3 keV in an archival EPIC spectrum. We will: 1) Determine the broad-band continuum; 2) Study the properties of the soft emission lines, determining the gas density and location, and thus its role in jet collimation; and 3) Confirm the strong reflection component suggested by EPIC.	EXTRAGALACTIC COMPACT SOURCES	7	A	RITA SAMBRUNA		USA	2	AO2	WARM GAS IN THE INNER REGIONS OF RADIO-LOUD AGN: THE CASE OF 3C445	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702056010/	Quick Look
354	Q0450-1310	73.3011	-13.0912	72.722633	-13.172561	69.927484	-35.377207	211.74785299	-32.06702416	263.6423	54535.8878240741	2008-03-10 21:18:28	54536.2502314815	2008-03-11 06:00:20	702062010	15.5102	13	15.5102	15.5102	0	15.5102	2	2	0	2	1	0	0	14.9887	14.9887	31.3059	0	PROCESSED	57541.8181828704	2016-06-02 19:38:11	54916	2009-03-26 00:00:00	54550.1640277778	2008-03-25 03:56:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021361	The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars.	EXTRAGALACTIC COMPACT SOURCES	7	C	GEORGE CHARTAS		USA	2	AO2	AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702062010/	Quick Look
355	XBONGBLUE2	217.7653	34.3413	217.240861	34.56211	200.146538	45.945194	57.71878971	67.47993323	130.3787	54454.1686921296	2007-12-20 04:02:55	54454.5050694445	2007-12-20 12:07:18	702084010	14.8162	13	14.8162	14.8162	0	14.8162	1	1	0	1	1	0	0	14.5794	14.5794	29.0559	0	PROCESSED	57540.9126851852	2016-06-01 21:54:16	54828	2008-12-28 00:00:00	54460.6654398148	2007-12-26 15:58:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021376	We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs.	EXTRAGALACTIC COMPACT SOURCES	7	C	CHRISTINE JONES		USA	2	AO2	OBSCURED AGN AND XBONGS IN BOOTES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702084010/	Quick Look
356	IRAS 05262+4432	82.4599	44.6406	81.547278	44.601887	84.24873	21.350791	165.01766257	5.72021917	78.2999	54721.6357523148	2008-09-12 15:15:29	54723.406412037	2008-09-14 09:45:14	703019010	82.086	80	82.0975	82.094	0	82.086	2	2	0	2	1	0	0	70.9075	70.9075	152.9541	0	PROCESSED	57543.8409490741	2016-06-04 20:10:58	55148	2009-11-13 00:00:00	54780.4562037037	2008-11-10 10:56:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030085	X-ray observations of obscured narrow-line Seyfert 1 galaxies (NLS1s) have never been performed effectively, in spite of the fact that absorbing material and nuclear emission of NLS1s are thought to be a crucial key to understand the fueling and accretion mechanisms, which may be directly related to the rapid evolution of supermassive black holes. We, therefore, propose 80 ksec observation of the candidate of an obscured NLS1 IRAS 05262+4432. High sensitivity throughout the 0.3-70 keV wide energy band of Suzaku allows us to strictly constrain the X-ray luminosity of primary emission and the geometry of the surrounding matter. From our observation, we expect to derive more complete unified picture of AGNs	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHITO HABA		JAP	3	AO3	SUZAKU VIEW OF OBSCURED NARROW-LINE SEYFERT 1 GALAXY IRAS 05262+4432	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703019010/	Quick Look
357	MRK 421	166.1081	38.2021	165.413329	38.471893	151.215505	29.492571	179.85015534	65.02934628	313.5582	54591.1196527778	2008-05-05 02:52:18	54595.3502199074	2008-05-09 08:24:19	703043010	180.7851	150	180.7931	180.7851	0	180.7931	2	2	0	2	1	0	0	163.5507	163.5507	343.6517	9	PROCESSED	57542.5998842593	2016-06-03 14:23:50	54972	2009-05-21 00:00:00	54606.5618287037	2008-05-20 13:29:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031341	We propose one 150 ksec Suzaku ToO observations of one of the three strong GeV-TeV gamma-ray blazars Mrk 421, Mrk 501, or 1ES 1959+650 during a 10 day multiwavelength campaign with coverage from radio to gamma-rays. The proposal is submitted by the VERITAS collaboration, assuring excellent TeV gamma-ray coverage. The Suzaku observations will play a key-role in interpreting the multiwavelength data set, allowing us to measure the time lag between the X-ray and gamma-ray flux variability and to scrutinize the correlation of the X-ray and gamma-ray spectral indices. The Suzaku and gamma-ray energy spectra will allow us to constrain the intensity of the IR Diffuse Extragalactic Background Radiation which absorbs TeV gamma-rays in extragalactic pairproduction processes.	EXTRAGALACTIC COMPACT SOURCES	7	A	HENRIC KRAWCZYNSKI		USA	3	AO3-TOO	TARGET OF OPPORTUNITY OBSERVATIONS OF THE BLAZARS MRK 421, MRK 501, AND 1ES 1959+650	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703043010/	Quick Look
358	NGC 4686	191.5508	54.5121	190.986823	54.785056	159.09559	52.489361	124.58283765	62.59936814	342.6621	54946.7002777778	2009-04-25 16:48:24	54947.7564699074	2009-04-26 18:09:19	704015010	44.8459	40	44.8539	44.8459	0	44.8459	2	2	0	2	1	0	0	42.3275	42.3275	91.232	0	PROCESSED	57546.4795717593	2016-06-07 11:30:35	55339	2010-05-23 00:00:00	54973.9296875	2009-05-22 22:18:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040060	Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe three Compton thick AGN candidates in the 22 months BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	4	AO4	DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704015010/	Quick Look
359	3C 35	18.0181	49.4424	17.27928	49.177164	38.209927	38.103766	126.37585323	-13.29131796	245.0044	55200.6165509259	2010-01-04 14:47:50	55202.466875	2010-01-06 11:12:18	704019010	84.7566	80	85.0286	84.7566	0	85.0206	2	2	0	2	1	0	0	66.3143	66.3143	147.5778	2	PROCESSED	57550.0615277778	2016-06-11 01:28:36	55584	2011-01-23 00:00:00	55218.1479050926	2010-01-22 03:32:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040096	Suzaku observations of two giant radio galaxies, 3C 35 and DA 240, with a total size of about 1 Mpc are proposed, in order to detect diffuse inverse Compton X-ray emission from their radio lobes. The X-ray flux from the lobes, in comparison with the radio one, provides a precise determination of electron and magnetic field energies there. A comparison of them with those in smaller radio galaxies is used to probe into the history of jets and lobes.	EXTRAGALACTIC COMPACT SOURCES	7	B	NAOKI ISOBE		JAP	4	AO4	SUZAKU OBSERVATION OF GIANT RADIO GALAXIES AS A PROBE OF JET HISTORY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704019010/	Quick Look
360	IGRJ01528	28.2011	-3.4464	27.56858	-3.692494	24.925792	-14.053354	157.35013019	-62.14500791	77.3667	55007.0338078704	2009-06-25 00:48:41	55008.1426388889	2009-06-26 03:25:24	704043010	46.9159	40	46.9159	47.6119	0	47.6248	3	2	0	2	1	0	0	42.1043	42.1043	95.7918	0	PROCESSED	57547.6882407407	2016-06-08 16:31:04	55386	2010-07-09 00:00:00	55019.1922337963	2009-07-07 04:36:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041414	We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc.	EXTRAGALACTIC COMPACT SOURCES	7	A	EZEQUIEL TREISTER		USA	4	AO4	THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704043010/	Quick Look
361	1150+497	178.3624	49.5318	177.710529	49.809967	153.770918	43.67464	145.51949415	64.97605225	131.4133	55512.7136805556	2010-11-12 17:07:42	55514.1042824074	2010-11-14 02:30:10	705003010	105.6558	100	105.7118	105.6558	0	105.7198	2	2	0	2	1	0	0	84.6438	84.6438	120.128	1	PROCESSED	57554.1053356482	2016-06-15 02:31:41	55892	2011-11-27 00:00:00	55524.2197337963	2010-11-24 05:16:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050007	A Suzaku observation of the iron line emitting blazar 1150+497 is proposed. The object is reported to exhibit a signature iron line. By measuring the equivalent width and line width, Suzaku will reveal the state of the accretion disc with the jet activity. It is notable that the blazar, aligning the jet with the line of sight, allow us to observe the jet and the accretion disc with a sufficient isochronism even with the violently variable sources.	EXTRAGALACTIC COMPACT SOURCES	7	C	HIROMI SETA		JAP	5	AO5	SUZAKU OBSERVATION OF AN FE-LINE BLAZAR 1150+497	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705003010/	Quick Look
362	EMS1535	345.6918	44.7374	345.120256	44.468031	9.799428	45.696922	103.4061071	-13.97501662	63.3944	55373.2448611111	2010-06-26 05:52:36	55374.0174768518	2010-06-27 00:25:10	705016010	42.3955	40	42.4035	42.3955	0	42.4035	1	1	0	1	1	0	0	42.7545	42.7545	66.7539	0	PROCESSED	57552.4062268518	2016-06-13 09:44:58	55772	2011-07-30 00:00:00	55404.2240625	2010-07-27 05:22:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050050	We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators".	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5	SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705016010/	Quick Look
363	1RXS J032613.6+02252	51.5615	2.4213	50.912043	2.246984	49.792333	-15.817317	180.7494445	-42.4285339	253.9336	55596.8403356482	2011-02-04 20:10:05	55597.6203125	2011-02-05 14:53:15	705038010	32.1971	32	32.1971	32.1971	0	32.1971	2	2	0	2	1	0	0	22.6441	22.6441	67.3879	1	PROCESSED	57600.8622106482	2016-07-31 20:41:35	55983	2012-02-26 00:00:00	55614.1886342593	2011-02-22 04:31:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051402	High frequency peaked BL Lacs are a peculiar subclass of Blazars characterized by non-thermal emission across the whole electromagnetic spectrum. Their spectral energy distributions (SEDs) include two main components: a low-energy component with power peaking in the range from the UV to the X-ray band, and a substantial high-energy component often dominated by gamma-rays. We propose 3 observations (32 ks each) of a selected sample of HBLs to study the behavior of the first component, widely interpreted as synchrotron radiation. First, we will be able to disentangle between different spectral shapes of the synchrotron SED of HBLs. Second, we will use the proposed observations to investigate the properties of the most representative sample of TeV candidate HBLs.	EXTRAGALACTIC COMPACT SOURCES	7	C	FRANCESCO MASSARO		USA	5	AO5	X-RAY CURVED SPECTRA IN HIGH FREQUENCY PEAKED BL LACS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705038010/	Quick Look
364	CBS 126	153.2712	35.8701	152.538495	36.117901	141.901695	23.115205	188.30426979	55.38335717	124.145	55487.3144907407	2010-10-18 07:32:52	55489.5529861111	2010-10-20 13:16:18	705042010	101.542	100	101.566	101.542	0	101.566	2	2	0	2	1	0	0	90.7438	90.7438	193.3897	2	PROCESSED	57553.8238541667	2016-06-14 19:46:21	55867	2011-11-02 00:00:00	55498.3270949074	2010-10-29 07:51:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051432	We propose to carry out a 100 ks Suzaku observation of Broad Line Seyfert 1 (BLS1) galaxy CBS 126. This source exhibits many properties which are thought to be typical of a Narrow Line Seyfert 1 (NLS1), such as a large soft X-ray excess and strong spectral variability, but unusual for a BLS1. Taking advantage of Suzaku's unique broad band X-ray energy window, our main goal is to clarify the nature of the unusual, variable, optically polarized spectrum of CBS 126. These interesting spectral features cover a wide energy range where Suzaku is ideal. With these proposed studies we will gain better understanding of accretion-powered AGN in general.	EXTRAGALACTIC COMPACT SOURCES	7	B	SACHIKO TSURUTA		USA	5	AO5	SPECTRAL AND TEMPORAL STUDIES OF THE SEYFERT 1 GALAXY CBS 126	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705042010/	Quick Look
365	NGC6251_LOBE	246.4248	82.6439	247.78516	82.752174	100.137256	73.058322	116.00587189	31.32598662	26.9674	55666.2760069444	2011-04-15 06:37:27	55667.0258564815	2011-04-16 00:37:14	706003010	38.0779	40	38.0779	38.0779	0	38.0779	2	2	0	2	1	0	0	37.5276	37.5276	64.784	0	PROCESSED	57601.5103356482	2016-08-01 12:14:53	56058	2012-05-11 00:00:00	55690.9897685185	2011-05-09 23:45:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060004	We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	6	AO6	SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706003010/	Quick Look
366	NGC6251_LOBE_BGD2	245.3877	82.3337	246.650515	82.446813	101.124392	73.239187	115.79036875	31.61025625	299.99	55789.4176967593	2011-08-16 10:01:29	55789.6225	2011-08-16 14:56:24	706005020	11.178	10	11.178	11.178	0	11.178	1	1	0	1	1	0	0	9.788	9.788	17.6879	0	PROCESSED	57602.7824421296	2016-08-02 18:46:43	56173	2012-09-03 00:00:00	55805.1871527778	2011-09-01 04:29:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060004	We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	6	AO6	SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706005020/	Quick Look
367	SWIFT J0709.4-3559	107.3109	-36.0226	106.863563	-35.940797	116.901156	-57.856606	247.327711	-12.25710974	260.0142	55653.0945601852	2011-04-02 02:16:10	55655.0640393518	2011-04-04 01:32:13	706008010	81.1739	80	81.1739	81.1739	0	81.1739	2	2	0	2	1	0	0	61.4621	61.4621	170.1239	2	PROCESSED	57601.393287037	2016-08-01 09:26:20	56037	2012-04-20 00:00:00	55670.2451967593	2011-04-19 05:53:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060030	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	6	AO6	BROAD BAND SPECTRA OF HARD X-RAY SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706008010/	Quick Look
368	PG 1322+659	200.9787	65.7065	200.558033	65.966727	149.375947	63.481771	117.62442893	51.08576313	141.5827	55892.4154050926	2011-11-27 09:58:11	55894.0862268518	2011-11-29 02:04:10	706018010	81.6869	80	81.7109	81.6869	0	81.7109	2	2	0	2	1	0	0	78.9168	78.9168	144.3439	2	PROCESSED	57603.9954513889	2016-08-03 23:53:27	56274	2012-12-13 00:00:00	55907.1929282407	2011-12-12 04:37:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060069	Measurement of iron abundance in active galactic nuclei (AGN) relative to that of alpha-elements possesses potential of elucidating the cosmic chemical evolution, in particular, when the formation of the first stars initiated. However, it has been found that iron abundances estimated from FeII(opt) and FeII(UV) in the broad line region (BLR) do not agree and their ratio is dependent on the BLR cloud column densities. Thus, in order to derive precise AGN iron abundances, independent measurement of the BLR cloud column densities is required. Here we propose to obtain precise X-ray energy spectra of several AGNs, of which FeII(opt)/FeII(UV) values we have already measured. By combining the optical and X-ray spectra, we can estimate iron abundances of these targets more precisely than ever.	EXTRAGALACTIC COMPACT SOURCES	7	C	HIROAKI SAMESHIMA		JAP	6	AO6	X-RAY MEASUREMENTS OF COLUMN DENSITIES OF THE BROAD LINE REGION CLOUDS TO CONSTRAIN THE COSMIC CHEMICAL EVOLUTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706018010/	Quick Look
369	RX J1633+4718	248.3661	47.3315	248.006234	47.43491	228.796037	67.698232	73.56753068	42.5999019	136.9343	55939.8747337963	2012-01-13 20:59:37	55940.8307407407	2012-01-14 19:56:16	706027030	44.1271	40	44.1271	44.1271	0	44.1271	2	2	0	2	1	0	0	38.9578	38.9578	82.592	0	PROCESSED	57604.3578703704	2016-08-04 08:35:20	56331	2013-02-08 00:00:00	55960.228587963	2012-02-03 05:29:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060089	RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time.	EXTRAGALACTIC COMPACT SOURCES	7	A	KIYOSHI HAYASHIDA		JAP	6	AO6	X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027030/	Quick Look
370	MRK 231	193.9205	56.8603	193.380984	57.130758	158.183244	55.13624	121.76268106	60.25831511	352.6128	55678.6054282407	2011-04-27 14:31:49	55682.3543402778	2011-05-01 08:30:15	706037010	197.5113	200	197.5113	197.5113	0	197.5113	2	2	0	2	1	0	0	191.7434	191.7434	323.8756	2	PROCESSED	57602.0326851852	2016-08-02 00:47:04	56065	2012-05-18 00:00:00	55697.4231597222	2011-05-16 10:09:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062008	We propose the first Suzaku observation of the nearest low-ionization BAL quasar/ULIRG, i.e. MRK 231, for which we have recently reported the most clear-cut evidence for AGN-driven feedback onto the host galaxy cold molecular gas component. Our target exhibits an hard X-ray (> 15 keV) excess in a previous BeppoSAX/PDS spectrum, suggesting the presence of a heavily obscured quasar at the heart of this peculiar system. By exploiting the Suzaku unique broad-band spectral coverage, we aim at deriving the column density of the nuclear absorber and, in turn, the intrinsic luminosity of the quasar with unprecedented accuracy.	EXTRAGALACTIC COMPACT SOURCES	7	A	ENRICO PICONCELLI		EUR	6	AO6	BROAD-BAND X-RAY SPECTROSCOPY OF THE NEAREST BAL QUASAR/ULIRG MARKARIAN 231	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706037010/	Quick Look
