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 181

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	4U 1820-30	275.9251	-30.4172	275.121541	-30.443999	275.136917	-7.082068	2.74021083	-7.94370371	265.2009	55111.1096643518	2009-10-07 02:37:55	55111.700162037	2009-10-07 16:48:14	404069050	21.7674	20	21.7674	21.7674	0	21.7674	1	1	0	1	1	0	0	15.6743	15.6743	51.0039	0	PROCESSED	57548.7799884259	2016-06-09 18:43:11	55496	2010-10-27 00:00:00	55127.2938194445	2009-10-23 07:03:06	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069050/	Quick Look
3	GX 9+9	262.9404	-16.8929	262.215892	-16.856936	263.194726	6.381396	8.57505694	9.06920034	97.5329	55271.6738773148	2010-03-16 16:10:23	55273.9918981482	2010-03-18 23:48:20	404071010	85.1871	75	85.2087	85.2031	0	85.1871	2	1	0	2	1	0	0	61.6942	61.6942	200.2639	0	PROCESSED	57550.9767476852	2016-06-11 23:26:31	55652	2011-04-01 00:00:00	55285.4179513889	2010-03-30 10:01:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042011	We propose two 75 ks Suzaku observations of the bright neutron star low mass X-ray binary (LMXB) GX9+9, spread over six months. We will investigate the presence of X-ray narrow absorption features in the Suzaku spectra, which are a signature of a disk wind. Such features, identified with ions such as Fe XXV and Fe XXVI, have been observed in a number of LMXBs and give us information about the mass outflow rate and the launching mechanism of the wind. We will study the connection of the disk wind to the presence of radio jet emission with simultaneous radio observations. Finally, we will determine if the broad Fe emission line indicated by the XMM-Newton spectrum is relativistically broadened. Variability will be studied as a function of accretion rate in the two proposed observations.	GALACTIC POINT SOURCES	4	B	MARIA DIAZ TRIGO		EUR	4	AO4	A STUDY OF THE DISK WIND-JET CONNECTION IN GX9+9 WITH MULTIWAVELENGTH OBSERVATIONS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404071010/	Quick Look
4	G54.1+0.3	292.6593	18.8091	292.105949	18.703083	298.434306	40.039537	54.05763723	0.20765467	245.096	54403.6644560185	2007-10-30 15:56:49	54406.3335532407	2007-11-02 08:00:19	502077010	101.6411	100	101.6411	101.6491	0	101.6491	2	2	0	2	1	0	0	92.9235	92.9235	230.5857	3	PROCESSED	57540.4530324074	2016-06-01 10:52:22	54786	2008-11-16 00:00:00	54417.8870833333	2007-11-13 21:17:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022032	A proprietary XMM-Newton observation reveals that the pulsar wind nebula G54.1+0.3 has a very hard spectrum (gamma ~ 1.5) and possibly a break between 5 and 10 keV. We propose a 100 ks SUZAKU observation to confirm unambiguously the presence of the break. If confirmed, the break would pose stringent constraints on models of electron emission and propagation in pulsar wind nebulae.	GALACTIC DIFFUSE EMISSION	5	C	FABRIZIO BOCCHINO		EUR	2	AO2	THE BREAK IN THE HARD X-RAY ENERGY OF THE PULSAR WIND NEBULA G54.1+0.3	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502077010/	Quick Look
5	HER X-1	254.4632	35.2657	254.012163	35.341297	246.023504	57.418254	58.05457552	37.50615868	268.4858	55461.0002083333	2010-09-22 00:00:18	55461.4494675926	2010-09-22 10:47:14	405058030	19.924	20	19.924	19.924	0	20.2438	2	2	0	1	1	0	0	17.5073	17.5073	38.8119	0	PROCESSED	57553.4994560185	2016-06-14 11:59:13	55836	2011-10-02 00:00:00	55470.1508796296	2010-10-01 03:37:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052001	We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity?	GALACTIC POINT SOURCES	4	B	R DIGER STAUBERT		EUR	5	AO5	VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405058030/	Quick Look
6	GX 339-4	255.7015	-48.7852	254.753736	-48.714186	259.571673	-25.859287	338.94105133	-4.32146688	83.6944	55603.7634722222	2011-02-11 18:19:24	55604.2349421296	2011-02-12 05:38:19	405063010	22.4594	100	22.4594	22.4594	0	22.4834	2	2	0	2	1	0	0	19.3287	19.3287	40.7279	0	PROCESSED	57600.9244675926	2016-07-31 22:11:14	55983	2012-02-26 00:00:00	55617.4120601852	2011-02-25 09:53:22	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052015	We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4	GALACTIC POINT SOURCES	4	A	CLEMENT CABANAC		EUR	5	AO5-TOO	PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063010/	Quick Look
7	GX 339-4	255.7013	-48.7848	254.753541	-48.713785	259.571479	-25.858904	338.94128957	-4.32111913	86.3597	55608.9686111111	2011-02-16 23:14:48	55609.6501967593	2011-02-17 15:36:17	405063020	21.0157	20	21.0157	21.0157	0	21.0157	2	2	0	2	1	0	0	17.5958	17.5958	58.8839	0	PROCESSED	57600.9613773148	2016-07-31 23:04:23	55988	2012-03-02 00:00:00	55621.1561342593	2011-03-01 03:44:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052015	We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4	GALACTIC POINT SOURCES	4	A	CLEMENT CABANAC		EUR	5	AO5-TOO	PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063020/	Quick Look
8	GX 339-4	255.7016	-48.7831	254.753859	-48.712086	259.571491	-25.857192	338.94276391	-4.32024293	90.1024	55616.8233680556	2011-02-24 19:45:39	55617.4487268518	2011-02-25 10:46:10	405063030	19.182	20	19.19	19.198	0	19.182	2	2	0	2	1	0	0	15.684	15.684	54.0259	1	PROCESSED	57601.0471180556	2016-08-01 01:07:51	55996	2012-03-10 00:00:00	55628.1679976852	2011-03-08 04:01:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052015	We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4	GALACTIC POINT SOURCES	4	A	CLEMENT CABANAC		EUR	5	AO5-TOO	PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063030/	Quick Look
9	GX 17+2	274.0108	-14.0482	273.300467	-14.065956	273.933278	9.337698	16.42401351	1.2676957	264.7715	55853.116099537	2011-10-19 02:47:11	55855.5287037037	2011-10-21 12:41:20	406070010	6.5069	100	6.7572	6.5069	0	6.7572	3	2	0	2	1	0	0	87.3599	87.3599	208.4297	3	PROCESSED	57603.5270023148	2016-08-03 12:38:53	56241	2012-11-10 00:00:00	55873.2944444445	2011-11-08 07:04:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062003	The behaviour of dense matter in neutron stars remains enigmatic. To probe this requires accurate measurements of neutron star radii and masses. We have recently shown that broad relativistic Fe emission lines in neutron star low-mass X-ray binaries can be used to constrain the neutron star radius. These sources also provide another tool, kHz quasi-periodic oscillations (QPOs). Combining a measurement of the velocity of the gas in the inner disk (from the Fe line) and the frequency of the kHz QPOs provides a method to measure the neutron star mass if kHz QPOs originate at the inner disk. We propose 100 ksec observations of GX 349+2 and GX 17+2 to provide a detailed Fe line profile. Simultaneously, we will also observe with RXTE to detect the kHz QPOs, allowing us to test this technique.	GALACTIC POINT SOURCES	4	A	EDWARD CACKETT		EUR	6	AO6	EXPLORING THE IRON LINE - KHZ QPO CONNECTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406070010/	Quick Look
10	4U 0352+30	58.8427	31.0494	58.059686	30.903757	63.208913	10.461571	163.07655547	-17.13553633	77.7002	56166.360150463	2012-08-27 08:38:37	56170.0980208333	2012-08-31 02:21:09	407088010	153.4893	150	153.4893	153.4893	0	153.4893	2	2	0	2	1	0	0	140.9919	140.9919	322.9236	3	PROCESSED	57607.0637268518	2016-08-07 01:31:46	56582	2013-10-17 00:00:00	56212.7609722222	2012-10-12 18:15:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072011	After 40 years of studies, surprisingly little is known about accreting pulsars at low-luminosities, yet these may be the most numerous class of neutron star binaries in the Galaxy. Upcoming large-scale surveys will likely reveal many such objects, but to identify them it is crucial to fully understand their properties. X Per, the archetypal source of this class, at 1 kpc from Earth is ideal target for detailed studies. In spite of that X Per is still puzzling. With the proposed program we aim to study X Per in detail, constrain its X-ray spectrum also as a function of the spin phase. Our study will be key to characterize the properties of low-luminosity X-ray pulsars population and will help to identify it in upcoming surveys.	GALACTIC POINT SOURCES	4	B	VICTOR DOROSHENKO		EUR	7	AO7	CRACKING THE X PER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407088010/	Quick Look
11	J1522-5734	230.5286	-57.5816	229.552952	-57.402737	244.521376	-37.577548	322.05619938	-0.4156844	274.4971	56154.6486342593	2012-08-15 15:34:02	56155.0078356482	2012-08-16 00:11:17	407094010	30.0295	25	30.0455	30.0295	0	30.0455	1	1	0	1	1	0	0	23.6862	23.6862	31.0239	0	PROCESSED	57606.8538194444	2016-08-06 20:29:30	56638	2013-12-12 00:00:00	56272.6647222222	2012-12-11 15:57:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072019	The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances.	GALACTIC POINT SOURCES	4	A	MARTINO MARELLI		EUR	7	AO7	SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407094010/	Quick Look
12	RBS1066	181.3063	39.3578	180.66961	39.636099	163.015077	36.071469	158.19944471	74.44309108	133.5252	56973.6795486111	2014-11-12 16:18:33	56973.8890277778	2014-11-12 21:20:12	809105010	10.2376	12	10.2376	10.5256	0	10.5256	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7665509259	2016-08-16 18:23:50	57358	2015-12-02 00:00:00	56992.4200810185	2014-12-01 10:04:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809105010/	Quick Look