371	LMC X-4	83.1886	-66.3594	83.180179	-66.392471	1.047321	-87.279275	276.32297371	-32.53740633	226.9086	54500.7929513889	2008-02-04 19:01:51	54501.0521875	2008-02-05 01:15:09	702036010	0	20	0	0	0	0	0	0	0	0	1	0	0	5.6729	5.6729	22.3779	1	PROCESSED	57541.4899537037	2016-06-02 11:45:32	54883	2009-02-21 00:00:00	54515.6401851852	2008-02-19 15:21:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021127	We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects.	EXTRAGALACTIC COMPACT SOURCES	7	A	RYAN HICKOX		USA	2	AO2	SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702036010/	Quick Look
372	4C+74.26	310.7114	75.111	310.85824	74.929178	50.846162	74.615216	108.98584774	19.50187948	247.6342	55888.5409027778	2011-11-23 12:58:54	55890.613275463	2011-11-25 14:43:07	706028010	101.4125	100	101.4125	101.4125	0	101.4125	2	2	0	2	1	0	0	117.8827	117.8827	179.0297	2	PROCESSED	57603.9949074074	2016-08-03 23:52:40	56269	2012-12-08 00:00:00	55901.2441203704	2011-12-06 05:51:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060101	We propose the 120 ks observation of Broad Line Radio Galaxy 4C+74.26. The purpose is to estimate the angular momentum of the central super massive black hole from the broadness of Fe-K line. We study the spectral changes on spectra in details on the Fe-K lines and reflection hump in HXD-PIN band. We try to study the correlation between the radio intensity and black hole spins.	EXTRAGALACTIC COMPACT SOURCES	7	C	HIROFUMI NODA		JAP	6	AO6	STUSY OF BROAD IRON LINE OF 4C+74.26 TO ESTIMATE THE SPIN OF CENTRAL SUPER MASSIVE BLACK HOLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706028010/	Quick Look
373	1H0419-577	66.5116	-57.211	66.267931	-57.322556	29.331877	-75.671402	266.99901337	-41.98911345	55.5914	54306.2319328704	2007-07-25 05:33:59	54309.0835532407	2007-07-28 02:00:19	702041010	205.8628	200	205.8708	205.8708	0	205.8628	2	2	0	2	1	0	0	152.8317	152.8317	246.3578	2	PROCESSED	57539.3963888889	2016-05-31 09:30:48	54706	2008-08-28 00:00:00	54339.7211111111	2007-08-27 17:18:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021304	A hotly debated question is whether Seyfert X-ray spectra are dominated by components that are blurred by strong gravitational effects close (< 20rg) to the central black hole. Models featuring either complex absorption or blurred disk spectra provide equally good parameterizations of the mean X-ray spectrum of many objects. To make progress with current instruments we require observations with a temporal baseline and flux that will allow us to look for key parameter correlations, as the two scenarios predict different time-dependent behavior. To that end, we propose a Suzaku observation of 1H0419-577, a target that exhibits a remarkable degree of spectral variability in the X-ray regime promising some definitive results in this important area.	EXTRAGALACTIC COMPACT SOURCES	7	B	TRACEY TURNER		USA	2	AO2	HOW IMPORTANT IS STRONG RELATIVISTIC BLURRING IN SPECTRA OF SEYFERT GALAXIES?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702041010/	Quick Look
374	NGC5548	214.4931	25.1252	213.926181	25.355393	201.995661	36.403773	31.92399813	70.49805067	305.6592	54275.9121643518	2007-06-24 21:53:31	54276.6918055556	2007-06-25 16:36:12	702042020	35.9152	30	35.9152	35.9152	0	35.9152	2	2	0	2	1	0	0	33.175	33.175	67.3419	3	PROCESSED	57539.0421759259	2016-05-31 01:00:44	54695	2008-08-17 00:00:00	54322.4919675926	2007-08-10 11:48:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021307	We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	2	AO2	NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042020/	Quick Look
375	NGC7582	349.5634	-42.322	348.875032	-42.595557	331.740868	-34.366673	348.21143031	-65.69925686	64.738	54248.9237152778	2007-05-28 22:10:09	54249.7328587963	2007-05-29 17:35:19	702052020	28.769	25	28.769	28.769	0	28.769	2	2	0	2	1	0	0	24.6824	24.6824	69.9059	0	PROCESSED	57538.7538541667	2016-05-30 18:05:33	54695	2008-08-17 00:00:00	54255.6928472222	2007-06-04 16:37:42	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021332	We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARCO CHIABERGE		USA	2	AO2	MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052020/	Quick Look
376	4C+74.26	310.5668	75.0616	310.712656	74.880312	50.693329	74.661974	108.92036641	19.50581044	289.6922	54401.4314467593	2007-10-28 10:21:17	54403.2606944444	2007-10-30 06:15:24	702057010	91.583	100	91.583	91.583	0	91.591	2	2	0	2	1	0	0	94.114	94.114	158.0298	1	PROCESSED	57540.3825925926	2016-06-01 09:10:56	54776	2008-11-06 00:00:00	54409.2446064815	2007-11-05 05:52:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021354	We propose a 100 ks observation of the bright broad-line radio galaxy 4C+74.26. A previous 35 ks XMM-Newton observation of 4C+74.26 yielded the first indication of a relativistically broadened Fe K line in a radio-loud AGN as well as other typical AGN properties (e.g., a warm absorber). The long observation proposed here will allow a detailed investigation of the Fe K line profile and improve significantly on the previous observation by detecting the associated Compton reflection hump with the HXD/PIN instrument. Modeling of these features will allow the first accurate determination of the geometry and structure of the inner accretion disk in a radio-loud AGN, and hence provide invaluable information for modeling the physics of the disk/jet interaction.	EXTRAGALACTIC COMPACT SOURCES	7	C	DAVID BALLANTYNE		USA	2	AO2	A CLOSE LOOK AT 4C+74.26 WITH SUZAKU: FOCUSING IN ON THE DISK/JET INTERACTION	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702057010/	Quick Look
377	RBS 1124	187.6975	70.7093	187.160497	70.985277	134.358757	62.072206	125.39855918	46.31993489	339.073	54204.9538078704	2007-04-14 22:53:29	54206.5786921296	2007-04-16 13:53:19	702114010	86.2284	88	86.2284	86.2284	0	86.2284	2	2	0	2	1	0	0	88.8555	88.8555	140.384	3	PROCESSED	57538.4340740741	2016-05-30 10:25:04	54744	2008-10-05 00:00:00	54210.6501851852	2007-04-20 15:36:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022019	We propose a 70 ks observation of RBS 1124 (z=0.208). This is the X--ray brightest radio--quiet quasar (> 4e45 erg/s in the 2-10 keV band) from the ROSAT bright source catalogue. The expected number of counts (e.g. about 120,000 in just one FI XIS unit and about 11,000 in the HXD/PIN) will provide the best quality X-ray spectrum so far for such a high luminosity AGN. We will investigate the main X-ray spectral components shedding light on this extreme class of objects with unprecedented accuracy making full use of the Suzaku sensitivity across the whole band (XIS and HXD).	EXTRAGALACTIC COMPACT SOURCES	7	A	GIOVANNI MINIUTTI		EUR	2	AO2	REVEALING THE X-RAY EMISSION/ACCRETION PROCESSES IN THE VERY LUMINOUS RADIO-QUIET AND X-RAY BRIGHT QUASAR RBS 1124	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702114010/	Quick Look
378	3C 452	341.4131	39.7498	340.846907	39.486403	2.315539	43.172801	98.13461856	-16.98917572	65.3539	54267.3964351852	2007-06-16 09:30:52	54268.8294444444	2007-06-17 19:54:24	702073010	66.68	53	66.696	66.68	0	66.696	2	2	0	2	1	0	0	61.4487	61.4487	123.8018	3	PROCESSED	57538.9941550926	2016-05-30 23:51:35	54695	2008-08-17 00:00:00	54319.4923032407	2007-08-07 11:48:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021372	The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702073010/	Quick Look
379	MCG+8-11-11	88.7233	46.5039	87.789525	46.495439	89.047199	23.067702	165.67352488	10.43795472	91.6485	54360.0736342593	2007-09-17 01:46:02	54362.2640509259	2007-09-19 06:20:14	702112010	98.7481	100	98.7481	98.7561	0	98.7641	2	2	0	2	1	0	0	89.2138	89.2138	186.4387	1	PROCESSED	57540.0368055556	2016-06-01 00:53:00	54751	2008-10-12 00:00:00	54371.4963078704	2007-09-28 11:54:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022004	We propose to observe with Suzaku for 100 ks one of the X-ray brightest AGN, the Seyfert 1 galaxy MCG+8-11-11, with the aim to measure the fraction of the reflection component and the iron abundance. Suzaku provides a unique opportunity to perform this kind of analysis, thanks to its broadband coverage. Moreover, the proposed observation will provide an extremely good spectrum, which will allow us to measure the iron line width, its Compton Shoulder and the ionization stage of iron. These three measurements will contribute to provide useful information on the nature of the iron line emitting material, its distance from the central Black Hole and the mass of the latter.	EXTRAGALACTIC COMPACT SOURCES	7	B	STEFANO BIANCHI		EUR	2	AO2	MCG+8-11-11: A BROADBAND SPECTRUM OF ONE OF THE X-RAY BRIGHTEST AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702112010/	Quick Look
380	IC4329A	207.3319	-30.3116	206.617739	-30.063444	216.345797	-17.778855	317.49719871	30.9175719	295.4804	54323.458599537	2007-08-11 11:00:23	54324.2127777778	2007-08-12 05:06:24	702113030	26.8959	25	26.8959	26.8959	0	26.8959	2	2	0	2	1	0	0	23.8723	23.8723	65.1309	0	PROCESSED	57539.4615972222	2016-05-31 11:04:42	54730	2008-09-21 00:00:00	54347.7226041667	2007-09-04 17:20:33	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022009	IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASSIMO CAPPI		EUR	2	AO2	SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113030/	Quick Look
381	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
382	SWIFT J2127.4+5654	322.001	56.878	321.622917	56.659223	3.253872	64.455644	97.78160785	4.29621592	243.6186	54443.0645023148	2007-12-09 01:32:53	54445.0487962963	2007-12-11 01:10:16	702122010	91.7304	88	0	91.7304	0	91.7304	0	2	0	2	1	0	0	89.3485	89.3485	171.3799	2	PROCESSED	57540.867974537	2016-06-01 20:49:53	55000	2009-06-18 00:00:00	54633.7130439815	2008-06-16 17:06:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022034	We propose to observe with Suzaku two Narrow Line Seyfert 1 galaxies detected by SWIFT/BAT and INTEGRAL with a flux in excess of $10^{-11}$~erg~s$^{-1}$~cm$^{-2}$ in the HXD/PIN band for 70~ks each. These proposed observations provide rare high quality spectra of NLS1s above 10~keV. This will remove the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM--Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources (namely absorption, reflection, nature of the soft excess...).	EXTRAGALACTIC COMPACT SOURCES	7	C	GIOVANNI MINIUTTI		EUR	2	AO2	HUNTING HARD-X-RAY-BRIGHT NLS1 GALAXIES FROM THE INTEGRAL CATALOGUE WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702122010/	Quick Look
383	SWIFT J0911.2+4533	137.9062	45.5305	137.073312	45.735684	126.030873	27.898314	174.70874001	43.11152809	111.3983	54764.185787037	2008-10-25 04:27:32	54766.2105787037	2008-10-27 05:03:14	703008010	93.879	80	93.879	93.879	0	93.895	2	2	0	2	1	0	0	80.2256	80.2256	174.9298	4	PROCESSED	57544.2883564815	2016-06-05 06:55:14	55148	2009-11-13 00:00:00	54782.4040625	2008-11-12 09:41:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030034	The hard X-ray survey with Swift BAT have been finding various types of AGNs. Many buried AGNs with very low scattered X-rays have been discovered, for example. We propose to obtain broad band spectra of Compton-thin buried AGNs in the Swift sample. The data will be used to measure the amount of absoption in the direct and reflected emission and to constrain the structure of the obscuring matter around the AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	3	AO3	THE STRUCTURE OF BURIED COMPTON-THIN AGNS DISCOVERED BY SWIFT	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703008010/	Quick Look
384	MRK 110	141.3383	52.3497	140.469294	52.565715	125.649662	35.070751	164.91808924	44.3703784	110.1475	54406.3443055556	2007-11-02 08:15:48	54408.31625	2007-11-04 07:35:24	702124010	90.8712	100	90.8712	90.8792	0	90.8792	2	2	0	2	1	0	0	86.5231	86.5231	170.3558	2	PROCESSED	57540.442037037	2016-06-01 10:36:32	54786	2008-11-16 00:00:00	54417.3880092593	2007-11-13 09:18:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	023012	We request a 100 ks SUZAKU observation of Mrk 110 to quantify the accretion disk geometry in this high luminosity narrow line Seyfert 1 galaxy. This is an unique low mass AGN which shows an almost featureless X-ray continuum described by a two component Comptonization model. It has shown, based on an XMM-Newton data, energy dependent delays which are consistent with the idea of a Comptonized plasma confined within 10 Schwartzschild radius of the central black hole. The proposed long observation will provide high signal-to-noise hard X-ray data, thus allowing us to extend the observed delay to higher energies and also to quantify the high energy spectral parameters like cut-off energy and reflection parameters. This will help us to identify the accretion disk geometry in this source.	EXTRAGALACTIC COMPACT SOURCES	7	C	ARIKKALA RAO	Gulab Dewangan	EUS	2	AO2	PROBING THE ACCRETION DISK GEOMETRY IN THE TYPE I SEYFERT GALAXY MRK 110	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702124010/	Quick Look
385	Q0827+243	127.7159	24.1868	126.975524	24.355663	124.075193	5.096736	200.01721235	31.87611482	114.1438	54766.2156828704	2008-10-27 05:10:35	54767.3363310185	2008-10-28 08:04:19	703003010	48.2277	40	48.2277	48.2277	0	48.2277	2	2	0	2	1	0	0	39.3031	39.3031	96.8001	0	PROCESSED	57544.2665625	2016-06-05 06:23:51	54557	2008-04-01 00:00:00	54788.24125	2008-11-18 05:47:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030004	We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	3	AO3	REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703003010/	Quick Look
386	3C454.3	343.4943	16.1419	342.876691	15.875412	351.363443	21.32571	86.11034311	-38.19103065	250.8076	54792.3878703704	2008-11-22 09:18:32	54793.6884143518	2008-11-23 16:31:19	703006010	46.9239	40	46.9239	46.9239	0	46.9239	2	2	0	2	1	0	0	43.344	43.344	112.3139	2	PROCESSED	57544.5029976852	2016-06-05 12:04:19	54557	2008-04-01 00:00:00	54811.7229050926	2008-12-11 17:20:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030004	We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	3	AO3	REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703006010/	Quick Look
387	SWIFT J0959.5-2258	149.843	-22.8716	149.261565	-22.631568	161.273539	-32.730158	259.02796733	24.98206567	303.2834	54635.9091087963	2008-06-18 21:49:07	54636.8148611111	2008-06-19 19:33:24	703013010	43.6634	40	43.6714	43.6794	0	43.6634	2	2	0	2	1	0	0	42.4061	42.4061	78.2379	0	PROCESSED	57542.8554861111	2016-06-03 20:31:54	55016	2009-07-04 00:00:00	54650.0591782407	2008-07-03 01:25:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030045	Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	3	AO3	DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703013010/	Quick Look
388	SWIFT J0501.9-3239	79.8743	-32.7041	79.409754	-32.754183	74.820458	-55.614502	236.069923	-32.60257079	297.9191	54567.6584259259	2008-04-11 15:48:08	54568.8788194444	2008-04-12 21:05:30	703014010	41.2985	40	41.2985	41.2985	0	41.2985	2	2	0	2	1	0	0	36.4342	36.4342	105.4259	0	PROCESSED	57542.3107291667	2016-06-03 07:27:27	54953	2009-05-02 00:00:00	54580.5155208333	2008-04-24 12:22:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030045	Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	3	AO3	DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703014010/	Quick Look
389	SWIFT J0134.1-3625	23.4345	-36.4661	22.87514	-36.722141	4.413021	-42.266283	261.71382804	-77.05672525	34.1001	54606.6796180556	2008-05-20 16:18:39	54607.8390277778	2008-05-21 20:08:12	703016010	48.5116	40	48.5196	48.5116	0	48.5276	2	2	0	2	1	0	0	41.2927	41.2927	100.1498	0	PROCESSED	57542.6141898148	2016-06-03 14:44:26	54985	2009-06-03 00:00:00	54616.4068402778	2008-05-30 09:45:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030045	Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	3	AO3	DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703016010/	Quick Look
390	SWIFT J0444.1+2813	71.029	28.2793	70.24739	28.187015	73.273115	5.933796	172.68057795	-11.38105828	85.0234	54719.7173958333	2008-09-10 17:13:03	54721.6306944445	2008-09-12 15:08:12	703021010	81.2986	80	81.2986	81.2986	0	81.2986	2	2	0	2	1	0	0	67.7654	67.7654	165.3039	0	PROCESSED	57543.831087963	2016-06-04 19:56:46	55148	2009-11-13 00:00:00	54780.4776736111	2008-11-10 11:27:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030124	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	3	AO3	BROAD BAND SPECTRA OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703021010/	Quick Look