13	H 1743+322	266.5667	-32.234	265.750828	-32.215343	267.051923	-8.827937	357.25546218	-1.83442728	271.9807	56924.2942476852	2014-09-24 07:03:43	56927.2779861111	2014-09-27 06:40:18	409059010	119.0885	100	119.0885	119.0965	0	119.5626	3	2	0	1	0	0	0	0	0	0	0	PROCESSED	57616.6267361111	2016-08-16 15:02:30	57310	2015-10-15 00:00:00	56940.6644560185	2014-10-10 15:56:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092020	We propose a triggered Suzaku 100 ks observation of a high-inclination Galactic black hole binary in the hard intermediate state. This will be simultaneous with an already accepted XMM-Newton observation (PI: A. Ingram) to test the Lense-Thirring model for the low frequency quasi-periodic oscillations seen in black hole (and neutron star) binaries. The Suzaku PIN data will enable us to extend the energy range over which the QPO can be studied, allowing us to get much better constraints on the reflection component in the QPO spectrum, and hence to more tightly probe the geometry and emission processes in the regions closest to the black hole.	GALACTIC POINT SOURCES	4	A	MAGNUS AXELSSON		EUR	9	AO9-TOO	TESTING THE LENSE-THIRRING ORIGIN OF THE LOW FREQUENCY QPO IN BLACK HOLE BINARIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409059010/	Quick Look
14	ABELL2244	255.6885	34.0502	255.230084	34.120069	248.255538	56.413781	56.77689495	36.30222985	232.8204	54392.7992013889	2007-10-19 19:10:51	54394.3959953704	2007-10-21 09:30:14	802078010	71.3811	63	71.3891	71.3971	0	71.3811	2	2	0	2	1	0	0	69.1077	69.1077	137.9498	3	PROCESSED	57540.332337963	2016-06-01 07:58:34	54771	2008-11-01 00:00:00	54403.2516666667	2007-10-30 06:02:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022036	In order to use clusters as cosmological probes, accurate mass determinations are needed. The ICM is an ideal candidate since it provides a map of the DM potential. Measuring the gas properties to the virial radius is imperative for determining the proper cluster mass, since a large part of the cluster mass resides beyond 1/2 r_vir. Current discrepancies in outer cluster kT profiles are due to large uncertainties due to the high background in Chandra and XMM-Newton. With its lower background, Suzaku is able to make this measurement. We propose a 50 ks observation of A2244. A2244 is an ideal candidate to make this measurement; at a redshift of z~0.1, the virial radius can be fit inside Suzaku's field of view, moreover A2244 is an unusual example of a relaxed cluster without a cool core.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DANIEL HUDSON		EUR	2	AO2	A2244 - MEASURING CLUSTER GAS TEMPERATURE TO THE VIRIAL RADIUS IN A RELAXED ISOTHERMAL CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802078010/	Quick Look
15	4U 1820-30	275.9218	-30.4206	275.118218	-30.447383	275.13391	-7.085348	2.73584989	-7.94270191	269.3964	55116.6321064815	2009-10-12 15:10:14	55117.1759143518	2009-10-13 04:13:19	404069060	24.6687	100	0	24.6687	0	24.6687	0	1	0	2	1	0	0	16.9505	16.9505	46.978	0	PROCESSED	57548.8754861111	2016-06-09 21:00:42	55507	2010-11-07 00:00:00	55131.3693518518	2009-10-27 08:51:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069060/	Quick Look
16	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
17	J1620-4927	245.1748	-49.4572	244.240353	-49.338216	252.062857	-27.548671	333.89109656	0.40900491	274.3002	56157.8029513889	2012-08-18 19:16:15	56158.5203356482	2012-08-19 12:29:17	407091010	29.2601	25	29.2601	29.2841	0	29.2601	1	1	0	1	1	0	0	29.8402	29.8402	61.9679	0	PROCESSED	57606.8716898148	2016-08-06 20:55:14	56592	2013-10-27 00:00:00	56226.6098148148	2012-10-26 14:38:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072019	The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances.	GALACTIC POINT SOURCES	4	A	MARTINO MARELLI		EUR	7	AO7	SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407091010/	Quick Look
18	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
19	GT MUS	174.8799	-65.348	174.296149	-65.070756	218.231345	-58.061728	295.52044001	-3.51633969	94.8564	54446.4736689815	2007-12-12 11:22:05	54449.187662037	2007-12-15 04:30:14	402095010	93.3087	80	93.3087	93.3087	0	93.3087	2	2	0	2	1	0	0	94.6965	94.6965	234.4699	3	PROCESSED	57540.9318287037	2016-06-01 22:21:50	54828	2008-12-28 00:00:00	54460.7707060185	2007-12-26 18:29:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022020	We propose to perform broad-band X-ray spectroscopy of the RS CVn-like system GT Muscae, with the aim to study the thermal and non-thermal components of its X-ray emitting plasma. Our target is a known hard X-ray source, detected with Uhuru and recently with Integral/IBIS in the 20-40 keV band, but lacking a dedicated observation with modern X-ray spectrometers. The proposed observation will allow us to investigate both the quiescent and flaring states of this complex (possibly interacting) binary system, by means of a variability study and a time-resolved spectral analysis of its X-ray emission. We aim to detect and constrain the non-thermal hard X-ray emission component, and to search for a possible Fe Kalpha line emission, thanks to the superb broad-band spectral capabilities of Suzaku.	GALACTIC POINT SOURCES	4	B	ANTONIO MAGGIO		EUR	2	AO2	BROAD-BAND X-RAY SPECTROSCOPY OF AN EXTREMELY ACTIVE CORONAL SOURCE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402095010/	Quick Look
20	A3526	191.1432	-39.6142	190.459557	-39.340673	207.301582	-31.717062	301.49310157	23.23836897	110.0059	55944.2688078704	2012-01-18 06:27:05	55944.754375	2012-01-18 18:06:18	806090010	18.3702	16	18.3782	18.3702	0	18.3857	2	2	0	2	1	0	0	14.795	14.795	41.9499	2	PROCESSED	57604.405775463	2016-08-04 09:44:19	56352	2013-03-01 00:00:00	55985.1138310185	2012-02-28 02:43:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806090010/	Quick Look
21	J2218.8-0258	334.694	-2.9598	334.046783	-3.210826	335.453457	7.033577	59.75779093	-46.24852305	49.9996	56072.7972685185	2012-05-25 19:08:04	56073.7370833333	2012-05-26 17:41:24	807086010	38.3981	35	38.4061	38.3981	0	38.4061	2	2	0	2	1	0	0	36.9739	36.9739	81.1958	1	PROCESSED	57605.5228703704	2016-08-05 12:32:56	56500	2013-07-27 00:00:00	56134.0402199074	2012-07-26 00:57:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072018	We propose to observe the three clusters of galaxies J2218.2-0350, J2218.6-0346 and J2218.8-0258 with exposure times of 15, 25 and 35 ks respectively. These clusters are part of a structure of four linearly aligned clusters, separated from each other by 4 to 10 Mpc. We will accurately determine their masses and orientation. This will allow us to fully map the tidal force field of the structure, which is the prime force behind the formation of filaments in the cosmic web. We will study the effects of cluster mass, separation and mutual orientation on the filamentary structure of the cosmic web and on the evolution of galaxies therein.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	E.G. PATRICK BOS		EUR	7	AO7	CLUSTERS AND THE COSMIC WEB	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807086010/	Quick Look
22	HESS J1731-347	263.0179	-34.7706	262.185573	-34.73474	264.142481	-11.47104	353.53173388	-0.68198005	79.8005	54154.7807060185	2007-02-23 18:44:13	54155.7432291667	2007-02-24 17:50:15	401099010	40.6189	38	40.6269	40.6189	0	40.6269	2	2	0	2	1	0	0	34.6479	34.6479	83.1559	0	PROCESSED	57537.4739351852	2016-05-29 11:22:28	54528	2008-03-03 00:00:00	54160.3931944444	2007-03-01 09:26:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012042	The hard (Gamma=2.0) TeV source HESS J1731-347 discovered in the H.E.S.S. Galactic plane survey has an intriguing possible counterpart seen in ROSAT survey data. The X-ray data show an unidentified, extended nebular structure with a hard spectrum, in close coincidence to the TeV source. It is plausible to assume that the same energetic particle population is responsible for the emission in both bands. Suzaku is optimally suited to establish the likely non-thermal nature of the X-ray spectrum and to search for the high-energy end of the emitting particle spectrum, which is likely visible in the HXD domain. The observations will help to clarify the nature of HESS J1731-347, which may be a new type of Galactic particle accelerator.	GALACTIC POINT SOURCES	4	A	GERD PUEHLHOFER		EUR	1	AO1	THE HIGH ENERGY PARTICLE SPECTRUM OF THE TEV/X-RAY NEBULA HESS J1731-347	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401099010/	Quick Look
23	SU AUR	73.9934	30.5715	73.195309	30.492884	76.133121	7.898373	172.51103259	-7.93275707	85.9197	54339.1713541667	2007-08-27 04:06:45	54340.7502199074	2007-08-28 18:00:19	402090010	57.3034	55	57.3114	57.3034	0	57.3114	2	2	0	2	1	0	0	54.3848	54.3848	136.4018	1	PROCESSED	57539.9114699074	2016-05-31 21:52:31	54723	2008-09-14 00:00:00	54350.6381597222	2007-09-07 15:18:57	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022007	We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra.	GALACTIC POINT SOURCES	4	A	JURGEN SCHMITT		EUR	2	AO2	ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402090010/	Quick Look
24	XTE J1759-220	269.9393	-22.0118	269.18599	-22.009675	269.934127	1.429042	7.5831003	0.77858469	86.479	54566.5188773148	2008-04-10 12:27:11	54567.6460532407	2008-04-11 15:30:19	403072010	48.961	50	49.361	49.425	0	48.961	2	2	0	2	1	0	0	43.9129	43.9129	97.3639	1	PROCESSED	57542.2983912037	2016-06-03 07:09:41	54953	2009-05-02 00:00:00	54580.4766550926	2008-04-24 11:26:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032012	Dipping low-mass X-ray binaries (LMXBs), a subclass of LMXBs that are viewed close to the disk plane, provide us with a rare opportunity to probe the structure of accretion disks. This was nicely illustrated with the discovery of Fe XXV and Fe XXVI absorption lines in all the dipping LMXBs observed with XMM and Chandra. It revealed the existence of a highly-ionized atmosphere above the disk which is likely present in any LMXB but only detectable in the ones seen close to edge-on. We propose to observe two recently discovered dipping binaries with Suzaku, to constrain the basic astrophysical properties (orbital period, distance, variability, high energy cutoff, etc) of these yet poorly observed sources, and to further investigate the ionized atmosphere in X-ray binaries in general.	GALACTIC POINT SOURCES	4	B	LAURENCE BOIRIN		EUR	3	AO3	NEW DIPPING X-RAY BINARIES TO PROBE ACCRETION DISKS AND THEIR IONIZED ATMOSPHER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403072010/	Quick Look
25	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
26	4U 1820-30	275.9248	-30.4209	275.121217	-30.447698	275.136502	-7.085754	2.73676025	-7.94514519	265.9319	55088.3645833333	2009-09-14 08:45:00	55088.8141087963	2009-09-14 19:32:19	404069020	21.0373	20	21.0373	21.0373	0	21.0373	1	1	0	1	1	0	0	17.17	17.17	38.8319	0	PROCESSED	57548.569837963	2016-06-09 13:40:34	55469	2010-09-30 00:00:00	55103.4457407407	2009-09-29 10:41:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069020/	Quick Look
27	10 LAC	339.8111	39.0619	339.249017	38.801118	0.373962	43.220063	96.65409432	-16.97165842	81.7456	55344.5001967593	2010-05-28 12:00:17	55345.0690162037	2010-05-29 01:39:23	405060010	25.0284	25	25.0284	25.0284	0	25.0284	2	2	0	2	1	0	0	21.7431	21.7431	49.1359	2	PROCESSED	57551.6393287037	2016-06-12 15:20:38	55731	2011-06-19 00:00:00	55365.1824305556	2010-06-18 04:22:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052005	We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models.	GALACTIC POINT SOURCES	4	A	LIDIA OSKINOVA		EUR	5	AO5	STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405060010/	Quick Look
28	EXO 2030+375	308.0462	37.6555	307.574628	37.484842	325.998165	53.954312	77.15821576	-1.21997822	58.3113	56070.8420717593	2012-05-23 20:12:35	56072.789849537	2012-05-25 18:57:23	407089010	77.9451	75	77.9531	77.9569	0	77.9451	2	1	0	2	1	0	0	72.515	72.515	168.2558	0	PROCESSED	57605.5425347222	2016-08-05 13:01:15	56449	2013-06-06 00:00:00	56083.2088888889	2012-06-05 05:00:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072013	We propose to observe the Be/X-ray binary system EXO 2030+375 in the ascending part of one of its normal periastron flares for 75ks to study the onset of the pulsar activity. Quasi-periodic hour-long flux oscillations were recently observed during INTEGRAL serendipitous observations and by EXOSAT in 1985. They appear to happen at the viscous time-scale of a disk, evidencing some kind of instability in the transition zone between the magnetosphere and the accretion disk. The broad-band coverage and sensitivity of Suzaku will allow us to investigate in detail the opening of the magnetic gate for this high-magnetic field neutron star by studying the high time resolution light curve, the shape of its pulsed signal and the spectral properties.	GALACTIC POINT SOURCES	4	A	CARLO FERRIGNO		EUR	7	AO7	UNVEIL ACCRETION ONSET DURING A NORMAL OUTBURST OF EXO 2030+375	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407089010/	Quick Look
29	CPD-28 2561	118.9748	-28.6234	118.467111	-28.489607	129.605392	-48.156505	245.44211654	-0.09136967	288.1635	56775.1365509259	2014-04-28 03:16:38	56775.9174768518	2014-04-28 22:01:10	409055010	26.9471	25	26.9471	26.9551	0	26.9631	2	2	0	2	1	0	0	23.1261	23.1261	67.4619	0	PROCESSED	57615.0079513889	2016-08-15 00:11:27	57214	2015-07-11 00:00:00	56848.6257638889	2014-07-10 15:01:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092005	We propose SUZAKU observations of the representative members of the class of magnetic massive O-type stars. The targets have measured magnetic fields and belong to similar spectral types. SUZAKU data will allow to compare the X-ray spectra of these objects that have similar stellar and wind parameters yet different magnetospheres. These observations will result in the first firm X-ray detections of our target stars. The analysis of XIS spectra will determine the emission measures and the temperatures of the hot gas. Our careful selection of targets will allow us to study the interplay between magnetic fields and stellar winds in O-type stars. These new observations for a comparative analysis of a homogeneous class of objects will be critical for driving the development of the theory.	GALACTIC POINT SOURCES	4	B	LIDIA OSKINOVA		EUR	9	AO9	COMPARATIVE STUDY OF MAGNETIC O-TYPE STARS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409055010/	Quick Look
30	HESS J1718-385	259.5512	-38.6075	258.69231	-38.554942	261.534502	-15.472357	348.79652534	-0.53531102	91.2393	54154.3587731482	2007-02-23 08:36:38	54154.7773611111	2007-02-23 18:39:24	501105010	20.744	19	20.744	20.744	0	20.744	1	1	0	1	1	0	0	15.8365	15.8365	36.1519	0	PROCESSED	57537.4491435185	2016-05-29 10:46:46	54527	2008-03-02 00:00:00	54158.2865740741	2007-02-27 06:52:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012044	HESS J1718-385 is a newly discovered TeV gamma-ray source, with an unusually hard energy spectrum, which lies in close proximity to an energetic pulsar. It is likely that this object belongs to the class of offset pulsar wind nebula (PWN), accelerating electrons and positrons up to ~100 TeV. So far no sensitive X-ray observations of this region have taken place. The synchrotron spectrum of the nebula is predicted to peak in the energy range of the Suzaku HXD. The unprecedented high energy sensitivity of this instrument is required to study the highest energy particles accelerated in this object. Spectral measurements by Suzaku would confirm the inverse-Compton origin of the VHE gamma-rays and place tight constraints on the maximum energy of accelerated electrons.	GALACTIC DIFFUSE EMISSION	5	A	JAMES HINTON		EUR	1	AO1	PROBING THE LIMITS OF PARTICLE ACCELERATION IN A NEW HARD SPECTRUM TEV GAMMA-RAY SOURCE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501105010/	Quick Look
31	AX J1714.1-3912	258.5249	-39.1972	257.66219	-39.139743	260.755226	-16.122974	347.85266774	-0.22742448	85.6964	55608.0538078704	2011-02-16 01:17:29	55608.9654050926	2011-02-16 23:10:11	505076010	32.6017	30	32.6017	32.6017	0	32.6017	2	2	0	2	1	0	0	28.3362	28.3362	78.7579	1	PROCESSED	57600.9625115741	2016-07-31 23:06:01	55988	2012-03-02 00:00:00	55621.1409027778	2011-03-01 03:22:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052012	Molecular clouds are predicted to emit strong non-thermal X-rays when they are close to particle-accelerating SNRs, but this emission has not been confirmed yet. We propose to observe the non-thermal X-ray source AX J1714.1-3912 to investigate its relationship with the SNR RX J1713.7-3946. ASCA observations have shown that the hard spectrum of the source may be associated with bremsstrahlung emission from particles accelerated in the SNR and diffusing in a nearby molecular cloud. This emission has never been observed in other SNRs. However, the association of the source with the remnant is still controversial and the ASCA data do not allow us to constrain the spectral properties. We aim at verifying the association with the remnant and at investigating the physical origin of the emission.	GALACTIC DIFFUSE EMISSION	5	A	MARCO MICELI		EUR	5	AO5	INVESTIGATING THE PHYSICAL ORIGIN OF AX J1714.1-3912	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505076010/	Quick Look
32	G7.6+2.0	268.7973	-21.391	268.047539	-21.383335	268.869887	2.045161	7.58937554	2.00788461	270.4016	56194.0843865741	2012-09-24 02:01:31	56194.4237037037	2012-09-24 10:10:08	507065010	16.521	10	16.529	16.521	0	16.5347	2	2	0	2	1	0	0	12.1603	12.1603	29.3139	2	PROCESSED	57607.1654050926	2016-08-07 03:58:11	56676	2014-01-19 00:00:00	56315.5110069444	2013-01-23 12:15:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072014	We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed.	GALACTIC DIFFUSE EMISSION	5	A	TOBIAS PRINZ		EUR	7	AO7	IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507065010/	Quick Look