391	NGC3227	155.8766	19.8689	155.194036	20.122276	150.387342	9.143225	216.98457422	55.44588075	115.8562	54767.3422685185	2008-10-28 08:12:52	54768.8487731482	2008-10-29 20:22:14	703022010	58.9172	50	58.9172	58.9172	0	58.9172	2	2	0	2	1	0	0	52.0337	52.0337	130.1478	1	PROCESSED	57544.2886689815	2016-06-05 06:55:41	54557	2008-04-01 00:00:00	54788.4566203704	2008-11-18 10:57:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031013	We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	3	AO3	NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022010/	Quick Look
392	NGC3227	155.8768	19.8689	155.194236	20.122276	150.38752	9.143295	216.98468368	55.44605831	113.2489	54782.1173032407	2008-11-12 02:48:55	54783.7293865741	2008-11-13 17:30:19	703022030	56.5715	50	56.5772	56.5852	0	56.5715	2	2	0	2	1	0	0	50.2231	50.2231	139.2698	1	PROCESSED	57544.401724537	2016-06-05 09:38:29	54557	2008-04-01 00:00:00	54797.3603356482	2008-11-27 08:38:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031013	We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	3	AO3	NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022030/	Quick Look
393	NGC 4051	180.7984	44.5394	180.160059	44.817725	159.257872	40.347523	148.85547697	70.08163582	138.344	54776.3187847222	2008-11-06 07:39:03	54782.1112731482	2008-11-12 02:40:14	703023010	274.5305	340	274.5305	274.5305	0	274.5305	2	2	0	2	1	0	0	220.1993	220.1993	441.4488	3	PROCESSED	57544.5089930556	2016-06-05 12:12:57	54557	2008-04-01 00:00:00	54795.7746527778	2008-11-25 18:35:30	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031014	The powerful combination of Principal Components Analysis with time-resolved X-ray spectroscopy of Seyfert AGN has shown strong evidence that changes in a complex absorber are the origin of much of observed AGN spectral and flux variability. Large column, high ionization layers of gas may arise in a disk wind, representing a significant new, and possibly dominant, component, responsible for shaping the X-ray spectrum of AGN. The broad bandpass of Suzaku gives us a unique opportunity to model primary and reflected continua and the effects of variable absorbing zones, and test wind and other models. We propose a long 340 ks exposure on the NLSy1 NGC 4051 whose large amplitude of variability and well-studied complex absorption will test those models to the limit	EXTRAGALACTIC COMPACT SOURCES	7	A	TRACEY TURNER		USA	3	AO3	DECONSTRUCTING SEYFERT SPECTRA - TIME FOR A PARADIGM SHIFT?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703023010/	Quick Look
394	PDS 456	262.0806	-14.2617	261.369911	-14.221632	262.221213	8.965556	10.39448289	11.16711992	96.2509	56359.500150463	2013-03-08 12:00:13	56362.375162037	2013-03-11 09:00:14	707035030	108.3397	450	108.3477	108.3477	0	108.3397	2	2	0	2	1	0	0	94.226	94.226	248.3918	3	PROCESSED	57610.7991435185	2016-08-10 19:10:46	56018	2012-04-01 00:00:00	56373.5603125	2013-03-22 13:26:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071431	PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456.	EXTRAGALACTIC COMPACT SOURCES	7	B	JAMES REEVES		USA	7	AO7	VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707035030/	Quick Look
395	SN 2005KD	60.8552	71.7156	59.486745	71.577171	76.353108	49.655537	136.84988934	14.24754739	218.8053	54568.8904976852	2008-04-12 21:22:19	54570.0348842593	2008-04-14 00:50:14	703025010	51.6289	50	51.6289	51.6369	0	51.6449	1	1	0	1	1	0	0	63.5726	63.5726	98.8639	1	PROCESSED	57542.2950694444	2016-06-03 07:04:54	54947	2009-04-26 00:00:00	54581.1998842593	2008-04-25 04:47:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031241	Supernovae (SNe) 2005kd and 2006jd are some of the brightest SNe ever detected in X-rays. The high X-ray luminosities (>E41 erg/s) are the results of the SN shock interacting with dense material in the environment of the SNe. We propose one Suzaku observation of each SN to obtain high-quality spectra that will be used to measure the temperature of the forward and reverse shock and to establish the rate of decline in comparison with existing Swift, Chandra and XMM-Newton data. The data will further be used to measure the circumstellar matter density and mass-loss rate of the progenitors to probe the nature of the SN progenitors. Our science objectives rely on Suzaku's uniqueness, i.e. the large collecting area, good spectral resolution, and the high sensitivity in the hard X-ray band.	EXTRAGALACTIC COMPACT SOURCES	7	B	STEFAN IMMLER		USA	3	AO3	SUZAKU OBSERVATIONS OF X-RAY BRIGHT SUPERNOVAE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703025010/	Quick Look
396	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
397	MRK 348	12.1911	31.9636	11.514938	31.691174	24.328489	24.485278	122.27104531	-30.90471809	71.8836	54645.9325694444	2008-06-28 22:22:54	54648.0591203704	2008-07-01 01:25:08	703029010	87.4614	80	88.5334	87.4614	0	88.5334	2	2	0	2	1	0	0	78.5504	78.5504	183.7239	0	PROCESSED	57542.9708333333	2016-06-03 23:18:00	55031	2009-07-19 00:00:00	54664.7845601852	2008-07-17 18:49:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031322	X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s.	EXTRAGALACTIC COMPACT SOURCES	7	A	VALENTINA BRAITO		USA	3	AO3	THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703029010/	Quick Look
398	PKS 0326-288	52.1551	-28.6965	51.63485	-28.868348	39.555316	-45.73648	224.90475513	-55.39691379	250.3682	55226.8889699074	2010-01-30 21:20:07	55228.3266087963	2010-02-01 07:50:19	704039010	58.0237	60	58.0238	58.0237	0	58.0237	3	2	0	2	1	0	0	49.6247	49.6247	124.1859	3	PROCESSED	57550.4794560185	2016-06-11 11:30:25	55616	2011-02-24 00:00:00	55249.7586805556	2010-02-22 18:12:30	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041413	We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195~keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log($L_x$) $> 45.5$~ergs~sec$^{-1}$) absorbed tyoe II QSOs in the local universe and the most ripe for study with suzaku. 3C~332 is believed to be Compton-thick as suggested by chandra observations, and the newly discovered source SWIFT~J2344.6-4233 at a redshift of $z=0.6$ is the most luminous object in the BAT sample with log($L_x$) $=46.5$~ergs~sec$^{-1}$.	EXTRAGALACTIC COMPACT SOURCES	7	C	WAYNE BAUMGARTNER		USA	4	AO4	SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704039010/	Quick Look
399	3C 332	244.4239	32.3632	243.942335	32.484407	233.11322	52.57597	52.6372471	45.34839384	292.5008	55051.0341782407	2009-08-08 00:49:13	55052.4655092593	2009-08-09 11:10:20	704038010	59.8339	60	59.8339	59.8339	0	59.8339	2	2	0	2	1	0	0	46.0491	46.0491	123.652	0	PROCESSED	57548.1132407407	2016-06-09 02:43:04	55437	2010-08-29 00:00:00	55067.2557986111	2009-08-24 06:08:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041413	We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195~keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log($L_x$) $> 45.5$~ergs~sec$^{-1}$) absorbed tyoe II QSOs in the local universe and the most ripe for study with suzaku. 3C~332 is believed to be Compton-thick as suggested by chandra observations, and the newly discovered source SWIFT~J2344.6-4233 at a redshift of $z=0.6$ is the most luminous object in the BAT sample with log($L_x$) $=46.5$~ergs~sec$^{-1}$.	EXTRAGALACTIC COMPACT SOURCES	7	C	WAYNE BAUMGARTNER		USA	4	AO4	SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704038010/	Quick Look
400	Q0940-1050	145.7249	-11.0726	145.114895	-10.843374	152.028873	-23.330401	246.39011763	30.43738638	275.7617	54616.2125578704	2008-05-30 05:06:05	54617.1321064815	2008-05-31 03:10:14	703040010	32.3623	28	32.3623	32.3623	0	32.3623	2	2	0	2	1	0	0	26.7776	26.7776	79.4378	1	PROCESSED	57542.689212963	2016-06-03 16:32:28	54999	2009-06-17 00:00:00	54633.6981828704	2008-06-16 16:45:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031334	Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	3	AO3	A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703040010/	Quick Look
401	PKS 0528+134	82.7307	13.5905	82.023508	13.553568	82.834667	-9.669991	191.31463869	-10.98486414	89.0231	54736.1098611111	2008-09-27 02:38:12	54741.6752777778	2008-10-02 16:12:24	703048010	203.4574	200	203.4654	203.4654	0	203.4574	2	2	0	2	1	0	0	135.3629	135.3629	443.8619	4	PROCESSED	57544.2063888889	2016-06-05 04:57:12	55148	2009-11-13 00:00:00	54780.7843287037	2008-11-10 18:49:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031345	We propose a Suzaku observation of bright gamma-ray blazar PKS 0528+134, to be conducted jointly with GLAST, radio, and optical telescopes. This observation was accepted in the previous AO, but was not conducted due to GLAST launch delays. The goal is to obtain time-resolved broadband spectra. The X-ray and gamma-ray fluxes are known to be rapidly variable, but the information regarding the correlation between the X-ray and gamma-ray flux is limited. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles.	EXTRAGALACTIC COMPACT SOURCES	7	A	GRZEGORZ MADEJSKI		USA	3	AO3	SUZAKU AND GLAST OBSERVATIONS OF PKS 0528+134	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703048010/	Quick Look
402	3C120	68.298	5.3556	67.633455	5.25115	67.433074	-16.401934	190.3728125	-27.39468757	237.4583	53782.5602199074	2006-02-16 13:26:43	53783.5876967593	2006-02-17 14:06:17	700001020	41.5545	160	41.5545	41.5545	41.5545	41.5545	2	2	2	2	1	0	0	36.8461	36.8461	88.772	2	PROCESSED	57533.0172685185	2016-05-25 00:24:52	54247	2007-05-27 00:00:00	54041.2956365741	2006-11-02 07:05:43	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001003	Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	0	SWG	BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001020/	Quick Look
403	3C120	68.2979	5.3541	67.633361	5.249649	67.432732	-16.403401	190.37414386	-27.39561637	262.5053	53796.9456828704	2006-03-02 22:41:47	53797.8606365741	2006-03-03 20:39:19	700001040	40.9051	160	40.9131	40.9211	40.9211	40.9051	2	2	2	2	1	0	0	40.3118	40.3118	79.0459	0	PROCESSED	57533.1408912037	2016-05-25 03:22:53	54247	2007-05-27 00:00:00	54041.627025463	2006-11-02 15:02:55	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001003	Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	0	SWG	BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001040/	Quick Look
404	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
405	PKS1258-321	195.0396	-32.3625	194.354396	-32.09316	206.904154	-23.820406	305.06853624	30.47306853	293.0551	55027.0059259259	2009-07-15 00:08:32	55027.6050231482	2009-07-15 14:31:14	704007010	28.4607	20	28.4607	28.7327	0	28.7274	3	2	0	2	1	0	0	24.0275	24.0275	51.7559	0	PROCESSED	57547.8136921296	2016-06-08 19:31:43	55406	2010-07-29 00:00:00	55040.1188657407	2009-07-28 02:51:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040049	We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	4	AO4	SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704007010/	Quick Look
406	CENTAURUS_A	201.3281	-43.0649	200.594745	-42.804861	217.131954	-31.381221	309.48077241	19.37569293	303.3465	55057.3798148148	2009-08-14 09:06:56	55059.1051388889	2009-08-16 02:31:24	704018030	55.9442	50	55.9522	55.9442	0	55.9442	2	2	0	2	1	0	0	46.4915	46.4915	149.0478	3	PROCESSED	57548.1889699074	2016-06-09 04:32:07	55434	2010-08-26 00:00:00	55068.1674768518	2009-08-25 04:01:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040085	We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku.	EXTRAGALACTIC COMPACT SOURCES	7	A	YASUSHI FUKAZAWA		JAP	4	AO4	SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704018030/	Quick Look
407	EMS0992	230.2572	-3.8213	229.602576	-3.642087	228.859181	14.124861	358.15856297	42.46037658	113.2867	55593.7858564815	2011-02-01 18:51:38	55594.1841898148	2011-02-02 04:25:14	705026010	18.979	20	18.979	18.979	0	18.979	3	2	0	2	1	0	0	14.832	14.832	34.3939	0	PROCESSED	57600.8001388889	2016-07-31 19:12:12	55973	2012-02-16 00:00:00	55607.0454976852	2011-02-15 01:05:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050126	Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects.	EXTRAGALACTIC COMPACT SOURCES	7	C	YASUYUKI TANAKA		JAP	5	AO5	SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705026010/	Quick Look
408	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
409	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
410	MRK 352	14.9991	31.7575	14.31506	31.488197	26.597079	23.289939	125.05610732	-31.07894727	255.5628	55202.4718402778	2010-01-06 11:19:27	55203.6009143518	2010-01-07 14:25:19	704025010	45.6717	40	45.6877	45.6717	0	45.6872	2	2	0	2	1	0	0	22.3693	22.3693	97.5358	1	PROCESSED	57550.0955439815	2016-06-11 02:17:35	55602	2011-02-10 00:00:00	55235.27125	2010-02-08 06:30:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041402	The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples.	EXTRAGALACTIC COMPACT SOURCES	7	B	LISA WINTER		USA	4	AO4	SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704025010/	Quick Look
411	QSO 1828+487	277.4042	48.7379	277.077989	48.702797	285.744941	71.774201	77.22058509	23.48843965	218.1356	56983.2742592593	2014-11-22 06:34:56	56983.6771875	2014-11-22 16:15:09	709026010	14.1766	15	14.1766	14.1766	0	14.1766	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.8008912037	2016-08-16 19:13:17	57442	2016-02-24 00:00:00	57076.4104861111	2015-02-23 09:51:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092023		EXTRAGALACTIC COMPACT SOURCES	7	C	MARCUS LANGEJAHN		EUR	9	AO9	false	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709026010/	Quick Look
412	EMS1341	301.2467	70.0571	301.259152	69.912683	31.029252	78.090273	102.85714193	19.4440121	233.7732	55527.303275463	2010-11-27 07:16:43	55527.7619675926	2010-11-27 18:17:14	705027010	23.0668	20	23.0668	23.0668	0	23.0668	1	1	0	1	1	0	0	21.5055	21.5055	39.6239	0	PROCESSED	57554.2240856482	2016-06-15 05:22:41	55903	2011-12-08 00:00:00	55537.0214814815	2010-12-07 00:30:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050126	Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects.	EXTRAGALACTIC COMPACT SOURCES	7	C	YASUYUKI TANAKA		JAP	5	AO5	SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705027010/	Quick Look
413	SWIFT J0904.3+5538	136.117	55.5749	135.191467	55.77395	120.650833	36.933195	161.50516347	40.6960792	282.0039	54949.092025463	2009-04-28 02:12:31	54949.700162037	2009-04-28 16:48:14	704027010	41.9438	40	41.9438	41.9438	0	41.9438	1	1	0	1	1	0	0	35.8838	35.8838	52.5359	1	PROCESSED	57546.4424537037	2016-06-07 10:37:08	55343	2010-05-27 00:00:00	54973.440474537	2009-05-22 10:34:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041402	The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples.	EXTRAGALACTIC COMPACT SOURCES	7	B	LISA WINTER		USA	4	AO4	SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704027010/	Quick Look
414	UGC 6728	176.2197	79.6106	175.467594	79.888182	114.113262	63.856037	126.64092866	37.03371002	285.5693	54988.5646759259	2009-06-06 13:33:08	54989.5125925926	2009-06-07 12:18:08	704029010	49.0039	40	49.0039	49.0039	0	49.0039	2	2	0	2	1	0	0	41.5347	41.5347	81.8839	0	PROCESSED	57547.4998726852	2016-06-08 11:59:49	55364	2010-06-17 00:00:00	54998.3390740741	2009-06-16 08:08:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041402	The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples.	EXTRAGALACTIC COMPACT SOURCES	7	B	LISA WINTER		USA	4	AO4	SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704029010/	Quick Look
415	MCG-2-58-22	346.1839	-8.6878	345.532632	-8.95779	343.915361	-2.560866	64.09176202	-58.7610593	247.1128	55167.9420486111	2009-12-02 22:36:33	55170.9356365741	2009-12-05 22:27:19	704032010	138.9688	130	139.0088	138.9688	0	139.0088	2	2	0	2	1	0	0	105.4957	105.4957	258.6277	2	PROCESSED	57549.8017361111	2016-06-10 19:14:30	55553	2010-12-23 00:00:00	55187.5510763889	2009-12-22 13:13:33	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041404	We propose a 130 ks Suzaku long-look to study the Fe K emission complex of the Seyfert 1.5 AGN MCG--2-58-22, which has the unique combination of being X-ray bright, ``bare'' (i.e., lacking a strong ionized absorber), and possibly hosting both a truncated accretion disk and ionized circumnuclear material. We aim to accurately constrain the geometry and ionization state of the accreting circumnuclear material of this likely low-Compton reflection source by resolving the Fe K alpha line and constraining its origin, which may likely be a truncated thin disk, and verifying a previous claim of emission from H-like Fe. We will also determine the origin of this object's soft excess.	EXTRAGALACTIC COMPACT SOURCES	7	B	ALEX MARKOWITZ		USA	4	AO4	A SUZAKU OBSERVATION OF MCG--2-58-22: A TRUNCATED OR IONIZED ACCRETION DISK?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704032010/	Quick Look