33	3C400.2 SE	294.8215	17.1213	294.25847	17.005668	300.577132	37.964226	53.58084569	-2.4098547	81.5889	56770.9416898148	2014-04-23 22:36:02	56771.4758449074	2014-04-24 11:25:13	509070010	24.9467	20	24.9547	24.9467	0	24.9627	1	1	0	1	1	0	0	22.7494	22.7494	46.1359	0	PROCESSED	57614.9903009259	2016-08-14 23:46:02	57152	2015-05-10 00:00:00	56789.6293865741	2014-05-12 15:06:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092010	Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances.	GALACTIC DIFFUSE EMISSION	5	A	JACCO VINK		EUR	9	AO9	THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509070010/	Quick Look
34	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
35	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
36	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
37	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
38	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
39	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
40	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
41	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
42	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
43	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
44	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
45	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
46	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
47	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
48	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
49	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
50	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
51	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
52	A3526	191.7105	-40.5689	191.023079	-40.2959	208.274178	-32.365083	301.98862911	22.29443097	109.9992	55942.9777314815	2012-01-16 23:27:56	55943.2362847222	2012-01-17 05:40:15	806086010	13.6391	12	13.6471	13.6471	0	13.6391	1	1	0	1	1	0	0	11.41	11.41	22.3279	0	PROCESSED	57604.3734606482	2016-08-04 08:57:47	56352	2013-03-01 00:00:00	55985.0806944444	2012-02-28 01:56:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806086010/	Quick Look
53	A2877-NORTH	17.5135	-45.1865	16.956259	-45.452478	352.566996	-47.330769	292.51418745	-71.56330592	266.5006	56649.9225810185	2013-12-23 22:08:31	56651.7884027778	2013-12-25 18:55:18	808102010	72.629	70	72.637	72.629	0	72.645	2	2	0	2	1	0	0	69.2641	69.2641	161.1857	0	PROCESSED	57613.7012615741	2016-08-13 16:49:49	57033	2015-01-11 00:00:00	56665.7969097222	2014-01-08 19:07:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082014	We propose to observe the galaxy group A2877 for a combine observation time of 150 ks, with two different pointings. The aim of the project is to obtain temperature and surface brightness profiles out to large radii to constrain entropies. We aim to see if the entropy profile flattens at large radii, which could indicate gas clumping and/or other processes. This would possibly be the first unrelaxed galaxy group whose entropy profile would have been studied in the outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	BHARADWAJ VIJAYSARATHY		EUR	8	AO8	INVESTIGATING THE OUTSKIRTS OF THE UNRELAXED GALAXY GROUP A2877	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808102010/	Quick Look
54	IC1262	263.2444	43.7719	262.868526	43.80553	257.468416	66.917452	69.53148075	32.08557503	39.6325	56784.7266319444	2014-05-07 17:26:21	56784.9377777778	2014-05-07 22:30:24	809103010	8.569	10	8.569	8.569	0	8.569	1	1	0	1	1	0	0	8.943	8.943	18.2319	0	PROCESSED	57615.0791898148	2016-08-15 01:54:02	57166	2015-05-24 00:00:00	56800.6274537037	2014-05-23 15:03:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809103010/	Quick Look
55	NGC 7556	348.9407	-2.3789	348.297581	-2.651844	348.895625	2.187169	76.06549974	-56.282291	247.7522	56983.6865972222	2014-11-22 16:28:42	56984.009837963	2014-11-23 00:14:10	809109010	15.119	15	15.119	15.119	0	15.119	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.8029861111	2016-08-16 19:16:18	57365	2015-12-09 00:00:00	57009.4127777778	2014-12-18 09:54:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809109010/	Quick Look
56	NGC4325	185.7751	10.6242	185.139474	10.901318	181.016229	12.032879	279.57257446	72.19853871	120.2615	56997.2271990741	2014-12-06 05:27:10	56997.680775463	2014-12-06 16:20:19	809110010	17.4681	15	17.4761	17.4681	0	17.4761	1	1	0	1	1	0	0	16.8093	16.8093	39.184	0	PROCESSED	57617.4727083333	2016-08-17 11:20:42	57376	2015-12-20 00:00:00	57010.1165162037	2014-12-19 02:47:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809110010/	Quick Look
57	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
58	EXO 0748-676	117.1051	-67.7525	117.068716	-67.625708	198.866436	-79.490243	279.97237585	-19.82332654	158.0884	54459.2369560185	2007-12-25 05:41:13	54460.2919444444	2007-12-26 07:00:24	402092010	45.8988	40	45.9126	45.8988	0	45.9046	2	2	0	2	1	0	0	43.5747	43.5747	91.1358	1	PROCESSED	57540.9732175926	2016-06-01 23:21:26	54854	2009-01-23 00:00:00	54483.1839351852	2008-01-18 04:24:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022014	We propose Suzaku observations of the dipping Low Mass X-ray Binaries (LMXBs) EXO 0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the absorbers and the HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components. This will allow to reliably determine the absolute values of the ionization parameters for each of the sources, which was not possible with XMM due to the lack of contemporaneous high energy spectra, providing for a detailed comparison of the absorbers with source properties such as luminosity.	GALACTIC POINT SOURCES	4	C	MARIA DIAZ TRIGO		EUR	2	AO2	BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402092010/	Quick Look
59	ABELL 3341	81.3893	-31.5876	80.918035	-31.630439	77.271182	-54.650323	235.16288585	-31.086571	266.8997	57094.3290393518	2015-03-13 07:53:49	57094.5780092593	2015-03-13 13:52:20	809104010	11.439	10	11.439	11.439	0	11.439	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.7607407407	2016-08-17 18:15:28	57478	2016-03-31 00:00:00	57108.4097685185	2015-03-27 09:50:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809104010/	Quick Look
60	ESO 137-G034	248.7664	-58.1298	247.710529	-58.026542	256.37198	-35.687232	329.07669192	-7.11373135	296.1293	54744.462650463	2008-10-05 11:06:13	54746.6745833333	2008-10-07 16:11:24	403075010	92.0525	90	92.0613	92.0587	0	92.0525	2	2	0	2	1	0	0	83.6615	83.6615	191.0897	1	PROCESSED	57544.095775463	2016-06-05 02:17:55	55148	2009-11-13 00:00:00	54780.6031828704	2008-11-10 14:28:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032025	Suzaku observations of hard X-ray (> 15 keV) selected, bright AGN discovered by INTEGRAL and Swift have revealed several examples of previously unknown Compton Thick (NH > 1e24 cm-2) AGN in the nearby Universe. Their broad band X-ray spectra show a high degree of complexity and a wide range of the relative intensities of the various components (i.e. scattered/reflected fraction; iron line intensity, etc.). We propose a medium/deep Suzaku observation of a bright source detected by INTEGRAL above 15 keV and optically identified with a nearby Seyfert 2 galaxy. Besides the various soft X-ray components, the flat 2-10 keV spectrum and the strong (EW ~ 1 keV) iron line present in an archival XMM-Newton observation strongly suggest that the nucleus is obscured by Compton-Thick gas.	GALACTIC POINT SOURCES	4	B	ROBERTO GILLI		EUR	3	AO3	ANOTHER COMPTON-THICK AGN JUST AROUND THE CORNER	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403075010/	Quick Look
61	4U 1820-30	275.9267	-30.4234	275.123101	-30.450207	275.138047	-7.08832	2.73525617	-7.94773658	265.1815	55083.1120023148	2009-09-09 02:41:17	55083.2015740741	2009-09-09 04:50:16	404069010	3.5175	20	3.5255	3.5175	0	3.5255	1	1	0	1	1	0	0	3.7124	3.7124	7.738	0	PROCESSED	57548.5052546296	2016-06-09 12:07:34	55475	2010-10-06 00:00:00	55109.4203125	2009-10-05 10:05:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069010/	Quick Look
62	MU COL	86.4962	-32.3107	86.031401	-32.328862	84.748669	-55.688941	237.28985275	-27.10600903	93.5874	55455.752337963	2010-09-16 18:03:22	55456.3113541667	2010-09-17 07:28:21	405059010	25.961	20	25.961	25.961	0	25.961	1	1	0	1	1	0	0	21.8734	21.8734	48.2879	0	PROCESSED	57553.4381018518	2016-06-14 10:30:52	55836	2011-10-02 00:00:00	55469.2452314815	2010-09-30 05:53:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052005	We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models.	GALACTIC POINT SOURCES	4	A	LIDIA OSKINOVA		EUR	5	AO5	STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405059010/	Quick Look
63	4U 1909+07	287.7097	7.5883	287.10413	7.505006	290.320155	29.788203	41.89273161	-0.82371888	247.9131	55502.7037847222	2010-11-02 16:53:27	55503.4337731482	2010-11-03 10:24:38	405073010	29.2982	25	29.2982	29.2982	0	29.2982	2	2	0	2	1	0	0	21.3911	21.3911	63.0519	0	PROCESSED	57553.9348958333	2016-06-14 22:26:15	55882	2011-11-17 00:00:00	55515.2869328704	2010-11-15 06:53:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052024	We propose the first observation of the neutron star HMXB 4U 1909+07 with Suzaku. The aim of the proposed 25 ksec observation is to study the broadband spectrum of the source. The data will provide information about the structure and ionization state of the accreted medium, as well as of the geometry of the accretion column and the strength of the magnetic field. No high-resolution CCD spectra of this source have been published so far. The source shows flaring behavior, so the wind is expected to be strongly clumped, which could be probed by studying the evolution of N_H and the iron line with high time resolution. Furthermore we will perform phase resolved spectroscopy to study the spectral variation with pulse phase and perform a detailed search for a CRSF.	GALACTIC POINT SOURCES	4	A	FELIX FUERST		EUR	5	AO5	STUDYING ACCRETION IN THE UNCELEBRATED HMXB 4U 1909+07	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405073010/	Quick Look
64	IGR J16318-4848	247.9691	-48.8061	247.034981	-48.699533	253.953463	-26.583352	335.63186461	-0.44896472	266.5948	53961.4825	2006-08-14 11:34:48	53964.3488310185	2006-08-17 08:22:19	401094010	97.2538	100	97.2698	97.2538	97.2698	97.2698	2	2	2	2	1	0	0	87.1128	87.1128	247.6059	5	PROCESSED	57535.3483564815	2016-05-27 08:21:38	54526	2008-03-01 00:00:00	54020.9181597222	2006-10-12 22:02:09	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012034	We propose a detailed study of Compton thick X-ray absorption in neutral or weakly ionized material by using 100ksec of Suzaku observations of the strongly absorbed (N_H~2E24cm2) Galactic X-ray binary IGR J16318-4848. Measuring a high signal to noise ratio broad band spectrum will allow us to determine the curvature in the >10keV continuum caused by Compton downscattering in the absorber, to deduce its ionization state from observations of the Fe Kalpha line, and to study the variability of the source and the absorber. These observations will also shed more light onto the nature of the compact object in IGR J16318-4848.	GALACTIC POINT SOURCES	4	B	JOERN WILMS		EUR	1	AO1	OBSERVING IGR J16318-4848: PROBING COMPTON-THICK ABSORPTION	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401094010/	Quick Look
65	4U 1543-624	236.9719	-62.5774	235.885471	-62.423392	250.451121	-41.357182	321.74901084	-6.34183385	299.1939	55826.4056828704	2011-09-22 09:44:11	55827.6217592593	2011-09-23 14:55:20	406072010	49.1851	50	49.1931	49.1851	0	49.2011	2	2	0	2	1	0	0	45.3094	45.3094	105.0599	1	PROCESSED	57603.2564699074	2016-08-03 06:09:19	56222	2012-10-22 00:00:00	55851.4556134259	2011-10-17 10:56:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062010	We propose to observe the ultra-compact X-ray binaries 4U 0614+091 and 4U 1543-624 for 50 ksec each. The aim of these observations is to constrain the inner radius of the accretion disc for both sources using the recently discovered in both sources relativistialy broadened OVIII Ly alpha line at ~0.7 keV. This constrains the radius of the neutron star. The second goal is to constrain the continuum using more physical model than was used in the literature so far. The unique, large energy coverage of Suzaku will enable us to break possible degeneracies between the properties of the broadened lines and the continuum, providing more convidence on the results.	GALACTIC POINT SOURCES	4	A	OLIWIA MADEJ		EUR	6	AO6	INVESTIGATING THE ORIGIN OF THE CONTINUUM AND LINE EMISSION IN THE UCXBS 4U 0614+091 AND 4U 1543-624	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406072010/	Quick Look
66	SGR 1806-20	272.1687	-20.4711	271.424026	-20.47983	272.024767	2.954425	9.94559743	-0.27498509	268.1397	54387.2332060185	2007-10-14 05:35:49	54388.333599537	2007-10-15 08:00:23	402094010	52.2477	50	52.2477	52.2717	0	52.2637	2	2	0	2	1	0	0	50.0895	50.0895	95.0599	1	PROCESSED	57540.2839583333	2016-06-01 06:48:54	54771	2008-11-01 00:00:00	54403.9548611111	2007-10-30 22:55:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022016	Among magnetars, SGR 1806-20 is particularly interesting since it emitted two years ago the most powerful giant flare ever observed. We are performing a long term monitoring in the soft X-rays with XMM-Newton and hard X-rays with INTEGRAL to study how the source evolves back to quiescence. We obtained in AO-1 a Suzaku observation that was carried out simultaneously with XMM-Newton and provided for the first time a broad band spectrum of SGR 1806-20 on a short timescale. A new observation is required to study the spectral variability in the hard X-ray range and possibly the properties of bursts.	GALACTIC POINT SOURCES	4	C	SANDRO MEREGHETTI		EUR	2	AO2	CONTINUED MONITORING OF SGR 1806-20 AFTER THE GIANT FLARE WITH SUZAKU AND XMM-NEWTON	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402094010/	Quick Look
67	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
68	4U 1820-30	275.9314	-30.4193	275.127829	-30.44613	275.142299	-7.084391	2.74079847	-7.94949913	261.8762	55102.6696759259	2009-09-28 16:04:20	55103.5002662037	2009-09-29 12:00:23	404069040	28.6994	20	28.6994	28.6994	0	28.6994	3	2	0	3	1	0	0	24.9261	24.9261	71.7519	2	PROCESSED	57548.6752546296	2016-06-09 16:12:22	55499	2010-10-30 00:00:00	55133.2273263889	2009-10-29 05:27:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069040/	Quick Look
69	HER X-1	254.4619	35.2659	254.010863	35.341503	246.021498	57.41824	58.05460857	37.50723847	268.3041	55461.7937037037	2010-09-22 19:02:56	55462.2467476852	2010-09-23 05:55:19	405058040	21.74	20	21.74	21.796	0	21.8704	1	1	0	1	1	0	0	19.803	19.803	39.1359	0	PROCESSED	57553.5121180556	2016-06-14 12:17:27	55840	2011-10-06 00:00:00	55474.0995486111	2010-10-05 02:23:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052001	We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity?	GALACTIC POINT SOURCES	4	B	R DIGER STAUBERT		EUR	5	AO5	VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405058040/	Quick Look
70	GX 339-4	255.7013	-48.7851	254.753538	-48.714085	259.571516	-25.859202	338.94105066	-4.32130146	91.6296	55620.1778703704	2011-02-28 04:16:08	55620.8022569445	2011-02-28 19:15:15	405063040	21.799	20	21.799	21.807	0	21.8168	3	3	0	3	1	0	0	18.8502	18.8502	53.9239	0	PROCESSED	57601.0624074074	2016-08-01 01:29:52	56009	2012-03-23 00:00:00	55642.1310300926	2011-03-22 03:08:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052015	We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4	GALACTIC POINT SOURCES	4	A	CLEMENT CABANAC		EUR	5	AO5-TOO	PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063040/	Quick Look
71	4U 1705-44	257.2257	-44.096	256.322601	-44.032282	260.19112	-21.088012	343.32512852	-2.33758895	104.9955	56013.5320486111	2012-03-27 12:46:09	56016.4231134259	2012-03-30 10:09:17	406076010	100.8112	100	100.8112	100.8192	0	100.8209	2	2	0	2	1	0	0	90.0759	90.0759	249.7677	2	PROCESSED	57605.1022453704	2016-08-05 02:27:14	56393	2013-04-11 00:00:00	56027.2013657407	2012-04-10 04:49:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062019	We propose a ToO Suzaku 100-ks observation of the neutron star X-ray binary 4U 1705-44, to perform a detailed study of its broad-band (0.4-200 keV) X-ray spectrum during a hard state. XIS data will provide important information on the iron K-shell features, and the broad-band spectral capabilities of the HXD will allow to study the hard X-ray spectrum and in particular the Compton reflection bump at 20-50 keV. We plan to fit both the iron features and the reflection bump with a self-consistent model, which will allow to prove (or disprove) a disk origin of the iron line. Moreover the proposed observation will allow to study the correlation between the spectral index of the primary spectrum and the reflection amplitude, which gives important constraints on the geometry of the system.	GALACTIC POINT SOURCES	4	A	TIZIANA DI SALVO		EUR	6	AO6-TOO	SUZAKU BROAD-BAND OBSERVATION OF 4U 1705-44: PROBING THE DISK ORIGIN OF THE IRON LINE IN THE HARD STATE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406076010/	Quick Look
72	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
73	FS AURIGAE	86.945	28.5962	86.152995	28.579446	87.308718	5.183997	180.53629966	0.22811281	90.5955	56541.1879050926	2013-09-06 04:30:35	56542.802974537	2013-09-07 19:16:17	408041010	62.1842	62	62.1842	62.1842	0	62.1842	2	2	0	2	1	0	0	61.0287	61.0287	139.5158	0	PROCESSED	57612.5675810185	2016-08-12 13:37:19	56981	2014-11-20 00:00:00	56616.7165046296	2013-11-20 17:11:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082012	FS Aur represents one of the most unusual cataclysmic variable to have ever been observed. It is famous for a variety of uncommon and puzzling periodic photometric and spectroscopic variabilities. Tovmassian, Zharikov & Neustroev (2007) proposed that the precession of a fast-rotating magnetically accreting white dwarf can successfully explain these phenomena. We request 62 ks observations of FS Aur to detect the magnetic WD, determine its spin period, confirm the flux and spectral variability with the precession period, inconclusively detected by Chandra and Swift, and thus to check the proposed model. The theory of compact objects predicts certain relations between the spin and precession periods, and our findings will provide a good test for the theory.	GALACTIC POINT SOURCES	4	B	VITALY NEUSTROEV		EUR	8	AO8	PROBING THE PRECESSION OF WHITE DWARF IN CLOSE BINARY SYSTEMS - FS AURIGAE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408041010/	Quick Look