416	MRK1018	31.5471	-0.2351	30.907355	-0.473179	29.3057	-12.234469	159.73232745	-57.66458833	73.6945	55015.0121759259	2009-07-03 00:17:32	55016.0939699074	2009-07-04 02:15:19	704044010	43.9014	40	43.9094	43.9014	0	43.9094	2	2	0	2	1	0	0	37.6884	37.6884	93.4578	5	PROCESSED	57547.7689467593	2016-06-08 18:27:17	55395	2010-07-18 00:00:00	55027.1070023148	2009-07-15 02:34:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041414	We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc.	EXTRAGALACTIC COMPACT SOURCES	7	A	EZEQUIEL TREISTER		USA	4	AO4	THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704044010/	Quick Look
417	NGC 3718	173.2341	53.1118	172.54734	53.387989	147.276263	44.880657	146.87581124	60.21394242	142.7392	55128.8497800926	2009-10-24 20:23:41	55130.255775463	2009-10-26 06:08:19	704048010	59.8882	60	59.9202	59.8882	0	59.9202	2	2	0	2	1	0	0	52.4392	52.4392	121.4599	0	PROCESSED	57548.9845138889	2016-06-09 23:37:42	55507	2010-11-07 00:00:00	55141.3212384259	2009-11-06 07:42:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041415	The SWIFT BAT hard (14-195 KeV) survey is performing the first unbiased hard X-ray survey of the entire sky with follow-up observations with the Swift XRT to fully identify the sample. In this survey we have found two very low luminosity nearby hard X-ray sources which show little, if any, evidence for nuclear activity in the optical or UV band, and have very low apparent Eddington ratios. We propose Suzaku observations of these objects to determine whether there is an X-ray spectral signature of a low Eddington ratio, as predicted if these objects are indeed in a radiatively inefficient accretion flow.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	4	AO4	SUZAKU OBSERVATIONS OF NGC4138 AND NGC3718	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704048010/	Quick Look
418	NGC 3997	179.448	25.2646	178.805338	25.542926	168.8766	22.834867	218.72362191	77.82883353	305.585	56439.4793981482	2013-05-27 11:30:20	56441.452974537	2013-05-29 10:52:17	708002010	87.1383	80	87.1383	87.1383	0	87.1383	2	2	0	2	1	0	0	83.0504	83.0504	170.508	2	PROCESSED	57611.4399305556	2016-08-11 10:33:30	56816	2014-06-08 00:00:00	56450.866724537	2013-06-07 20:48:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080015	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	8	AO8	BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708002010/	Quick Look
419	NGC 1365	53.3909	-36.1409	52.913513	-36.307906	36.789839	-53.036651	237.95774893	-54.60665436	30.5416	55374.0284143518	2010-06-27 00:40:55	55377.9834606482	2010-06-30 23:36:11	705031010	151.6134	450	151.6294	151.6134	0	151.6214	2	2	0	2	1	0	0	123.2422	123.2422	341.6577	2	PROCESSED	57552.5171064815	2016-06-13 12:24:38	55287	2010-04-01 00:00:00	55434.2469444445	2010-08-26 05:55:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051112	We propose 3 observations (~4 days each) of the Seyfert galaxy NGC 1365, at 2-week intervals. We aim to use eclipses to unambiguously identify the broad Fe K line, examine variability of the HXD/PIN excess, and to search for changes in the physical properties of the ionized absorber in this bright, nearby AGN. Shorter observations of this galaxy with XMM-Newton, Chandra and Suzaku showcase several remarkable physical traits: (1) FeXXV and FeXXVI K-shell absorption lines (the highest s/n detection so far among AGN), (2) rapidly varying cold absorption, (3) a highly significant relativistic Fe K emission line, and (4) a factor ~4 excess flux at high energies. The proposed observations will provide legacy spectra for what is arguably the single most physically-revealing obscured AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	LAURA BRENNEMAN		USA	5	AO5	A LONG LOOK AT NGC 1365: DISC TOMOGRAPHY, IONIZED ABSORPTION AND HIGH ENERGY EXCESS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705031010/	Quick Look
420	NGC 6251	248.2903	82.5391	249.646931	82.638978	99.623854	73.274498	115.75265542	31.17774629	182.5432	55532.2390625	2010-12-02 05:44:15	55534.0341898148	2010-12-04 00:49:14	705039010	87.0706	85	87.0706	87.0706	0	87.0706	2	2	0	2	1	0	0	75.8074	75.8074	155.0879	1	PROCESSED	57554.3327546296	2016-06-15 07:59:10	55931	2012-01-05 00:00:00	55565.375162037	2011-01-04 09:00:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051411	We propose an 85-ks Suzaku observation of NGC 6251, the brightest example of a low-excitation radio galaxy (LERG). We have previously suggested that LERGs violate conventional AGN unification schemes: they may lack an obscuring torus and are likely to accrete in a radiatively inefficient manner, with almost all of the energy released by the accretion process being channeled into powerful jets. However, Suzaku observations at low and high energies are needed to test this model directly. We will use the XIS and HXD to search for the signatures of accretion-related X-ray emission: (1) the 6.4 keV Fe Ka line, (2) heavily absorbed X-ray emission, and (3) the >10 keV Compton reflection bump. These results will have important implications for models of accretion and feedback in radio-loud AGN.	EXTRAGALACTIC COMPACT SOURCES	7	C	DANIEL EVANS		USA	5	AO5	A DIRECT TEST OF THE NUCLEAR X-RAY DICHOTOMY IN RADIO-LOUD AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705039010/	Quick Look
421	PDS 456	262.0809	-14.2537	261.370252	-14.213634	262.221057	8.97356	10.4015562	11.17111116	96.1694	55636.625462963	2011-03-16 15:00:40	55639.3564930556	2011-03-19 08:33:21	705041010	125.5272	130	125.5352	125.5272	0	125.5327	2	2	0	2	1	0	0	100.875	100.875	235.9276	2	PROCESSED	57601.2862615741	2016-08-01 06:52:13	56050	2012-05-03 00:00:00	55677.3183564815	2011-04-26 07:38:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051421	PDS 456 is the most luminous nearby AGN and a recent Suzaku observation revealed a powerful ionized outflow moving at 0.25c with kinetic output matching the quasar bolometric luminosity. Above 10 keV the HXD appears to show a factor 3 rise in flux over the XIS, implying that a high column density absorber (>10^24 cm^-2) is located close to the X-ray source in order to partially covers its emission. We propose to study the remarkable X-ray absorption towards PDS 456 through two further 130 ks Suzaku observations. This will:-i) confirm the nature of the hard excess, ii) determine whether spectral variability can be explained by variable partial covering and iii) enable us to measure the imprint of the ionized outflow at Fe K with unprecedented accuracy.	EXTRAGALACTIC COMPACT SOURCES	7	B	TRACEY TURNER		USA	5	AO5	THE COMPTON-THICK OUTFLOW IN THE TYPE I QSO PDS 456	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705041010/	Quick Look
422	SPT-CLJ2344-4243	356.1816	-42.7169	355.522212	-42.994645	336.755816	-37.082735	339.63806237	-69.34299043	226.1467	56605.0105902778	2013-11-09 00:15:15	56607.4106597222	2013-11-11 09:51:21	708012010	86.2043	80	86.2043	86.2043	0	86.2043	2	2	0	2	1	0	0	80.0289	80.0289	207.3477	3	PROCESSED	57613.3115625	2016-08-13 07:28:39	56383	2013-04-01 00:00:00	56653.7570949074	2013-12-27 18:10:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080071	SPT-CLJ2344-4243 is a distant (z=0.596) extremely luminous (Lx=8x10^45erg/s) cluster with a strong cooling flow rate of 3820 Msun/year. The central galaxy of the cluster shows huge star formation activity and has a luminous (Lx=3x10^45 erg/s) AGN. According to the paper by McDonald et al. (2012) and Fe I detection by our analysis of the archived data of Suzaku, this AGN is likely to be a type 2 QSO, for which we don ft know any other example situated at the center of a cluster. We are observing a special phase of co-evolution of a cluster, its central galaxy, and SMBH at its center. We propose to perform 80ks x 4 times observations with Suzaku to estimate SMBH mass in this system through X-ray variability and to get Fe I line detection with higher confidence.	EXTRAGALACTIC COMPACT SOURCES	7	C	SHUTARO UEDA		JAP	8	AO8	CO-EVOLUTION IN SMBH, GALAXY AND CLUSTERS; SUZAKU OBSERVATION OF A TYPE 2 QSO AT THE CENTER OF SPT-CLJ2344-4243	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708012010/	Quick Look
423	MKN 590	33.6446	-0.7698	33.006332	-1.002435	31.137585	-13.457637	163.50990373	-56.94179664	250.4206	55584.0937615741	2011-01-23 02:15:01	55585.6252083333	2011-01-24 15:00:18	705043010	61.5547	150	61.5867	61.5547	0	61.5707	2	2	0	2	1	0	0	55.1599	55.1599	132.2758	0	PROCESSED	57600.7325	2016-07-31 17:34:48	55965	2012-02-08 00:00:00	55599.1867824074	2011-02-07 04:28:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051433	We propose a 150 ks Suzaku long-look to study the Compton reflection component, soft excess, ionized emission and possible ionized reflection of the Seyfert 1.2 AGN Mkn 590, which has an unobscured line of sight or "bare nucleus" and as of yet unquantified reflection. We aim to accurately constrain the geometry of the circumnuclear material and determine the ionization states of both the Compton-thin and Compton-thick material surrounding the black hole by studying the origin of the soft excess, determining the likelihood of ionized reflection and accurately measuring the intensity of neutral, H-like and He-like Fe emission lines.	EXTRAGALACTIC COMPACT SOURCES	7	C	ELIZABETH RIVERS		USA	5	AO5	QUANTIFYING THE COMPTON REFLECTION AND IONIZED EMISSION IN MKN 590	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705043010/	Quick Look
424	NGC 2992	146.4352	-14.2714	145.83373	-14.040218	154.019094	-26.058459	249.66741784	28.82528499	102.6298	53680.5956481482	2005-11-06 14:17:44	53681.5850925926	2005-11-07 14:02:32	700005010	37.5029	120	37.5029	38.7568	37.518	37.715	2	2	2	2	1	0	0	32.073	32.073	85.4859	1	PROCESSED	57527.9475231482	2016-05-19 22:44:26	54247	2007-05-27 00:00:00	54037.5593518518	2006-10-29 13:25:28	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001013	NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	0	SWG	THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005010/	Quick Look
425	NGC 4945	196.3459	-49.5284	195.615808	-49.260687	217.044106	-38.699389	305.256234	13.28040137	283.285	55381.636087963	2010-07-04 15:15:58	55382.6765856482	2010-07-05 16:14:17	705047010	39.0737	40	39.0817	39.0817	0	39.0737	1	1	0	1	1	0	0	34.0751	34.0751	89.8719	1	PROCESSED	57552.4706481482	2016-06-13 11:17:44	55770	2011-07-28 00:00:00	55404.2681134259	2010-07-27 06:26:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051442	We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval.	EXTRAGALACTIC COMPACT SOURCES	7	B	GUIDO RISALITI		USA	5	AO5	HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047010/	Quick Look
426	NGC 4945	196.3265	-49.5207	195.596537	-49.252961	217.025208	-38.698833	305.24375345	13.28878787	296.6587	55403.0670717593	2010-07-26 01:36:35	55404.1745717593	2010-07-27 04:11:23	705047030	40.3266	40	40.3426	40.3266	0	40.3426	2	2	0	2	1	0	0	34.6182	34.6182	95.6358	0	PROCESSED	57552.7156134259	2016-06-13 17:10:29	55780	2011-08-07 00:00:00	55414.0832407407	2010-08-06 01:59:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051442	We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval.	EXTRAGALACTIC COMPACT SOURCES	7	B	GUIDO RISALITI		USA	5	AO5	HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047030/	Quick Look
427	3C78	47.1071	4.1138	46.452233	3.923143	45.835066	-12.996467	174.85308943	-44.51284685	84.4195	55793.5846990741	2011-08-20 14:01:58	55795.7502430556	2011-08-22 18:00:21	706013010	97.0122	100	97.0122	97.0122	0	97.0122	3	2	0	2	1	0	0	85.9075	85.9075	187.0878	0	PROCESSED	57602.928275463	2016-08-02 22:16:43	56176	2012-09-06 00:00:00	55806.3891435185	2011-09-02 09:20:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060046	We propose to observe two radio galaxies 3C78 and PKS0625-354 which were detected by the Fermi gamma-ray satellte survey during the 1st year, in order to investigate the X-ray emission more precisely than ever. In the case of jet emission, we can constrain the jet parameter well from the multi-wavelength spectrum and obtain the jet kinetic energy. In the case of disk emission, we can obtain the jet to disk energy ratio. This observation will enable us to obtain the jet parameters of these galaxies and compare them with others.	EXTRAGALACTIC COMPACT SOURCES	7	B	YASUSHI FUKAZAWA		JAP	6	AO6	ORIGIN OF THE X-RAY EMISSION OF GAMAM-RAY RADIO GALAXIES 3C78 AND PKS0625-354	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706013010/	Quick Look
428	NGC6251_LOBE_BGD1	247.6537	82.9256	249.113456	83.028127	99.179697	72.901441	116.18672095	31.0445068	26.9624	55667.0269328704	2011-04-16 00:38:47	55667.4328125	2011-04-16 10:23:15	706004010	18.822	20	18.8357	18.822	0	18.8356	3	2	0	2	1	0	0	18.9572	18.9572	35.0659	1	PROCESSED	57601.5125694445	2016-08-01 12:18:06	56058	2012-05-11 00:00:00	55691.0888194444	2011-05-10 02:07:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060004	We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	6	AO6	SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706004010/	Quick Look
429	HESS J1943+213	295.9916	21.301	295.448325	21.18018	303.194	41.793482	57.76229591	-1.30331963	246.7107	55875.6293055556	2011-11-10 15:06:12	55876.6015393518	2011-11-11 14:26:13	706007010	38.8815	40	38.8815	38.8895	0	38.8895	2	2	0	2	1	0	0	35.313	35.313	83.972	1	PROCESSED	57603.7570601852	2016-08-03 18:10:10	56256	2012-11-25 00:00:00	55890.6970833333	2011-11-25 16:43:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060028	A new point-like source HESS J1943+213 has been detected at TeV energies at the position coinciding with the unidentified hard X-ray objects IGR J19443+2117. All the available observational constraints favor an identification of HESS J1943+213 as a BL Lac at redshift z>0.14. If correct, this would be the first time an AGN is discovered serendipitously from TeV observations in the Galactic Plane. It would be also the most extreme BL Lac known, with the persistent synchrotron continuum extending up to the observed energies >100 keV. A good quality broad X-ray spectrum is needed to confirm the blazar association and the extreme character of the peculiar object HESS J1943+213. Here we argue that a relatively moderate Suzaku exposure of 40 ksec will enable us to obtain such a spectrum.	EXTRAGALACTIC COMPACT SOURCES	7	C	LUKASZ STAWARZ		JAP	6	AO6	PECULIAR UNIDENTIFIED TEV SOURCE HESS J1943+213 IN THE GALACTIC PLANE: EXTREME BLAZAR OR SOMETHING ELSE?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706007010/	Quick Look
430	SWIFT J1310.9-5553	197.6868	-55.8722	196.924529	-55.606324	222.251055	-43.758692	305.6577855	6.89731776	290.4478	55761.4489467593	2011-07-19 10:46:29	55762.6432523148	2011-07-20 15:26:17	706009010	82.785	80	82.793	82.785	0	82.785	2	2	0	2	1	0	0	67.5081	67.5081	103.1779	1	PROCESSED	57602.6323263889	2016-08-02 15:10:33	56213	2012-10-13 00:00:00	55845.247662037	2011-10-11 05:56:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060030	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	6	AO6	BROAD BAND SPECTRA OF HARD X-RAY SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706009010/	Quick Look
431	3C 98	59.723	10.4395	59.038566	10.297703	59.781896	-9.882185	179.82925767	-31.05249617	81.003	55812.5811342593	2011-09-08 13:56:50	55815.280787037	2011-09-11 06:44:20	706015010	101.144	100	101.144	101.144	0	101.144	2	2	0	2	1	0	0	89.8389	89.8389	233.214	3	PROCESSED	57603.1723611111	2016-08-03 04:08:12	56218	2012-10-18 00:00:00	55851.4528356482	2011-10-17 10:52:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060055	Whether radio-loud and radio-quiet AGN may be unified under one model is still open to debate. The most important limitation in such work is that jet beaming swamps nuclear emission, so we must study powerful radio sources which are not affected by this bias. These are the Narrow Line Radio Galaxies (NLRGs). Heavy obscuration means that their primary emission is visible only above 10 keV. 3C 98 is an important member of the NLRG class because its hard band power dominates the full radio to X-ray core luminosity. We propose a 100 ks observation of this source with Suzaku to detect the core continuum emission and reflection above 10 keV. 3C~98 is one of few NLRGs for which we can expect to model (rather than just detect) the hard X-ray flux, and hence use it for testing unification schemes.	EXTRAGALACTIC COMPACT SOURCES	7	B	POSHAK GANDHI		JAP	6	AO6	HARD X-RAY EMISSION AND REFLECTION IN RADIO GALAXIES: 3C 98	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706015010/	Quick Look