74	4U 1735-44	264.7398	-44.4536	263.827347	-44.425856	265.968173	-21.085622	346.05003995	-6.99385769	96.4379	57098.6918402778	2015-03-17 16:36:15	57099.2717824074	2015-03-18 06:31:22	408043030	4.3665	20	4.3665	4.9159	0	4.967	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8209027778	2016-08-17 19:42:06	57479	2016-04-01 00:00:00	57112.402662037	2015-03-31 09:39:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082017	We propose to observe the bursting low-mass X-ray binary 4U 1735-44 with Suzaku for a total exposure time of 60 ks. We plan to investigate the broad-band X-ray spectrum by performing a detailed spectroscopic and timing analysis in the energy range 0.4-100 keV. The main scientific aims of this observation are to detect and study the iron Kalpha line at 6.4-7 keV, simultaneously with the expected iron edge at 7-9 keV, emission lines at lower energy (such as S, Ar and Ca at 2.62 keV, 3.31 keV and 3.90 keV, respectively), and either a Compton reflection hump at 20-40 keV or a hard tail at energy above 25 keV (depending of the state of the source), thanks to the broad-band capabilities of Suzaku. This will allow to infer and probe the origin of these components, which is still debated.	GALACTIC POINT SOURCES	4	A	ELISE EGRON		EUR	8	AO8	BROAD-BAND SPECTRAL ANALYSIS AND STUDY OF THE DISK REFLECTION COMPONENT IN 4U 1735-44 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408043030/	Quick Look
75	G278.0+12.4	158.151	-43.7043	157.610146	-43.446336	182.388463	-47.807278	278.01040448	12.3478226	304.0284	56102.6152199074	2012-06-24 14:45:55	56102.9842476852	2012-06-24 23:37:19	507067010	18.996	17.5	19.004	18.996	0	19.004	1	1	0	1	1	0	0	16.442	16.442	31.8799	0	PROCESSED	57605.7438078704	2016-08-05 17:51:05	56582	2013-10-17 00:00:00	56219.6572916667	2012-10-19 15:46:30	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072014	We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed.	GALACTIC DIFFUSE EMISSION	5	A	TOBIAS PRINZ		EUR	7	AO7	IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507067010/	Quick Look
76	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
77	UGC03957 NORTH	114.9138	55.8102	113.899292	55.925218	106.552165	33.791456	161.76581362	28.79157051	294.9973	56006.0767939815	2012-03-20 01:50:35	56007.0710532407	2012-03-21 01:42:19	806091010	41.3662	45	41.3662	41.3662	0	41.3662	2	2	0	2	1	0	0	40.6312	40.6312	85.9019	1	PROCESSED	57604.9833217593	2016-08-04 23:35:59	56389	2013-04-07 00:00:00	56022.2738888889	2012-04-05 06:34:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062024	Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	BRENDA MIRANDA OCEJO		EUR	6	AO6	MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806091010/	Quick Look
78	UGC03957 SOUTH	115.5259	55.024	114.524001	55.141747	107.151159	33.092194	162.70412876	29.04503782	294.9967	56007.0719907407	2012-03-21 01:43:40	56008.1328125	2012-03-22 03:11:15	806092010	48.8159	45	48.8159	48.8159	0	48.8159	2	2	0	2	1	0	0	46.4169	46.4169	91.6439	3	PROCESSED	57604.9862731482	2016-08-04 23:40:14	56389	2013-04-07 00:00:00	56022.2514930556	2012-04-05 06:02:09	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062024	Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	BRENDA MIRANDA OCEJO		EUR	6	AO6	MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806092010/	Quick Look
79	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
80	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
81	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
82	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
83	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
84	G299.5-0.6	184.8049	-63.1515	184.121711	-62.873858	220.875708	-53.463768	299.30360744	-0.50694599	313.6989	56144.5663773148	2012-08-05 13:35:35	56144.9523032407	2012-08-05 22:51:19	507064010	13.8351	10	13.8431	13.8351	0	13.8431	1	1	0	1	1	0	0	13.2722	13.2722	33.3359	0	PROCESSED	57606.7635763889	2016-08-06 18:19:33	56630	2013-12-04 00:00:00	56264.5463541667	2012-12-03 13:06:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072014	We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed.	GALACTIC DIFFUSE EMISSION	5	A	TOBIAS PRINZ		EUR	7	AO7	IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507064010/	Quick Look
85	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
86	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
87	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
88	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
89	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
90	3C400.2 SW	294.5545	17.147	293.991762	17.032549	300.267467	38.043132	53.47817432	-2.17482828	81.5886	56761.5284375	2014-04-14 12:40:57	56762.0730555556	2014-04-15 01:45:12	509069010	24.1528	20	24.1528	24.1528	0	24.1537	2	2	0	2	1	0	0	23.915	23.915	47.0479	3	PROCESSED	57614.2434027778	2016-08-14 05:50:30	57138	2015-04-26 00:00:00	56772.6111226852	2014-04-25 14:40:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092010	Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances.	GALACTIC DIFFUSE EMISSION	5	A	JACCO VINK		EUR	9	AO9	THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509069010/	Quick Look
91	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
92	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
93	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
94	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
95	A3526	191.8847	-40.8272	191.196139	-40.554367	208.554246	-32.533282	302.13618529	22.03852437	109.9993	55942.6812037037	2012-01-16 16:20:56	55942.9772569444	2012-01-16 23:27:15	806085010	15.0057	11	15.0097	15.0057	0	15.0116	2	2	0	2	1	0	0	14.9297	14.9297	25.576	0	PROCESSED	57604.3736805556	2016-08-04 08:58:06	56331	2013-02-08 00:00:00	55960.1598726852	2012-02-03 03:50:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806085010/	Quick Look
96	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
97	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
98	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
99	A2163	243.8156	-6.2315	243.147928	-6.107198	243.010913	14.789433	6.59879538	30.51803676	282.2871	54696.6726851852	2008-08-18 16:08:40	54700.4008449074	2008-08-22 09:37:13	803071010	135.7864	130	135.7944	135.7864	0	135.7944	2	2	0	2	1	0	0	122.1262	122.1262	322.0615	5	PROCESSED	57543.4331597222	2016-06-04 10:23:45	55080	2009-09-06 00:00:00	54713.5071875	2008-09-04 12:10:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032023	Measurements of intracluster gas temperatures out to large radii, where much of the cluster mass resides, are of the utmost importance for the use of clusters in precision cosmology and for studies of cluster physics. Previous attempts to measure robust temperatures at cluster virial radii failed. Here, we demonstrate that such measurements are feasible now for the first time with the Suzaku X-ray CCDs, using our observation of the cluster A2204, carefully treating background and PSF. To determine the temperature profile of the cluster population as a whole, more such observations are required. We show that A2163 is the optimal complementary target for such an investigation. We, therefore, propose to observe A2163 to measure the gas temperature to 15% accuracy out to the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	THOMAS REIPRICH		EUR	3	AO3	GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS OF A2163	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803071010/	Quick Look
100	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
101	A76 WEST	9.903	6.838	9.256884	6.56348	11.779086	2.367721	117.68922859	-55.91332108	260	55183.8756481482	2009-12-18 21:00:56	55184.3334953704	2009-12-19 08:00:14	804088010	15.1164	15	15.1244	15.1164	0	15.1324	2	2	0	2	1	0	0	14.2066	14.2066	39.5479	0	PROCESSED	57549.8934722222	2016-06-10 21:26:36	55575	2011-01-14 00:00:00	55209.4668055556	2010-01-13 11:12:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042018	In our flux limited survey of galaxy clusters in the ROSAT All-Sky Atlas we find that about 5 - 10 percent of the galaxy clusters have a diffuse, low X-ray surface brightness. These objects could possibly be explained as dynamically very young clusters, which have not yet formed a central core. Three such clusters in our XMM-Newton study of an unbiased sub-sample of 33 galaxy clusters, REXCESS, show suprisingly high entropies in their centers which does not readily support the early formation stage. To shed more light on the nature of these clusters we propose to observe two extremely low surface brightness clusters at low redshift, for which we also have detailed optical data. SUZAKU with its low background is ideally suited for this study.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	HANS BOEHRINGER		EUR	4	AO4	SHEDDING LIGHT ON THE NATURE OF EXTREMELY LOW SURFACE BRIGHTNESS CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804088010/	Quick Look
102	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
103	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
104	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