432	1FGL J0103.1+4840	15.7305	48.657	15.006375	48.388615	36.058904	38.14189	124.88749892	-14.17113818	69.2705	55753.0127430556	2011-07-11 00:18:21	55755.0002199074	2011-07-13 00:00:19	706025010	84.3622	80	84.3622	84.3622	0	84.3622	2	2	0	2	1	0	0	79.727	79.727	171.6957	2	PROCESSED	57602.5903935185	2016-08-02 14:10:10	56148	2012-08-09 00:00:00	55778.4339814815	2011-08-05 10:24:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060084	In this proposal, we'd like to make a suggestion of 2 "steady" unassociated Fermi-LAT gamma-ray sources with Suzaku. 2-year Fermi-LAT observation detected 2412 sources, but 1194 sources are still unassociated. Proposed objects are located at high Galactic latitude, and selected not likely to be associated with blazar(AGN) and pulsar. These lightcurves do not show the significant temporal variability. To confirm their stability, we checked Test Statistic Value of 1FGL and 2-year Fermi observation. Deep Observation with Suzaku (1FGLJ0103: 80ks, 1FGL1946:40ks) is expected to reveal the nature of these unassociated objects, or at least impose strict limits at 2-10keV. Of course, it is necessary that multi-wavelength observation. We'll plan to arrange tie-ups with other wavelength researcher.	EXTRAGALACTIC COMPACT SOURCES	7	B	KOTO MAEDA		JAP	6	AO6	SUZAKU OBSERVATION OF "STEADY" UNASSOCIATED FERMI-LAT GAMMA-RAY SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706025010/	Quick Look
433	RX J1633+4718	248.3647	47.3332	248.004849	47.436616	228.791999	67.699433	73.56993988	42.60070523	133.9355	55962.6778240741	2012-02-05 16:16:04	55963.7502430556	2012-02-06 18:00:21	706027040	45.4834	40	45.4834	45.4834	0	45.4834	2	2	0	2	1	0	0	40.3113	40.3113	92.6459	0	PROCESSED	57604.5712152778	2016-08-04 13:42:33	56345	2013-02-22 00:00:00	55978.5479282407	2012-02-21 13:09:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060089	RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time.	EXTRAGALACTIC COMPACT SOURCES	7	A	KIYOSHI HAYASHIDA		JAP	6	AO6	X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027040/	Quick Look
434	SMC X-1	19.2772	-73.44	18.945719	-73.703155	312.351206	-66.472298	300.41207357	-43.56242986	167.9636	55825.1720949074	2011-09-21 04:07:49	55825.6536805556	2011-09-21 15:41:18	706030070	18.1239	18	18.2772	18.2852	0	18.1239	2	2	0	1	1	0	0	18.3687	18.3687	41.5959	0	PROCESSED	57603.2202662037	2016-08-03 05:17:11	56218	2012-10-18 00:00:00	55851.4509027778	2011-10-17 10:49:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030070/	Quick Look
435	SMC X-1	19.2766	-73.4376	18.945062	-73.700756	312.356716	-66.471322	300.41185267	-43.56483062	244.987	55907.8985069444	2011-12-12 21:33:51	55908.2709722222	2011-12-13 06:30:12	706030090	17.3055	18	17.4079	17.4079	0	17.3055	1	1	0	1	1	0	0	18.413	18.413	32.1719	0	PROCESSED	57604.1197685185	2016-08-04 02:52:28	56289	2012-12-28 00:00:00	55920.9743981482	2011-12-25 23:23:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030090/	Quick Look
436	H1821+643	275.4676	64.3592	275.403785	64.332814	318.33431	86.843842	94.01912066	27.4276768	65.0012	56398.4117013889	2013-04-16 09:52:51	56402.5419328704	2013-04-20 13:00:23	708037010	246.5839	400	246.5839	246.5919	0	246.5999	2	2	0	2	1	0	0	251.0273	251.0273	356.8299	0	PROCESSED	57611.1526273148	2016-08-11 03:39:47	56383	2013-04-01 00:00:00	56425.7059606482	2013-05-13 16:56:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081436	H1821+643 (z=0.297) is not "just another quasar". This luminous active galactic nucleus (AGN) is an extremely rare example of a powerful quasar at the center of a rich, cooling-core cluster of galaxies. As such, it may represent a key evolutionary stage in the complex interplay between AGN and the core regions of the intracluster medium (ICM). Our analysis of archival XMM-Newton data has found evidence for a relativistically broad iron line. Here, we build on this request deep (400ks) Suzaku spectroscopy of H1821+643 to (1) measure the spin of this supermassive black hole and (2) search for powerful highly ionized outflows. In addition to measuring spin in the most luminous and distant object yet, this will enable us to test key predictions of recent models for AGN feedback.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	8	AO8	THE BLACK HOLE SPIN AND IONIZED OUTFLOWS IN THE COOLING-FLOW QUASAR H1821+643	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708037010/	Quick Look
437	NGC 4593	189.9132	-5.341	189.26831	-5.066485	191.201043	-0.986248	297.48043001	57.40595243	111.8998	57021.7640856482	2014-12-30 18:20:17	57025.333287037	2015-01-03 07:59:56	709014050	145.2819	30	145.2819	145.3032	0	145.2899	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.5760069445	2016-08-17 13:49:27	57415	2016-01-28 00:00:00	57049.4542939815	2015-01-27 10:54:11	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090097	In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	9	AO9	X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014050/	Quick Look
438	NGC 1566	65.0038	-54.9403	64.723209	-55.058612	32.065014	-73.361775	264.31301386	-43.39149342	351.3031	56066.0671759259	2012-05-19 01:36:44	56067.2738310185	2012-05-20 06:34:19	707002010	72.791	80	72.791	72.791	0	72.791	2	2	0	2	1	0	0	71.9581	71.9581	104.2239	2	PROCESSED	57605.4671875	2016-08-05 11:12:45	56442	2013-05-30 00:00:00	56076.0434606482	2012-05-29 01:02:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070003	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with intermediate to high luminosities. Here we propose to observe two of the lowest luminosity AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	7	AO7	BROAD BAND SPECTRA OF HARD X-RAY SELECTED LOW LUMINOSITY AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707002010/	Quick Look
439	ARK 120	79.0439	-0.2064	78.404432	-0.260846	78.068932	-23.195412	201.74563913	-21.16237248	274.9546	54191.755162037	2007-04-01 18:07:26	54193.905150463	2007-04-03 21:43:25	702014010	100.8635	100	100.8635	100.8635	0	100.8635	2	2	0	2	1	0	0	95.3121	95.3121	185.7439	1	PROCESSED	57538.0955324074	2016-05-30 02:17:34	54744	2008-10-05 00:00:00	54200.5657060185	2007-04-10 13:34:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020035	We propose to obtain the broad-band spectra of the bright Seyfert 1 Ark 120 with Suzaku. Since Ark 120 shows no strong absorption features in its X-ray spectrum, we can cleanly measure the shape of the continuum and Fe K line without introducing any ambiguity caused by absorption along the line of sight. The spectrum will be used to test the diskline hypothesis in Seyferts and to study the fundamental processes producing broad band spectra of AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	2	AO2	THE ORIGIN OF THE BROAD FE LINE IN THE SEYFERT 1 ARK 120	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702014010/	Quick Look
440	ESO 511-G030	214.8452	-26.6475	214.125784	-26.417987	221.40413	-12.023995	326.22882256	32.21510552	286.6511	56128.5082523148	2012-07-20 12:11:53	56128.7501388889	2012-07-20 18:00:12	707023010	5.7461	270	5.7461	5.7541	0	5.7621	1	1	0	1	1	0	0	3.9886	3.9886	20.8879	0	PROCESSED	57606.6388194444	2016-08-06 15:19:54	56646	2013-12-20 00:00:00	56214.9581944445	2012-10-14 22:59:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071413	The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		USA	7	AO7	MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707023010/	Quick Look
441	PG 1404+226	211.5943	22.4043	211.013582	22.642135	200.388612	32.841534	21.50519934	72.36517417	124.2434	56284.2179398148	2012-12-23 05:13:50	56286.1272453704	2012-12-25 03:03:14	707026010	80.2969	80	80.3129	80.2969	0	80.3049	2	2	0	2	1	0	0	70.5848	70.5848	164.9457	1	PROCESSED	57608.3815972222	2016-08-08 09:09:30	56687	2014-01-30 00:00:00	56320.7751157407	2013-01-28 18:36:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071419	We propose a 80 ks observation of a NLS galaxy, PG1404+226, with Suzaku/XIS to investigate the physical conditions of extreme absorbers known as the ultra-fast-outflows (UFOs; v/c~0.1-0.2) of variable resonant absorption features from many ions (e.g. Ne IX, Ne X, Mg XII and S XVI) in the soft X-ray band (~0.5-3.5 keV), and we propose the first Suzaku observation of this object to (i) independently confirm/refute the previous claims of the presence of these UFOs including a potential detection of Fe K-shell absorbers, (ii) examine their variabilities and compare the outflow properties at low and high XIS-flux states, (iii) compare its outflow rate and kinetic power with those in other AGN UFOs, and (iv) utilize a high-quality Suzaku data to improve our MHD disk-wind model.	EXTRAGALACTIC COMPACT SOURCES	7	C	KEIGO FUKUMURA		USA	7	AO7	PROBING THE ULTRA-FAST-OUTFLOWS OF PG1404+226 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707026010/	Quick Look
442	NGC 3516	166.6912	72.5534	165.838584	72.823761	123.385975	57.972253	133.24889589	42.41461595	284.0065	56441.4603009259	2013-05-29 11:02:50	56442.6355787037	2013-05-30 15:15:14	708006040	54.218	50	54.218	54.218	0	54.218	2	2	0	2	1	0	0	53.1207	53.1207	101.54	1	PROCESSED	57615.5831134259	2016-08-15 13:59:41	56383	2013-04-01 00:00:00	56503.6575347222	2013-07-30 15:46:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080066	We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	8	AO8	THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006040/	Quick Look
443	SBS 1301+540	196.0153	53.8063	195.478385	54.074176	163.182611	53.62856	118.79430047	63.22042238	133.9261	56991.9979976852	2014-11-30 23:57:07	56994.5141435185	2014-12-03 12:20:22	709018010	94.3176	100	94.3176	95.1576	0	95.1736	2	2	0	2	1	0	0	105.4641	105.4641	217.3498	5	PROCESSED	57617.4634143518	2016-08-17 11:07:19	57451	2016-03-04 00:00:00	57084.1361574074	2015-03-03 03:16:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091411	We propose to carry out Suzaku observations, 100 ks each, of two Seyfert I nuclei, IGR J16558-5203 and SBS 1301+540, hard X-ray selected by Swift. Our goal is to distinguish between various competing models proposed for the X-ray spectra of Seyfert I nuclei. Specifically we will explore the effects of strong gravity, by testing the ionized relativistic reflection (hereafter IRR) and by measuring the spin of the black hole. We will take advantage of Suzaku s excellent capability in the broad bands from the soft through medium to hard X-ray bands. With our proposed studies we will gain deeper understanding of accretion-powered AGN in general.	EXTRAGALACTIC COMPACT SOURCES	7	C	SACHIKO TSURUTA		USA	9	AO9	SPECTRAL STUDIES OF SOME HARD X RAY SELECTED SEYFERT NUCLEI	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709018010/	Quick Look
444	IRAS 05078+1626	77.6911	16.4922	76.970259	16.431142	78.130409	-6.443089	186.12002752	-13.50176431	259.3263	56351.6301736111	2013-02-28 15:07:27	56352.6112847222	2013-03-01 14:40:15	707029010	46.0167	45	46.0167	46.0167	0	46.0167	2	2	0	2	1	0	0	44.1101	44.1101	84.7558	1	PROCESSED	57610.7197916667	2016-08-10 17:16:30	56749	2014-04-02 00:00:00	56372.578287037	2013-03-21 13:52:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071424	A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN.	EXTRAGALACTIC COMPACT SOURCES	7	C	TRACEY TURNER		USA	7	AO7	INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707029010/	Quick Look
445	MCG-5-23-16	146.9228	-30.9448	146.373555	-30.712217	162.622685	-41.142645	262.74496877	17.23993252	295.4404	56448.2467476852	2013-06-05 05:55:19	56450.9584606482	2013-06-07 23:00:11	708021020	138.8466	300	138.8466	138.8466	0	138.8466	2	2	0	2	1	0	0	140.4914	140.4914	234.282	2	PROCESSED	57611.5159490741	2016-08-11 12:22:58	56383	2013-04-01 00:00:00	56461.7776736111	2013-06-18 18:39:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081416	Significant recent developments in probing environments around AGN black holes has been achieved using X-ray reverberation. They were initially detected in the soft excess of several NLS1s, then recently, the first Fe K reverberation was also seen. In addition to measuring x-rays reverberating a few r_g from the event horizon, short/long delays from different radii have been separated for the first time in NGC4151. Here we propose to observe MCG-5-23-1 for 300 ks in order to study its iron K reverberation. It is optimally one of the brightest and most variable AGN in X-rays. Archival data already show very exciting signatures of Fe K reverberation. With new observations we aim to constrain the emitting region size and study the emission originating at different distances from of the hole.	EXTRAGALACTIC COMPACT SOURCES	7	A	ABDERAHMEN ZOGHBI		USA	8	AO8	IRON K REVERBERATION IN MCG 5-23-16	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708021020/	Quick Look
446	MKN 915	339.1982	-12.5468	338.534901	-12.806507	336.087416	-3.520949	51.05925373	-55.2984956	243.0396	56622.9636458333	2013-11-26 23:07:39	56624.1320601852	2013-11-28 03:10:10	708029010	41.22	40	41.22	41.22	0	41.22	2	2	0	2	1	0	0	37.3893	37.3893	100.9399	0	PROCESSED	57613.4605787037	2016-08-13 11:03:14	56383	2013-04-01 00:00:00	56637.6375347222	2013-12-11 15:18:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081419	The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come.	EXTRAGALACTIC COMPACT SOURCES	7	C	TAHIR YAQOOB		USA	8	AO8	ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708029010/	Quick Look
447	MKN 1148	12.9805	17.4231	12.320857	17.151473	18.75445	10.92233	123.09650608	-45.44849404	266.997	56656.2855555556	2013-12-30 06:51:12	56657.0627662037	2013-12-31 01:30:23	708033010	28.3189	30	28.3189	28.3269	0	28.3269	2	2	0	2	1	0	0	23.1005	23.1005	67.1379	2	PROCESSED	57613.7155324074	2016-08-13 17:10:22	56383	2013-04-01 00:00:00	56702.7526273148	2014-02-14 18:03:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081419	The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come.	EXTRAGALACTIC COMPACT SOURCES	7	C	TAHIR YAQOOB		USA	8	AO8	ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708033010/	Quick Look
448	NGC 4593	189.9148	-5.3464	189.269905	-5.071886	191.204626	-0.990591	297.48422734	57.40070716	292.7769	56830.338275463	2014-06-22 08:07:07	56831.0988657407	2014-06-23 02:22:22	709014020	30.961	30	30.977	30.961	0	30.985	1	1	0	1	1	0	0	30.408	30.408	65.688	0	PROCESSED	57615.3154976852	2016-08-15 07:34:19	57212	2015-07-09 00:00:00	56846.5106365741	2014-07-08 12:15:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090097	In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	9	AO9	X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014020/	Quick Look
449	PMN J1603-4904	240.9652	-49.0681	240.045662	-48.930987	248.937832	-27.726173	332.15292306	2.57171396	292.7209	56547.6621643518	2013-09-12 15:53:31	56548.4842013889	2013-09-13 11:37:15	708035010	50.9129	50	50.9252	50.9129	0	50.9172	3	2	0	3	1	0	0	49.2803	49.2803	70.99	0	PROCESSED	57612.626875	2016-08-12 15:02:42	56956	2014-10-26 00:00:00	56588.7813657407	2013-10-23 18:45:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081432	We propose a 50ksec Suzaku observation of the gamma-ray emitting compact symmetric radio source PMN J1603-4904 as a crucial part of the first simultaneous radio to gamma-ray campaign on this object. Constraining the X-ray spectrum of the compact radio source is needed to properly model the broadband spectral energy distribution (SED), which is essential for understanding the physical nature of this unusual object. The Swift detection allows no spectral modeling of its very faint X-ray counterpart, hence, precise spectral investigations with Suzaku are strongly required. PMN J1603-4904 is one of the few young radio galaxy candidates associated with a bright Fermi gamma-ray source, thus it plays a key role in investigating the underlying emission mechanism of newly born active galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	A	ROOPESH OJHA		USA	8	AO8	CONSTRAINING THE NATURE OF PMN J1603-4904: IS IT A GAMMA-LOUD YOUNG RADIO GALAXY?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708035010/	Quick Look
450	SWIFT J0250.7+4142	42.6629	41.6747	41.856234	41.468698	53.00104	24.122797	145.63636615	-15.88173015	76.5152	56872.0541898148	2014-08-03 01:18:02	56873.8814930556	2014-08-04 21:09:21	709006010	82.1549	80	82.1629	82.1629	0	82.1549	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.4596527778	2016-08-16 11:01:54	57267	2015-09-02 00:00:00	56902.7258564815	2014-09-02 17:25:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090019	Swift/BAT extragalactic survey above E >15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe two Compton thick AGN candidates in the 70 month BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	9	AO9	DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709006010/	Quick Look
451	NGC 4593	189.9131	-5.3423	189.268209	-5.067785	191.201461	-0.987483	297.48045078	57.40464867	113.7512	57006.6309375	2014-12-15 15:08:33	57007.3023263889	2014-12-16 07:15:21	709014030	30.5312	30	30.5312	30.5392	0	30.5392	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.5109722222	2016-08-17 12:15:48	57383	2015-12-27 00:00:00	57017.413900463	2014-12-26 09:56:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090097	In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	9	AO9	X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014030/	Quick Look
452	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
453	PKS1510-089	228.2094	-9.0956	227.535962	-8.908847	228.284042	8.500549	351.2919833	40.14272744	102.2005	54858.1887615741	2009-01-27 04:31:49	54859.2258564815	2009-01-28 05:25:14	703005010	44.3054	40	44.3054	44.3054	0	44.3054	2	2	0	2	1	0	0	16.6537	16.6537	89.5979	0	PROCESSED	57545.3861342593	2016-06-06 09:16:02	54557	2008-04-01 00:00:00	54880.5404282407	2009-02-18 12:58:13	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	030004	We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	3	AO3	REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703005010/	Quick Look
454	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
455	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
456	HOLMBERG IX X-1	149.4599	69.05	148.442008	69.288451	119.782652	51.677007	141.95121201	41.07533054	294.5528	56780.1586111111	2014-05-03 03:48:24	56780.8752546296	2014-05-03 21:00:22	709015010	31.886	30	31.886	31.886	0	31.886	2	2	0	2	1	0	0	30.8618	30.8618	61.9159	0	PROCESSED	57615.0271990741	2016-08-15 00:39:10	57218	2015-07-15 00:00:00	56852.5963194444	2014-07-14 14:18:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091251	Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs.	EXTRAGALACTIC COMPACT SOURCES	7	A	DOMINIC WALTON		USA	9	AO9	MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015010/	Quick Look
457	Q0142-100	26.3171	-9.7556	25.697719	-10.005838	20.677718	-19.226515	161.63610788	-68.48152364	68.9469	56854.9601041667	2014-07-16 23:02:33	56856.4794328704	2014-07-18 11:30:23	709019010	60.9751	55	60.9831	60.9831	0	60.9751	2	2	0	2	1	0	0	10.53	10.53	22.736	0	PROCESSED	57615.4077083333	2016-08-15 09:47:06	57261	2015-08-27 00:00:00	56895.341412037	2014-08-26 08:11:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091431	The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission.	EXTRAGALACTIC COMPACT SOURCES	7	B	BIN CHEN		USA	9	AO9	CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709019010/	Quick Look
458	HE0512-3329	78.54	-33.4465	78.079714	-33.502938	72.667363	-56.201883	236.6358247	-33.85842065	104.8837	56933.2970833333	2014-10-03 07:07:48	56934.0071180556	2014-10-04 00:10:15	709020020	27.5086	60	27.5086	27.5166	0	27.5166	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6104976852	2016-08-16 14:39:07	57345	2015-11-19 00:00:00	56979.4110300926	2014-11-18 09:51:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091431	The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission.	EXTRAGALACTIC COMPACT SOURCES	7	B	BIN CHEN		USA	9	AO9	CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709020020/	Quick Look
459	MARKARIAN 3	93.8921	71.0501	92.441744	71.065491	91.879164	47.635184	143.28202475	22.71957945	87.4437	56931.9222337963	2014-10-01 22:08:01	56932.4181597222	2014-10-02 10:02:09	709022010	23.831	20	23.831	23.831	0	23.8376	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5994328704	2016-08-16 14:23:11	57345	2015-11-19 00:00:00	56979.4072569444	2014-11-18 09:46:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092008	We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each.	EXTRAGALACTIC COMPACT SOURCES	7	A	MATTEO GUAINAZZI		EUR	9	AO9	MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022010/	Quick Look
460	NGC5548	214.4931	25.1284	213.926191	25.358593	201.994041	36.406695	31.93341942	70.49864062	309.3821	54269.9362847222	2007-06-18 22:28:15	54270.6389814815	2007-06-19 15:20:08	702042010	31.1188	30	31.1188	31.1188	0	31.1188	2	2	0	2	1	0	0	27.1759	27.1759	60.7059	0	PROCESSED	57538.9803703704	2016-05-30 23:31:44	54695	2008-08-17 00:00:00	54319.4659953704	2007-08-07 11:11:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021307	We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	2	AO2	NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042010/	Quick Look
461	IGR J16185-5928	244.6464	-59.4001	243.583076	-59.27851	254.074844	-37.350679	326.66672881	-6.44446627	90.0003	54505.6700115741	2008-02-09 16:04:49	54507.0211111111	2008-02-11 00:30:24	702123010	76.6076	88	76.631	76.6236	0	76.6076	2	2	0	2	1	0	0	75.2553	75.2553	116.7259	0	PROCESSED	57541.5586226852	2016-06-02 13:24:25	54888	2009-02-26 00:00:00	54515.6564699074	2008-02-19 15:45:19	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022034	We propose to observe with Suzaku two Narrow Line Seyfert 1 galaxies detected by SWIFT/BAT and INTEGRAL with a flux in excess of $10^{-11}$~erg~s$^{-1}$~cm$^{-2}$ in the HXD/PIN band for 70~ks each. These proposed observations provide rare high quality spectra of NLS1s above 10~keV. This will remove the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM--Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources (namely absorption, reflection, nature of the soft excess...).	EXTRAGALACTIC COMPACT SOURCES	7	B	GIOVANNI MINIUTTI		EUR	2	AO2	HUNTING HARD-X-RAY-BRIGHT NLS1 GALAXIES FROM THE INTEGRAL CATALOGUE WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702123010/	Quick Look
462	SWIFT J1322.2-1641	200.5819	-16.7858	199.912392	-16.524578	205.294799	-7.530887	313.4989766	45.45121448	290.037	55013.9738310185	2009-07-01 23:22:19	55014.9981365741	2009-07-02 23:57:19	704022010	41.3487	40	41.3487	41.6207	0	41.6127	2	2	0	2	1	0	0	36.2368	36.2368	88.4858	7	PROCESSED	57547.7444097222	2016-06-08 17:51:57	55393	2010-07-16 00:00:00	55027.0523148148	2009-07-15 01:15:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	043059	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA	MAURO DADINA	JEU	4	AO4	SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704022010/	Quick Look
463	PKS0625-354	96.7724	-35.4904	96.328951	-35.45865	100.652009	-58.681247	243.45420005	-19.97253333	121.4596	55868.6502199074	2011-11-03 15:36:19	55871.6231597222	2011-11-06 14:57:21	706014010	100.7198	100	100.7278	100.7278	0	100.7198	2	2	0	2	1	0	0	86.4342	86.4342	256.8138	4	PROCESSED	57603.7550231482	2016-08-03 18:07:14	56250	2012-11-19 00:00:00	55881.2887731482	2011-11-16 06:55:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060046	We propose to observe two radio galaxies 3C78 and PKS0625-354 which were detected by the Fermi gamma-ray satellte survey during the 1st year, in order to investigate the X-ray emission more precisely than ever. In the case of jet emission, we can constrain the jet parameter well from the multi-wavelength spectrum and obtain the jet kinetic energy. In the case of disk emission, we can obtain the jet to disk energy ratio. This observation will enable us to obtain the jet parameters of these galaxies and compare them with others.	EXTRAGALACTIC COMPACT SOURCES	7	B	YASUSHI FUKAZAWA		JAP	6	AO6	ORIGIN OF THE X-RAY EMISSION OF GAMAM-RAY RADIO GALAXIES 3C78 AND PKS0625-354	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706014010/	Quick Look
464	IC 342 X2	56.548	68.1243	55.335293	67.96844	72.578132	46.699378	138.10903546	10.56584534	237.0509	55640.3693981482	2011-03-20 08:51:56	55641.8058101852	2011-03-21 19:20:22	705009020	75.4467	80	75.4707	75.4467	0	75.4787	2	2	0	2	1	0	0	74.2577	74.2577	124.0898	1	PROCESSED	57601.2497800926	2016-08-01 05:59:41	56019	2012-04-02 00:00:00	55652.0183680556	2011-04-01 00:26:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050041	The nature of ultraluminous X-ray sources (ULXs) is one of the important unresolved issues in the modern astrophysics. A Suzaku HXD spectrum above 10 keV and its variation, in combination with those with XIS, provide us with an unique opportunity to determine unambiguously the physical state of ULXs, which is a key information to solve their nature. Here, two 80 ks Suzaku exposures are proposed on a bright ULX IC 342 X2, one of the most promising candidates for hard X-ray detection.	EXTRAGALACTIC COMPACT SOURCES	7	A	NAOKI ISOBE		JAP	5	AO5	HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705009020/	Quick Look
465	EMS1274	285.5178	-51.1684	284.542504	-51.240609	280.974965	-28.317711	345.57919311	-22.40122796	103.8598	55299.2761921296	2010-04-13 06:37:43	55300.0056944445	2010-04-14 00:08:12	705014010	43.9253	40	43.9253	43.9333	0	43.9333	2	2	0	2	1	0	0	34.9581	34.9581	63.0159	0	PROCESSED	57551.1958333333	2016-06-12 04:42:00	55675	2011-04-24 00:00:00	55309.2111458333	2010-04-23 05:04:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050050	We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators".	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5	SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705014010/	Quick Look
466	3C111	64.5838	38.0364	63.747621	37.915108	69.36876	16.399466	161.66578558	-8.81556542	79.7358	55441.1593055556	2010-09-02 03:49:24	55442.8995138889	2010-09-03 21:35:18	705040010	80.683	80	80.691	80.683	0	80.691	2	2	0	2	1	0	0	73.3707	73.3707	150.3079	1	PROCESSED	57553.2986458333	2016-06-14 07:10:03	55822	2011-09-18 00:00:00	55456.2202430556	2010-09-17 05:17:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051412	Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components.	EXTRAGALACTIC COMPACT SOURCES	7	A	RITA SAMBRUNA		USA	5	AO5	PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705040010/	Quick Look
467	3C111	64.5838	38.0341	63.747638	37.912808	69.368333	16.397202	161.66743119	-8.81719194	77.8463	55448.0268865741	2010-09-09 00:38:43	55449.7585416667	2010-09-10 18:12:18	705040020	79.4198	80	79.4198	79.4198	0	79.4198	2	2	0	2	1	0	0	71.809	71.809	149.6058	0	PROCESSED	57553.3942592593	2016-06-14 09:27:44	55827	2011-09-23 00:00:00	55461.3122106482	2010-09-22 07:29:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051412	Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components.	EXTRAGALACTIC COMPACT SOURCES	7	A	RITA SAMBRUNA		USA	5	AO5	PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705040020/	Quick Look
468	MRK 841	226.0057	10.444	225.402057	10.638407	220.18036	26.59752	11.21871304	54.63485497	108.0015	55944.7625347222	2012-01-18 18:18:03	55947.3599305556	2012-01-21 08:38:18	706029020	110.289	350	110.2915	110.289	0	110.2915	2	2	0	2	1	0	0	92.2182	92.2182	224.404	1	PROCESSED	57604.469224537	2016-08-04 11:15:41	55652	2011-04-01 00:00:00	55985.3097337963	2012-02-28 07:26:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061119	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	6	AO6-LP	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706029020/	Quick Look
469	SWIFT J0544.4-4328	86.0099	-43.419	85.632201	-43.439311	82.65148	-66.759602	249.50201979	-30.05213281	308.9989	57140.9252083333	2015-04-28 22:12:18	57143.359212963	2015-05-01 08:37:16	709005010	84.362	100	84.362	92.7251	0	92.7171	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.0749537037	2016-08-18 01:47:56	57527	2016-05-19 00:00:00	57160.6331597222	2015-05-18 15:11:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	090018	We propose to observe two hard X-ray bright Seyfert galaxies with a highly accreting small BH. This class of objects is of importance in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be fundamental pieces of information to better understand accretion physics and ``feedback'' processes in galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	C	YUICHI TERASHIMA		JAP	9	AO9	ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED LOW-MASS SEYFERTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709005010/	Quick Look
470	OT+081	267.8906	9.6366	267.297097	9.648276	267.507831	33.058606	34.9082961	17.63584745	268.2827	55830.0996759259	2011-09-26 02:23:32	55830.3911921296	2011-09-26 09:23:19	706047010	10.774	10	10.774	10.774	0	10.774	1	1	0	1	1	0	0	11.036	11.036	25.1519	1	PROCESSED	57603.2492708333	2016-08-03 05:58:57	56225	2012-10-25 00:00:00	55875.6247569444	2011-11-10 14:59:39	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061601	We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	6	AO6	EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706047010/	Quick Look
471	RXJ0134-4258	23.5686	-42.9671	23.03099	-43.222871	359.764354	-47.882347	276.92816891	-71.93227434	245.0998	56290.2726851852	2012-12-29 06:32:40	56292.2506481482	2012-12-31 06:00:56	707014010	81.429	50	81.4485	81.445	0	81.429	2	2	0	2	1	0	0	16.1219	16.1219	37.6859	0	PROCESSED	57608.396087963	2016-08-08 09:30:22	56702	2014-02-14 00:00:00	56336.5473263889	2013-02-13 13:08:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070081	RXJ0134.2-4258 was detected in the ROSAT all sky observation (RASS), later identified as a radio loud (RL) narrow line Seyfert 1 galaxy. During the RASS, the soft X-ray spectrum of this source was steep. Following observations with ROSAT, ASCA, Swift, and XMM-Newton (XMM) showed flatter spectra. The XMM spectra are fitted with a power law with an cut-off (EC) at 4 keV, where a blackbody (BB) component was not evident. Either type of spectrum is not common for Seyferts. We consider this peculiarity is related to the RL nature of this object, originated in the jet. We will observe this source with Suzaku, which has higher energy resolution than XMM, to reveal the long term variability of this source. Particular interests go to the EC energy, bb component, and the iron K emission line.	EXTRAGALACTIC COMPACT SOURCES	7	C	HIROAKI TAKAHASHI		JAP	7	AO7	X-RAY EMISSION FROM THE BRIGHTEST RADIO LOUD NARROW LINE SEYFERT 1 RXJ0134.2-4258	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707014010/	Quick Look
472	0827+243	127.7155	24.1863	126.975126	24.355162	124.074961	5.096162	200.01763935	31.87561316	105.3936	56213.3893287037	2012-10-13 09:20:38	56213.5959837963	2012-10-13 14:18:13	707041010	8.0392	10	8.0472	8.0392	0	8.0472	1	1	0	1	1	0	0	7.737	7.737	17.8479	0	PROCESSED	57607.7474652778	2016-08-07 17:56:21	56598	2013-11-02 00:00:00	56232.4327199074	2012-11-01 10:23:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071601	We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	7	AO7	MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707041010/	Quick Look
473	MKN 6	103.0685	74.413	101.450971	74.472117	95.572656	51.225087	140.3435691	26.1094153	254.4482	57133.5883333333	2015-04-21 14:07:12	57134.7015046296	2015-04-22 16:50:10	710001010	50.6541	50	50.6541	51.3396	0	51.3396	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.0317476852	2016-08-18 00:45:43	57548	2016-06-09 00:00:00	57154.4415162037	2015-05-12 10:35:47	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101730	We request two quasi-simultaneous NuSTAR + Suzaku-XIS pointings of the radio-loud Sy 1.5 Mkn 6 to understand the complexity of its accreting circumnuclear gas structures. A series of high-quality, broadband X-ray spectra, including coverage above 10 keV, are needed to properly quantify the variable and complex line of sight absorbers. These new observations, in conjunction with radio and previous X-ray observations, will be a unique opportunity to understand accretion modes in the innermost regions of a radio-loud AGN that has recently undergone a merger.	EXTRAGALACTIC COMPACT SOURCES	7	A	ALEX MARKOWITZ		USA	10	AO10	COMPLEX CIRCUMNUCLEAR ABSORPTION IN RADIO-LOUD AGN: VARIABLE ABSORPTION IN MKN 6	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710001010/	Quick Look