105	UGC03957 WEST	114.5487	55.2415	113.541037	55.354916	106.445391	33.192967	162.38027408	28.51701147	289.9984	56004.175150463	2012-03-18 04:12:13	56005.2466550926	2012-03-19 05:55:11	806093010	48.2169	45	48.2249	48.2169	0	48.2249	1	1	0	1	1	0	0	46.846	46.846	92.5679	0	PROCESSED	57604.9538773148	2016-08-04 22:53:35	56388	2013-04-06 00:00:00	56020.0984837963	2012-04-03 02:21:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062024	Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	BRENDA MIRANDA OCEJO		EUR	6	AO6	MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806093010/	Quick Look
106	SERSIC 159-03	348.4959	-42.7314	347.802109	-43.003937	330.666566	-34.355163	348.33340728	-64.81387916	47.3295	53851.5323611111	2006-04-26 12:46:36	53853.2668055556	2006-04-28 06:24:12	801093010	67.7843	70	67.8003	67.8003	67.7843	67.7923	2	2	2	2	1	0	0	41.5833	41.5833	149.8278	2	PROCESSED	57533.6210532407	2016-05-25 14:54:19	54400	2007-10-27 00:00:00	53907.8625231482	2006-06-21 20:42:02	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012045	We propose to observe the cluster of galaxies Sersic 159-03 using a total exposure time of 70 ks to investigate the soft excess emission previously detected in the observations with ROSAT and XMM-Newton. The superior redistribution function of Suzaku will allow us to determine whether the O VII line emission detected with XMM-Newton is of local (Galactic) origin or is emitted by the warm-hot intergalactic medium (WHIM) in the vicinity of the cluster. The strong soft emission around this cluster together with the much improved response function of the XIS detectors at low energies make Sersic 159-03 the most promising target to unambiguously detect the WHIM for the first time in emission with Suzaku.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JELLE KAASTRA		EUR	1	AO1	O VII LINE EMISSION IN SERSIC 159-03 - WHIM OR GALACTIC ORIGIN?	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801093010/	Quick Look
107	HYDRA A SW	139.253	-12.251	138.651756	-12.041032	145.924531	-26.640711	242.88145003	24.78864489	106.4205	56241.8334490741	2012-11-10 20:00:10	56242.8342708333	2012-11-11 20:01:21	807090010	39.8399	40	39.8479	39.8559	0	39.8399	1	1	0	1	1	0	0	33.7085	33.7085	86.4639	0	PROCESSED	57607.9882407407	2016-08-07 23:43:04	56631	2013-12-05 00:00:00	56265.6332986111	2012-12-04 15:11:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072020	Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DOMINIQUE ECKERT		EUR	7	AO7	MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807090010/	Quick Look
108	NGC 6338	258.8129	57.4208	258.599761	57.475287	235.015954	79.490546	85.8195722	35.41601483	46.4308	56771.4831712963	2014-04-24 11:35:46	56771.8058333333	2014-04-24 19:20:24	809099010	15.4756	10	15.4756	15.4756	0	15.4756	3	2	0	2	1	0	0	14.5259	14.5259	26.0449	0	PROCESSED	57614.9892708333	2016-08-14 23:44:33	57155	2015-05-13 00:00:00	56789.6384722222	2014-05-12 15:19:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809099010/	Quick Look
109	AWM4	241.2331	23.9108	240.70062	24.045882	232.521444	43.67819	39.92527821	46.49145981	302.6954	56859.2473263889	2014-07-21 05:56:09	56859.4627314815	2014-07-21 11:06:20	809102010	9.31	11	9.31	9.438	0	9.438	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.4155092593	2016-08-15 09:58:20	57239	2015-08-05 00:00:00	56873.5548958333	2014-08-04 13:19:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809102010/	Quick Look
110	ABELL 3733	315.4567	-28.0341	314.710836	-28.231283	309.79285	-10.656463	17.77333082	-39.60697798	260.2652	56981.8706481482	2014-11-20 20:53:44	56982.1530439815	2014-11-21 03:40:23	809108010	14.5884	15	14.5964	14.6044	0	14.5884	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7988541667	2016-08-16 19:10:21	57362	2015-12-06 00:00:00	56996.4060300926	2014-12-05 09:44:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809108010/	Quick Look
111	A3404	101.1266	-54.2028	100.864696	-54.149703	118.987538	-76.520827	263.61200949	-22.68018452	319.1401	54971.6181944444	2009-05-20 14:50:12	54974.625162037	2009-05-23 15:00:14	804089010	122.0929	121	122.1009	122.1009	0	122.0929	2	2	0	2	1	0	0	106.1261	106.1261	259.7879	4	PROCESSED	57546.7060532407	2016-06-07 16:56:43	55358	2010-06-11 00:00:00	54992.6862615741	2009-06-10 16:28:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042025	Robust and precise mass measurements for a large number of galaxy clusters represent the single most important step to prepare for dark energy cluster surveys to be performed, e.g., with eROSITA. Robustness and precision can best be achieved by a comparative and combined analysis of independent techniques. Here, we propose to use measurements from Suzaku, APEX-SZ, and wide-field optical telescopes to determine cluster masses up to the virial radius. X-ray, SZ, and gravitational lensing reduction and analyses will all be performed by experts at a single location. We demonstrate that we have selected the optimal targets for this study. Further, we show promising results from our Suzaku analysis of cluster outskirts, from our lensing pipeline, as well as from our combined SZ/X-ray method.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	THOMAS REIPRICH		EUR	4	AO4	COMBINED SUZAKU/APEX-SZ/LENSING MASS MEASUREMENTS OF THE GALAXY CLUSTERS A3404 AND A2537	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804089010/	Quick Look
112	A2877-SOUTH	17.378	-46.6527	16.824483	-46.918871	351.212416	-48.486015	293.76700694	-70.15260223	237.9995	56647.8346643518	2013-12-21 20:01:55	56649.916875	2013-12-23 22:00:18	808103010	83.5172	80	83.5172	83.5252	0	83.5332	2	2	0	2	1	0	0	81.2993	81.2993	179.8979	4	PROCESSED	57613.6802199074	2016-08-13 16:19:31	57033	2015-01-11 00:00:00	56665.8173263889	2014-01-08 19:36:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082014	We propose to observe the galaxy group A2877 for a combine observation time of 150 ks, with two different pointings. The aim of the project is to obtain temperature and surface brightness profiles out to large radii to constrain entropies. We aim to see if the entropy profile flattens at large radii, which could indicate gas clumping and/or other processes. This would possibly be the first unrelaxed galaxy group whose entropy profile would have been studied in the outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	BHARADWAJ VIJAYSARATHY		EUR	8	AO8	INVESTIGATING THE OUTSKIRTS OF THE UNRELAXED GALAXY GROUP A2877	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808103010/	Quick Look
113	A3528-S OFFSET 1	193.8801	-29.4768	193.202783	-29.206094	204.617979	-21.613954	303.99602967	33.38651365	289.4829	56500.4359953704	2013-07-27 10:27:50	56501.528587963	2013-07-28 12:41:10	808104010	40.3411	50	40.3491	40.3491	0	40.3411	2	2	0	2	1	0	0	40.8623	40.8623	94.384	2	PROCESSED	57612.0687037037	2016-08-12 01:38:56	56955	2014-10-25 00:00:00	56587.7834490741	2013-10-22 18:48:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082018	We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	LORENZO LOVISARI		EUR	8	AO8	TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808104010/	Quick Look
114	A3526	191.2847	-39.8559	190.600127	-39.582502	207.545871	-31.88181	301.61867579	22.99978629	109.9984	55943.9465393518	2012-01-17 22:43:01	55944.2683333333	2012-01-18 06:26:24	806089010	15.9106	15	15.9186	15.9106	0	15.9186	1	1	0	1	1	0	0	12.985	12.985	27.7919	0	PROCESSED	57604.3987268518	2016-08-04 09:34:10	56332	2013-02-09 00:00:00	55964.1580439815	2012-02-07 03:47:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806089010/	Quick Look
115	J2218.6-0346	334.6629	-3.7693	334.013965	-4.02026	335.129241	6.290164	58.79146355	-46.71055995	71.7798	56063.8991550926	2012-05-16 21:34:47	56064.7196875	2012-05-17 17:16:21	807085010	28.629	25	28.629	28.629	0	28.629	2	2	0	2	1	0	0	26.8327	26.8327	70.8839	1	PROCESSED	57605.4341550926	2016-08-05 10:25:11	56442	2013-05-30 00:00:00	56076.0273726852	2012-05-29 00:39:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072018	We propose to observe the three clusters of galaxies J2218.2-0350, J2218.6-0346 and J2218.8-0258 with exposure times of 15, 25 and 35 ks respectively. These clusters are part of a structure of four linearly aligned clusters, separated from each other by 4 to 10 Mpc. We will accurately determine their masses and orientation. This will allow us to fully map the tidal force field of the structure, which is the prime force behind the formation of filaments in the cosmic web. We will study the effects of cluster mass, separation and mutual orientation on the filamentary structure of the cosmic web and on the evolution of galaxies therein.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	E.G. PATRICK BOS		EUR	7	AO7	CLUSTERS AND THE COSMIC WEB	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807085010/	Quick Look
116	A3528-S OFFSET 3	194.0873	-29.8404	193.408879	-29.569931	204.956936	-21.869821	304.20210274	33.01923597	288.9994	56502.3985300926	2013-07-29 09:33:53	56503.6522453704	2013-07-30 15:39:14	808106010	61.2339	60	61.2579	61.2499	0	61.2339	2	2	0	2	1	0	0	61.6474	61.6474	108.3097	2	PROCESSED	57612.1235763889	2016-08-12 02:57:57	56955	2014-10-25 00:00:00	56587.4691782407	2013-10-22 11:15:37	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082018	We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	8	AO8	TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808106010/	Quick Look