474	MARKARIAN 3	93.9093	71.025	92.46011	71.040478	91.888941	47.610328	143.30979342	22.71730777	267.1766	57116.4730902778	2015-04-04 11:21:15	57116.9877199074	2015-04-04 23:42:19	709022050	21.4556	20	21.4556	21.4556	0	21.4556	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.9089814815	2016-08-17 21:48:56	57550	2016-06-11 00:00:00	57183.6622916667	2015-06-10 15:53:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092008	We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each.	EXTRAGALACTIC COMPACT SOURCES	7	A	MATTEO GUAINAZZI		EUR	9	AO9	MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709022050/	Quick Look
475	NGC 3516	166.6817	72.5579	165.82888	72.82825	123.376111	57.97325	133.24892211	42.40929053	306.0068	57154.3345023148	2015-05-12 08:01:41	57157.0348611111	2015-05-15 00:50:12	710009010	117.7012	120	117.7012	123.0032	0	124.7632	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.6915277778	2016-08-18 16:35:48	57593	2016-07-24 00:00:00	57224.4439467593	2015-07-21 10:39:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	100040	In the AO-8 cycle, we have proposed several X-ray and optical simultaneous observations of a type I Seyfert galaxy NGC 3516, and obtained a good correlation between those wavelengths in its faint phase. The result suggests that a hard primary X-ray continua found in NGC 3516 by Noda et al. (2013) is generated in a corona formed closely to an accretion disk, which is possibly a radiatively inefficient accretion flow. As a next step, we examine whether or not an X-ray variation is also correlated with that in optical, when NGC 3516 is in the bright phase, and the other primary X-ray continuum, also reported by Noda et al. (2013), is dominant. For it, we propose an X-ray and optical simultaneous observation of NGC 3516 with an exposure of 120 ksec, which is triggered by a Swift monitoring.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	10	AO10-TOO	X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF NGC 3516 IN ITS BRIGHT PHASE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710009010/	Quick Look
476	OJ 287	133.7046	20.1043	132.989527	20.295378	130.505611	2.596765	206.8173824	35.82032681	285.8742	57145.5508449074	2015-05-03 13:13:13	57148.4467592593	2015-05-06 10:43:20	710011010	111.6388	323	111.6388	111.6388	0	111.6388	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.1122800926	2016-08-18 02:41:41	57113	2015-04-01 00:00:00	57164.5257523148	2015-05-22 12:37:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101431	Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously.	EXTRAGALACTIC COMPACT SOURCES	7	A	RICK EDELSON		USA	10	AO10	SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011010/	Quick Look
477	NGC 2992	146.4592	-14.2821	145.857736	-14.050853	154.047551	-26.059819	249.69438343	28.83515423	128.4959	53717.4275462963	2005-12-13 10:15:40	53718.506412037	2005-12-14 12:09:14	700005030	46.8361	120	46.8441	46.8681	46.8361	46.8601	2	2	2	2	1	0	0	44.2983	44.2983	93.2079	1	PROCESSED	57532.4690046296	2016-05-24 11:15:22	54247	2007-05-27 00:00:00	54039.2254861111	2006-10-31 05:24:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001013	NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	0	SWG	THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005030/	Quick Look
478	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
479	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
480	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
481	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
482	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
483	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
484	Q1158-1843	180.1895	-18.9957	179.549068	-18.717273	187.964658	-17.299195	286.65628264	42.26876142	291.8577	54636.8208912037	2008-06-19 19:42:05	54637.4202314815	2008-06-20 10:05:08	703039010	24.085	22	24.101	24.085	0	24.101	2	2	0	2	1	0	0	22.4309	22.4309	51.7819	1	PROCESSED	57542.8567361111	2016-06-03 20:33:42	55014	2009-07-02 00:00:00	54648.3349305556	2008-07-01 08:02:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031334	Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates.	EXTRAGALACTIC COMPACT SOURCES	7	B	GEORGE CHARTAS		USA	3	AO3	A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703039010/	Quick Look
485	MCG-6-30-15	203.9706	-34.2946	203.254215	-34.039458	215.17105	-22.544253	313.28931603	27.68170589	107.0204	53744.9738310185	2006-01-09 23:22:19	53749.1390277778	2006-01-14 03:20:12	700007010	143.1965	300	143.1965	143.3162	143.2685	143.2445	2	2	2	2	1	0	0	126.2903	126.2903	359.8399	4	PROCESSED	57532.7604398148	2016-05-24 18:15:02	54247	2007-05-27 00:00:00	54040.4060416667	2006-11-01 09:44:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001035	The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales .	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREW FABIAN		JAP	0	SWG	REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007010/	Quick Look
486	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
487	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
488	NGC3227	155.8772	19.8688	155.194637	20.122177	150.387911	9.14334	216.98506904	55.4463804	114.6051	54774.1503587963	2008-11-04 03:36:31	54775.6780555556	2008-11-05 16:16:24	703022020	53.6995	50	53.6995	53.6995	0	53.6995	2	2	0	2	1	0	0	50.2891	50.2891	131.9718	3	PROCESSED	57544.3625810185	2016-06-05 08:42:07	54557	2008-04-01 00:00:00	54788.4371643518	2008-11-18 10:29:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031013	We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	3	AO3	NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022020/	Quick Look
489	MCG-02-14-009	79.0657	-10.5106	78.475918	-10.56483	77.084553	-33.463679	211.75204832	-25.86275025	68.0451	54706.9410069444	2008-08-28 22:35:03	54710.0308333333	2008-09-01 00:44:24	703060010	142.1522	125	142.1522	142.1522	0	142.1522	2	2	0	2	1	0	0	129.5879	129.5879	266.9199	1	PROCESSED	57543.5182986111	2016-06-04 12:26:21	55100	2009-09-26 00:00:00	54731.4652430556	2008-09-22 11:09:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032009	MCG--02-14-009 appears to have the strongest relativistic iron line of all the Seyfert 1s: a short 5 ks XMM-Newton observation found the line to have an EW 530-770 eV, two times larger than for MCG-6-30-15. We propose a 125 ks Suzaku observation of this AGN, which provides a unique opportunity to probe the innermost accretion disk in the region of strong gravity. The main goals are: (a) utilise the unique broad bandpass of Suzaku to detect the expected strong reflection hump and determine the form of the X-ray continuum; (b) accurately measure the relativistic iron K line profile and thereby the geometry of the X-ray emitting region and (c) determine whether the iron line responds to the continuum down to the orbital timescales of the inner disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		EUR	3	AO3	MCG-02-14-009: PROBING THE PHYSICAL PROPERTIES OF THE STRONGEST IRON K LINE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703060010/	Quick Look
490	2MASX J02485937+2630	42.225	26.5707	41.491892	26.363374	47.759882	9.863115	153.13364356	-29.32417791	74.088	55030.159224537	2009-07-18 03:49:17	55031.3766782407	2009-07-19 09:02:25	704013010	42.9501	40	42.9501	43.2153	0	43.2247	2	2	0	2	1	0	0	29.5403	29.5403	105.1719	0	PROCESSED	57547.8817013889	2016-06-08 21:09:39	55415	2010-08-07 00:00:00	55048.2541435185	2009-08-05 06:05:58	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	040060	Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe three Compton thick AGN candidates in the 22 months BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	4	AO4	DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704013010/	Quick Look
491	2FGL J0923.5+1508	140.9887	15.0811	140.300178	15.296347	138.613889	-0.175811	215.96780071	40.48329137	287.9737	56046.2642939815	2012-04-29 06:20:35	56048.4933449074	2012-05-01 11:50:25	707007010	95.2554	90	95.2794	95.2554	0	95.2794	2	2	0	2	1	0	0	89.5878	89.5878	192.568	1	PROCESSED	57605.3423611111	2016-08-05 08:13:00	56434	2013-05-22 00:00:00	56068.6261921296	2012-05-21 15:01:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070024	We propose X-ray follow up observations of two high redshift blazar candidates in the Fermi/LAT unidentified sources. The aim of this proposal is to detect X-ray emissions from high redshift blazars (z >> 3) buried in unidentified Fermi/LAT sources and to find the most distant LAT detected blazar. Gamma-ray photons above 10 GeV are attenuated by interactions with UV photons which result in creating electron-positron pairs. Therefore, attenuation signatures are predicted to be observed in gamma-ray spectra and such attenuation of high redshift blazars with redshift up to z ~ 6 provide information about UV background out to the epoch of cosmological reionization. By utilizing the attenuation, we can investigate the UV radiation state of the early universe.	EXTRAGALACTIC COMPACT SOURCES	7	B	YOSUKE TAKAHASHI		JAP	7	AO7	SUZAKU OBSERVATIONS OF HIGH REDSHIFT BLAZAR CANDIDATES IN THE FERMI UNIDENTIFIED SOURCE SAMPLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707007010/	Quick Look
492	IC4329A	207.3321	-30.3098	206.617944	-30.061645	216.345264	-17.777119	317.49793706	30.91926559	298.5047	54332.9765740741	2007-08-20 23:26:16	54333.5558333333	2007-08-21 13:20:24	702113050	24.0262	25	24.0262	24.0262	0	24.0262	2	2	0	2	1	0	0	18.8256	18.8256	50.0439	1	PROCESSED	57539.6252083333	2016-05-31 15:00:18	54730	2008-09-21 00:00:00	54350.649375	2007-09-07 15:35:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022009	IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASSIMO CAPPI		EUR	2	AO2	SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702113050/	Quick Look
493	IC 4329A	207.3331	-30.3096	206.618942	-30.061447	216.346028	-17.776613	317.49896941	30.91923491	296.2	56152.0924652778	2012-08-13 02:13:09	56154.6425578704	2012-08-15 15:25:17	707025010	117.5938	120	117.5938	117.5938	0	117.5938	2	2	0	2	1	0	0	112.9986	112.9986	220.2637	2	PROCESSED	57606.8955208333	2016-08-06 21:29:33	56540	2013-09-05 00:00:00	56170.1592824074	2012-08-31 03:49:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071417	We propose simultaneous NuSTAR/Suzaku observations of NGC 4151 and IC 4329A. These pointings will achieve three goals: (1) They will provide the best-ever broad-band X-ray spectra of two of the brightest Seyfert galaxies in the 0.5-80 keV band; (2) They will enable broad-band, time-resolved X-ray spectroscopy of these fascinating and variable sources; (3) They will serve as invaluable calibration targets for the two observatories. The spectral coverage and sensitivity will enable the continuum, absorption and reflection components of each spectrum to be conclusively disentangled, allowing us to determine whether inner disk reflection signatures are present. We will also be able to break the degeneracy between the coronal temperature and optical depth in both AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	LAURA BRENNEMAN		USA	7	AO7	SHEDDING NEW LIGHT ON THE BROAD-BAND X-RAY SPECTRA OF NGC 4151 AND IC 4329A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707025010/	Quick Look
494	NGC 1448	56.1426	-44.6942	55.730836	-44.850191	33.469346	-61.660504	251.59735556	-51.37690943	264.6522	54879.3481828704	2009-02-17 08:21:23	54880.4501041667	2009-02-18 10:48:09	703062010	52.9653	50	52.9653	52.9653	0	52.9653	2	2	0	2	1	0	0	55.0869	55.0869	95.202	1	PROCESSED	57545.5960763889	2016-06-06 14:18:21	55330	2010-05-14 00:00:00	54893.4451041667	2009-03-03 10:40:57	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032018	We propose for a 50 ks Suzaku observation of NGC 1448, a nearby (15 Mpc) gas-rich and dust-obscured Scd galaxy that is optically classified as an HII galaxy. From our Spitzer-IRS mid-IR spectroscopy, we have found the first evidence for an obscured AGN in NGC 1448. On the basis of this data, NGC 1448 appears to be harboring a rapidly growing small obscured black hole (M_BH ~ 6x10^5 M_Sun; Eddington ratio of >0.1), and therefore appears to be an analog of the nearby Compton-thick AGN NGC 4945. To date, no sensitive hard X-ray constraints exist for NGC 1448, which are required to provide a direct measurement of the absorption and mass accretion rate, and thus to test if NGC 1448 is also a Compton-thick AGN.	EXTRAGALACTIC COMPACT SOURCES	7	C	DAVID ALEXANDER		EUR	3	AO3	NGC 1448: A MISSING COMPTON-THICK AGN IN OUR BACKYARD?	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703062010/	Quick Look
495	NGC 4138	182.4434	43.7345	181.812692	44.012643	161.129219	40.276316	147.09151655	71.38668226	137.6226	55137.5331365741	2009-11-02 12:47:43	55138.8849305556	2009-11-03 21:14:18	704047010	60.7716	60	60.8436	60.7716	0	60.8436	2	2	0	2	1	0	0	35.8724	35.8724	116.7818	2	PROCESSED	57549.0852893518	2016-06-10 02:02:49	55517	2010-11-17 00:00:00	55151.1923263889	2009-11-16 04:36:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041415	The SWIFT BAT hard (14-195 KeV) survey is performing the first unbiased hard X-ray survey of the entire sky with follow-up observations with the Swift XRT to fully identify the sample. In this survey we have found two very low luminosity nearby hard X-ray sources which show little, if any, evidence for nuclear activity in the optical or UV band, and have very low apparent Eddington ratios. We propose Suzaku observations of these objects to determine whether there is an X-ray spectral signature of a low Eddington ratio, as predicted if these objects are indeed in a radiatively inefficient accretion flow.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	4	AO4	SUZAKU OBSERVATIONS OF NGC4138 AND NGC3718	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704047010/	Quick Look
496	EMS1160	264.608	87.3047	269.889788	87.318057	90.726547	69.241949	120.03425165	27.94259409	59.9344	55312.9874537037	2010-04-26 23:41:56	55313.4279513889	2010-04-27 10:16:15	705012010	20.2796	20	20.2796	20.2796	0	20.2796	2	2	0	2	1	0	0	19.8004	19.8004	38.0539	1	PROCESSED	57551.2894097222	2016-06-12 06:56:45	55693	2011-05-12 00:00:00	55327.1544791667	2010-05-11 03:42:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050050	We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators".	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	5	AO5	SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705012010/	Quick Look
497	EMS1388	309.878	-56.3562	308.912808	-56.532938	296.209629	-36.489343	341.17879119	-37.12820094	256.6037	55497.456400463	2010-10-28 10:57:13	55498.1383912037	2010-10-29 03:19:17	705028010	21.5336	20	21.5416	21.5416	0	21.5336	2	2	0	2	1	0	0	18.3735	18.3735	58.9099	0	PROCESSED	57553.876724537	2016-06-14 21:02:29	55875	2011-11-10 00:00:00	55508.9886342593	2010-11-08 23:43:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	050126	Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects.	EXTRAGALACTIC COMPACT SOURCES	7	C	YASUYUKI TANAKA		JAP	5	AO5	SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705028010/	Quick Look
498	B3 0309+411	48.2809	41.3324	47.459303	41.145685	57.252935	22.518841	149.59257755	-14.09014879	253.0016	55976.5100462963	2012-02-19 12:14:28	55979.0410532407	2012-02-22 00:59:07	706036010	104.6245	100	104.6245	104.6296	0	104.6245	2	2	0	2	1	0	0	95.453	95.453	218.6719	2	PROCESSED	57604.7018981482	2016-08-04 16:50:44	56360	2013-03-09 00:00:00	55992.2317824074	2012-03-06 05:33:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062007	We propose to observe B3 0309+411, an X--ray bright FRII BLRG detected by INTEGRAL for 100 ks. BRLGs have been poorly studied in X-rays and usually show weak reprocessing spectral features with respect to their radio-quiet counterparts. B3 0309+411 has been already followed-up with XMM-Newton and, the XMM-Newton and INTEGRAL data suggests that the source could 1) be strongly reflection-dominated; 2) exhibit extreme flux/spectral variability; 3) be severely affected by absorption. The Suzaku observation will unveil the puzzling spectral shape of this peculiar BLRG, allowing to determine with accuracy the reflection properties which would have a large impact on our understanding of the disk/jet contribution in BLRG.	EXTRAGALACTIC COMPACT SOURCES	7	B	FRANCESCA PANESSA		EUR	6	AO6	B3 0309+411: A REFLECTION--DOMINATED BROAD LINE RADIO GALAXY?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706036010/	Quick Look
499	FAIRALL 51	281.2238	-62.3567	280.059933	-62.408117	276.678489	-39.176005	333.20743511	-23.0882296	252.0031	56539.073587963	2013-09-04 01:45:58	56539.5245486111	2013-09-04 12:35:21	708046010	31.5576	30	31.5576	31.5676	0	31.5656	2	2	0	2	1	0	0	25.6549	25.6549	38.9559	0	PROCESSED	57612.4964236111	2016-08-12 11:54:51	56956	2014-10-26 00:00:00	56587.5110763889	2013-10-22 12:15:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082016	Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures.	EXTRAGALACTIC COMPACT SOURCES	7	A	JIRI SVOBODA		EUR	8	AO8	STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708046010/	Quick Look
500	NGC2273	102.5972	60.7838	101.469265	60.841838	97.733599	37.680709	155.04232679	23.32753471	246.2514	54211.2737384259	2007-04-21 06:34:11	54212.5071643518	2007-04-22 12:10:19	702003010	90.0126	50	90.0286	90.0206	0	90.0126	2	2	0	2	1	0	0	69.5887	69.5887	106.5579	1	PROCESSED	57538.4439583333	2016-05-30 10:39:18	54744	2008-10-05 00:00:00	54216.1628703704	2007-04-26 03:54:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	020005	Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei.	EXTRAGALACTIC COMPACT SOURCES	7	A	HISAMITSU AWAKI		JAP	2	AO2	REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702003010/	Quick Look
501	NGC 4941	196.0528	-5.5595	195.404956	-5.291518	196.919842	1.18027	308.80102111	57.16661738	292.811	56100.4695833333	2012-06-22 11:16:12	56102.2446643518	2012-06-24 05:52:19	707001010	80.8593	80	80.8593	80.8593	0	80.8593	2	2	0	2	1	0	0	76.7486	76.7486	153.32	1	PROCESSED	57605.7725115741	2016-08-05 18:32:25	56480	2013-07-07 00:00:00	56113.2872800926	2012-07-05 06:53:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070003	The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with intermediate to high luminosities. Here we propose to observe two of the lowest luminosity AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background.	EXTRAGALACTIC COMPACT SOURCES	7	A	YOSHIHIRO UEDA		JAP	7	AO7	BROAD BAND SPECTRA OF HARD X-RAY SELECTED LOW LUMINOSITY AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707001010/	Quick Look
502	2FGL J0022.2-1853	5.5431	-18.8956	4.911171	-19.172887	357.260083	-19.481593	82.15155077	-79.37005347	62.0041	56077.5533564815	2012-05-30 13:16:50	56078.2856944445	2012-05-31 06:51:24	707009010	34.8678	30	34.8678	34.8678	0	34.8678	2	2	0	2	1	0	0	35.1964	35.1964	63.2639	1	PROCESSED	57605.5769444444	2016-08-05 13:50:48	56456	2013-06-13 00:00:00	56090.1516435185	2012-06-12 03:38:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070034	We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN).	EXTRAGALACTIC COMPACT SOURCES	7	B	JUN KATAOKA		JAP	7	AO7	FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707009010/	Quick Look
503	NGC1365	53.4048	-36.1458	52.927471	-36.312752	36.803781	-53.045581	237.96516908	-54.5951856	59.0002	56116.8446064815	2012-07-08 20:16:14	56117.6910763889	2012-07-09 16:35:09	707017020	33.5858	30	33.5938	33.6018	0	33.5858	2	2	0	2	1	0	0	32.579	32.579	73.1059	2	PROCESSED	57606.5919791667	2016-08-06 14:12:27	56508	2013-08-04 00:00:00	56142.1709606482	2012-08-03 04:06:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	070095	NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. }	EXTRAGALACTIC COMPACT SOURCES	7	B	YASUSHI FUKAZAWA		JAP	7	AO7	MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017020/	Quick Look
504	HE0512-3329	78.5402	-33.4449	78.079903	-33.501337	72.668068	-56.200323	236.63398617	-33.8579138	105.1284	56932.4291435185	2014-10-02 10:17:58	56932.6252083333	2014-10-02 15:00:18	709020010	6.8649	60	6.873	6.8729	0	6.8649	3	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.600474537	2016-08-16 14:24:41	57345	2015-11-19 00:00:00	56979.403125	2014-11-18 09:40:30	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091431	The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission.	EXTRAGALACTIC COMPACT SOURCES	7	B	BIN CHEN		USA	9	AO9	CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709020010/	Quick Look
505	NGC 3516	166.74	72.5773	165.887815	72.847717	123.371896	57.999258	133.21492543	42.40213112	153.6201	56572.1874537037	2013-10-07 04:29:56	56573.9780092593	2013-10-08 23:28:20	708006050	0	50	0	0	0	0	0	0	0	0	1	0	0	37.2053	37.2053	154.6998	0	PROCESSED	57612.8632291667	2016-08-12 20:43:03	56383	2013-04-01 00:00:00	56631.766712963	2013-12-05 18:24:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	080066	We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines.	EXTRAGALACTIC COMPACT SOURCES	7	A	HIROFUMI NODA		JAP	8	AO8	THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006050/	Quick Look
506	HOLMBERG II X-1	124.8826	70.7169	123.581394	70.873481	106.843254	49.308296	144.27185866	32.72527495	119.959	56562.4955555556	2013-09-27 11:53:36	56563.5730324074	2013-09-28 13:45:10	708015020	49.283	50	49.283	49.283	0	49.283	2	2	0	2	1	0	0	48.206	48.206	93.0879	0	PROCESSED	57612.7832986111	2016-08-12 18:47:57	56954	2014-10-24 00:00:00	56588.5225462963	2013-10-23 12:32:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081251	Recent X-ray observations have produced evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in an unusual super-Eddington state. Current data are unable to deliver a clear answer, as attempts to model the 0.5-10keV spectra have been plagued by degeneracies resulting from the limited bandpass, owing to the previous lack of focusing hard X-ray telescopes. Combined, Suzaku and NuSTAR will obtain high-quality spectra covering 0.5-30keV, providing powerful probes for understanding the accretion modes and nature of the central BHs. A definitive statement on the existence of either 100-1000Msun black holes or extreme accretion states will be an important legacy of both missions.	EXTRAGALACTIC COMPACT SOURCES	7	A	DOMINIC WALTON		USA	8	AO8	COORDINATED SUZAKU AND NUSTAR OBSERVATIONS OF HOLMBERG II X-1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708015020/	Quick Look
507	ARP220	233.7664	23.5658	233.223657	23.731386	223.777121	41.366844	36.73879852	53.01919685	114.8377	53742.3490856482	2006-01-07 08:22:41	53744.9654398148	2006-01-09 23:10:14	700006010	98.5506	100	98.5586	98.5506	98.5586	98.5586	2	2	2	2	1	0	0	93.3623	93.3623	226.0419	2	PROCESSED	57532.6850925926	2016-05-24 16:26:32	54247	2007-05-27 00:00:00	54040.0356597222	2006-11-01 00:51:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001033	We propose a 100 ks observation of the nearest ultraluminous infrared galaxy (ULIG) Arp220. The major objective is to search for evidence of heavily obscured nuclei. First detection of a Compton-thick source may be possible with the HXD's sensitivity, if a powerful nucleus is present, leading to a major discovery. The good quality XIS spectrum can be decisive for the origin of the strong Fe K line, barely detected with the previous XMM-Newton observation.	EXTRAGALACTIC COMPACT SOURCES	7	A	KAZUSHI IWASAWA		JAP	0	SWG	HARD X-RAY EMISSION FROM THE NEAREST ULTRALUMINOUS INFRARED GALAXY ARP220	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700006010/	Quick Look
508	M81	148.8829	69.0533	147.858629	69.290285	119.502258	51.56628	142.10623941	40.90540672	287.1391	57160.4721180556	2015-05-18 11:19:51	57162.9807523148	2015-05-20 23:32:17	710017010	97.7022	100	97.7022	99.738	0	99.7444	3	2	0	2	0	0	0	0	0	0.3	0	PROCESSED	57618.7210532407	2016-08-18 17:18:19	57543	2016-06-04 00:00:00	57177.3710300926	2015-06-04 08:54:17	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	102700	We propose to observe the Low-Luminosity Active Galactic Nucleus of M81 for 200 ksec with NuSTAR and for 100 ksec with Suzaku. In low accretion rate AGN, where does the optically thick part of the accretion disk stop? Does it go in to within a few gravitational radii of the black hole, as in higher accretion rate Seyfert galaxies, or does it stop hundreds of gravitational radii from the black hole? Using NuSTAR and Suzaku spectra we will measure the strengths of the Compton reflection hump, Fe K alpha, Fe XXV and Fe XXVI lines. This will determine whether the Fe K alpha line is produced by reflection off the optically thick outer disk, or is produced in the optically thin inner flow. We will measure the reflection fraction and constrain the source geometry and disk transition radius.	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREW YOUNG		EUR	10	AO10	M81: ACCRETION GEOMETRY AT LOW EDDINGTON RATES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710017010/	Quick Look
509	WKK 4438	223.8214	-51.5512	222.94068	-51.348796	237.577105	-33.176773	321.7239088	6.74451921	87.8973	55948.1066319445	2012-01-22 02:33:33	55950.0610069444	2012-01-24 01:27:51	706011010	70.3088	100	70.3168	70.3088	0	70.3248	2	2	0	2	1	0	0	61.486	61.486	168.8259	3	PROCESSED	57604.5330324074	2016-08-04 12:47:34	56469	2013-06-26 00:00:00	56103.2331597222	2012-06-25 05:35:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	060032	We propose to observe two hard X-ray bright narrow-line Seyfert 1 galaxies, which are an important class of objects in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be a fundamental piece of information to better understand accretion physics and ``feedback'' processes in galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	B	YUICHI TERASHIMA		JAP	6	AO6	ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED NARROW-LINE SEYFERT 1S	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706011010/	Quick Look
510	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
511	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
512	SWIFT J0918.5+0425	139.5114	4.476	138.856225	4.686688	140.50448	-10.713106	227.10001498	34.41934616	102.3204	54408.8894097222	2007-11-04 21:20:45	54410.2293981482	2007-11-06 05:30:20	702076010	61.0185	53	61.0185	61.0401	0	61.0185	2	2	0	2	1	0	0	56.1565	56.1565	115.7659	2	PROCESSED	57540.4472916667	2016-06-01 10:44:06	54787	2008-11-17 00:00:00	54419.0312847222	2007-11-15 00:45:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021372	The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs.	EXTRAGALACTIC COMPACT SOURCES	7	C	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702076010/	Quick Look
513	1H 0419-577	66.5658	-57.2343	66.322649	-57.345613	29.362681	-75.708089	267.01881665	-41.95465908	226.9739	55212.4834259259	2010-01-16 11:36:08	55214.8224421296	2010-01-18 19:44:19	704064010	122.8354	140	123.1154	122.8354	0	123.1154	2	2	0	2	1	0	0	113.4392	113.4392	202.0668	4	PROCESSED	57550.2328472222	2016-06-11 05:35:18	55594	2011-02-02 00:00:00	55228.2152893518	2010-02-01 05:10:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041417	A 'hard excess' has been detected in 2007 Suzaku PIN data for the nearby quasar 1H 0419-577 relative to models fitting below 10 keV. The excess can be accounted for with Compton-thick partial-covering gas probably part of a clumpy disk wind originating inside of the BLR. The observed Fe Ka line luminosity is consistent with an origin in an equatorial wind. Blurred reflection models cannot satisfactorily fit the source and so 1H0419-577 provides a rare distinction between two observationally-similar classes of model. We propose two 140 ks follow-up Suzaku observations separated by months to probe the properties of the Compton-thick gas via variability measurements: this is an important new science area that can only be studied using the broad bandpass available from Suzaku.	EXTRAGALACTIC COMPACT SOURCES	7	C	TRACEY TURNER		USA	4	AO4	STUDYING THE COMPTON-THICK PARTIAL-COVERING ABSORPTION IN 1H 0419-577	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704064010/	Quick Look
514	3C 105	61.8399	3.6518	61.183972	3.519003	60.504157	-16.952891	187.66746701	-33.63397375	251.3728	54501.5363078704	2008-02-05 12:52:17	54503.0833912037	2008-02-07 02:00:05	702074010	38.319	53	38.319	38.319	0	38.319	2	2	0	2	1	0	0	48.8811	48.8811	133.6558	2	PROCESSED	57541.5364351852	2016-06-02 12:52:28	54883	2009-02-21 00:00:00	54515.7678819444	2008-02-19 18:25:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021372	The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702074010/	Quick Look
515	ESO 263-G013	152.4256	-42.8603	151.905124	-42.614062	176.412344	-49.376708	273.99206854	10.74227458	292.0779	54252.4568287037	2007-06-01 10:57:50	54253.5946064815	2007-06-02 14:16:14	702120010	45.2947	40	45.3027	45.3027	0	45.2947	2	2	0	2	1	0	0	40.1035	40.1035	98.2999	2	PROCESSED	57538.8009143518	2016-05-30 19:13:19	54745	2008-10-06 00:00:00	54258.5006134259	2007-06-07 12:00:53	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022033	The high-energy detectors onboard Swift and INTEGRAL are mapping the hard (>10 keV) X-ray sky. Although limited to bright X-ray fluxes (~1e-11 erg/cm2/s), the large area surveyed so far has allowed to build up sizable samples of hard X-ray selected AGN almost unbiased against X-ray absorption. On the basis of a careful analysis of the available X-ray observations below 10 keV, we identified a sample of relatively bright AGN which are likely to be obscured by Compton-thick (logN_H >24) cold gas. Two of them were observed in EAO-1 and the results confirmed our predictions. We propose further Suzaku observations of 3 bright objects (F(20-40 keV) ~ 0.7-1.4 x 1e-11 erg/cm2/s) which will allow us to unveil previously unknown nearby heavily obscured AGN.	EXTRAGALACTIC COMPACT SOURCES	7	B	ANDREA COMASTRI		EUR	2	AO2	BRIGHT COMPTON-THICK GALAXIES IN THE BACKYARD - PART II	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702120010/	Quick Look
516	NGC 7469	345.7842	8.9301	345.154297	8.660604	350.460681	13.82437	83.10914575	-45.403242	63.4793	54641.7015856482	2008-06-24 16:50:17	54644.683599537	2008-06-27 16:24:23	703028010	112.1128	100	112.1251	112.1331	0	112.1128	2	2	0	2	1	0	0	91.5571	91.5571	257.6126	2	PROCESSED	57542.968125	2016-06-03 23:14:06	55027	2009-07-15 00:00:00	54658.7891319444	2008-07-11 18:56:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031311	We propose a 100 ksec observation of the X-ray bright Seyfert 1 AGN NGC 7469, a strong candidate for having ionized reflection from the accretion disk. Only the broad bandpass provided by Suzaku, including >12 keV coverage via the HXD, will allow us to deconvolve the broadband emitting components, including the strong Compton reflection hump, broad Fe K line, and soft excess. With the XIS, we will study in detail the Fe K emission complex, including the narrow 6.4 keV Fe K core and in particular the prominent ``blue wing'' near 6.9 keV. Our proposed observation will thus be an example of how broad bandpass X-ray observations can critically test blurred, ionized disk reflection model in Seyfert 1s.	EXTRAGALACTIC COMPACT SOURCES	7	B	ALEX MARKOWITZ		USA	3	AO3	IONIZED DISK REFLECTION IN THE SEYFERT AGN NGC 7469	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703028010/	Quick Look
517	IRAS 12072-0444	182.4393	-5.0116	181.797769	-4.733385	184.228917	-3.627834	283.97337665	56.31820605	111.9489	55534.0444328704	2010-12-04 01:03:59	55535.5169328704	2010-12-05 12:24:23	705045010	61.9339	60	61.9419	61.9419	0	61.9339	2	2	0	2	1	0	0	28.1596	28.1596	127.206	0	PROCESSED	57554.3475810185	2016-06-15 08:20:31	55910	2011-12-15 00:00:00	55544.3011226852	2010-12-14 07:13:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051441	We propose two Suzaku-HXD observations of two ULIRGs hosting a deeply buried AGN. These two objects are expected to host a powerful AGN in the luminosity range of quasars, based on solid evidence from mid-IR Spitzer spectroscopy. However, these sources are completely buried behind a screen of dust with column density in excess of 10^24 cm^-2, so not only the primary emission below 10 keV is obscured, but the reflected emission, usually ascribed to a circumnuclear "torus", is also absent. This suggests a complete spherical coverage of the X-ray source along all directions. The unique capabilities of Suzaku at high energies will allow to confirm the existence of these objects, representing the most extreme examples of buried AGNs, both in terms of obscuration and of intrinsic luminosity.	EXTRAGALACTIC COMPACT SOURCES	7	C	GUIDO RISALITI		USA	5	AO5	BURIED QUASAR 2S INSIDE ULIRGS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705045010/	Quick Look
518	NGC 6814	295.6733	-10.3371	294.986368	-10.456223	295.709061	10.841132	29.34034439	-16.02176478	260.0004	55867.6992013889	2011-11-02 16:46:51	55868.637662037	2011-11-03 15:18:14	706032010	42.12	40	42.1435	42.136	0	42.12	2	2	0	2	1	0	0	40.0918	40.0918	81.0698	1	PROCESSED	57603.6893518518	2016-08-03 16:32:40	56248	2012-11-17 00:00:00	55881.0746527778	2011-11-16 01:47:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061411	Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASAAKI HAYASHIDA		USA	6	AO6	SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706032010/	Quick Look

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