117	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
118	XTE J1710-281	257.5483	-28.1282	256.762614	-28.066297	258.983914	-5.161686	356.35839186	6.92613447	86.2275	55278.9207638889	2010-03-23 22:05:54	55281.1460300926	2010-03-26 03:30:17	404068010	76.1385	75	76.1385	76.1465	0	76.1465	3	3	0	3	1	0	0	23.6565	23.6565	192.2397	3	PROCESSED	57551.0466435185	2016-06-12 01:07:10	55668	2011-04-17 00:00:00	55301.5227662037	2010-04-15 12:32:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042003	We propose to observe XTE J1710-281, a low-mass X-ray binary showing bursts, eclipses and dips. We want to determine the nature of the X-ray emission in this yet poorly-studied system and exploit the fact it is viewed close to edge-on to probe the structure of the disk and of the ionized plasma located above it. The broad-band coverage of Suzaku XIS and HXD will allow us to determine the overall shape of the ionizing continuum, which is a key parameter to infer the properties of the warm absorber whose narrow spectral signatures will be simultaneously detected thanks to the good spectral resolution of XIS near 6 keV.	GALACTIC POINT SOURCES	4	C	LAURENCE BOIRIN		EUR	4	AO4	SUZAKU TO INVESTIGATE A LOW-MASS X-RAY BINARY SHOWING BURSTS, ECLIPSES, AND DIPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404068010/	Quick Look
119	HESS J1718-385	259.5578	-38.4584	258.700067	-38.405877	261.528277	-15.323293	348.92137939	-0.45364037	266.9006	54706.233599537	2008-08-28 05:36:23	54706.9286342593	2008-08-28 22:17:14	503108010	23.5097	20	23.5097	23.5097	0	23.5097	2	2	0	2	1	0	0	19.4402	19.4402	60.0479	1	PROCESSED	57543.4301851852	2016-06-04 10:19:28	55093	2009-09-19 00:00:00	54720.4386689815	2008-09-11 10:31:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032026	HESS J1718-385 is a newly discovered Very High Energy (VHE) source with an unusually hard energy spectrum, close to an energetic pulsar. The classification as a VHE Pulsar Wind Nebula (PWN) was confirmed by observations of the region with XMM-Newton and Suzaku. XMM showed a compact X-ray PWN around the pulsar, whereas Suzaku revealed low surface brightness emission close to the VHE source. To morphologically connect this low surface brightness emission to the X-ray PWN, we propose another short, 20 ksec Suzaku pointing, aiming between the VHE source center and the pulsar location. The data will allow to identify the new Suzaku source with the compact X-ray PWN. The spectra will be used to investigate the unusual particle energy distribution that is derived from the hard VHE spectrum.	GALACTIC DIFFUSE EMISSION	5	A	GERD PUEHLHOFER		EUR	3	AO3	SUZAKU OBSERVATIONS OF THE LOW SURFACE BRIGHTNESS X-RAY PULSAR WIND NEBULA CANDIDATE ASSOCIATED WITH HESS J1718-385	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503108010/	Quick Look
120	J1803-2149	270.7914	-21.8184	270.03917	-21.820419	270.725404	1.620434	8.14241987	0.18738401	269.7005	56191.3371643518	2012-09-21 08:05:31	56192.1730671296	2012-09-22 04:09:13	407092010	31.9986	25	32.0218	32.0146	0	31.9986	2	2	0	2	1	0	0	28.8812	28.8812	72.2179	1	PROCESSED	57607.1276736111	2016-08-07 03:03:51	56584	2013-10-19 00:00:00	56218.5534259259	2012-10-18 13:16:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072019	The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances.	GALACTIC POINT SOURCES	4	A	MARTINO MARELLI		EUR	7	AO7	SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407092010/	Quick Look
121	GX 339-4	255.7041	-48.783	254.756356	-48.711998	259.573299	-25.856913	338.94384752	-4.32149031	92.8952	55627.5468518518	2011-03-07 13:07:28	55628.0320138889	2011-03-08 00:46:06	405063050	16.9925	20	16.9925	20.2693	0	20.2693	2	2	0	2	1	0	0	15.9851	15.9851	41.8741	2	PROCESSED	57601.1142476852	2016-08-01 02:44:31	56015	2012-03-29 00:00:00	55645.2088078704	2011-03-25 05:00:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052015	We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4	GALACTIC POINT SOURCES	4	A	CLEMENT CABANAC		EUR	5	AO5-TOO	PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405063050/	Quick Look
122	AX J1818.8-1559	274.7184	-16.0002	273.997976	-16.021361	274.56335	7.365738	15.02984997	-0.2600064	265.8517	55849.5538888889	2011-10-15 13:17:36	55852.1474537037	2011-10-18 03:32:20	406074010	95.1912	100	99.3859	99.3859	0	95.1912	2	2	0	2	1	0	0	83.8746	83.8746	224.0699	1	PROCESSED	57603.4900347222	2016-08-03 11:45:39	56241	2012-11-10 00:00:00	55873.993599537	2011-11-08 23:50:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062016	The Galactic X-ray source AX J1818.8-1559 is a possible new member of the small class of magnetar candidates since a short and soft burst was detected in the 15--100 keV range from this source in 2007 with INTEGRAL. We request a Suzaku pointing of 100 ks in order to carry out a sensitive search for pulsations. This, together with the good quality spectrum, possibly extending in the hard X-ray range, that can be obtained with the Suzaku instruments, will allow us to reveal the nature of AX J1818.8-1559, most likely adding a new member to the small but rapidly increasing family of magnetar candidates	GALACTIC POINT SOURCES	4	B	SANDRO MEREGHETTI		EUR	6	AO6	A NEW GALACTIC MAGNETAR CANDIDATE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406074010/	Quick Look
123	J1746-3239	266.7261	-32.6662	265.90725	-32.648308	267.198391	-9.25684	356.95543166	-2.17351712	72.0153	56365.6469675926	2013-03-14 15:31:38	56366.4022453704	2013-03-15 09:39:14	407093010	27.3469	25	27.3469	27.3469	0	27.3469	2	2	0	2	1	0	0	27.005	27.005	65.2519	2	PROCESSED	57610.8216087963	2016-08-10 19:43:07	56745	2014-03-29 00:00:00	56379.530775463	2013-03-28 12:44:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072019	The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances.	GALACTIC POINT SOURCES	4	A	MARTINO MARELLI		EUR	7	AO7	SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407093010/	Quick Look
124	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
125	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
126	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
127	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
128	M87N BRIGHT	187.7	12.7001	187.067492	12.976168	181.920384	14.695127	283.404729	74.78396174	297.7704	54625.0923263889	2008-06-08 02:12:57	54625.6259722222	2008-06-08 15:01:24	803070010	24.2485	20	24.2565	24.2485	0	24.2565	1	1	0	1	1	0	0	20.2709	20.2709	46.1039	1	PROCESSED	57542.7423263889	2016-06-03 17:48:57	55009	2009-06-27 00:00:00	54642.2018865741	2008-06-25 04:50:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032011	We propose to take advantage of Suzaku's low background and good collecting area to observe a strong surface brightness discontinuity, most likely a cold front, in the outskirts of M87. We will make accurate temperature and pressure profiles across this cold front, determine the energy associated with it, and compare this to the energy of known AGN-ICM interaction features in M87. With Suzaku's superior spectral redistribution function we will for the first time measure Mg and O in the M87 outskirts and improve constraints on relative contributions by SNIa and SNII. We will study abundance and abundance-ratio variations across the cold front and determine the role of gas sloshing in transporting metals produced by the central galaxy into the ICM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		EUR	3	AO3	THE ENERGETICS AND METAL ABUNDANCE PATTERNS IN THE OUTSKIRTS OF M87	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803070010/	Quick Look
129	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
130	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
131	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
132	ABELL 2204	248.0963	5.6404	247.481247	5.74563	245.314616	27.222606	21.10023438	33.35451369	261.3606	53995.3098958333	2006-09-17 07:26:15	53996.5098958333	2006-09-18 12:14:15	801091010	49.1113	55	49.1113	49.1113	49.1113	49.1113	2	2	2	2	1	0	0	51.9372	51.9372	103.6439	1	PROCESSED	57535.6038194444	2016-05-27 14:29:30	54526	2008-03-01 00:00:00	54020.8840277778	2006-10-12 21:13:00	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012018	Measurements of the intracluster gas temperatures out to large radii, where most of the cluster mass resides, are of the utmost importance for the use of clusters in precision cosmology and for studies of cluster physics. Previous attempts to measure temperatures at the cluster virial radius have failed. Here we show that such measurements appear feasible now for the first time with the Suzaku X-ray CCDs. Furthermore, we show that A2204 and A2163 are optimal targets for such an investigation. We, therefore, propose to observe A2204 for 55 ks and A2163 for 100 ks to measure the gas temperature to 10% and 15% accuracy (1-sigma), respectively, out to the cluster virial radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	THOMAS REIPRICH		EUR	1	AO1	A2204 AND A2163: GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS	SPE	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801091010/	Quick Look
133	ABELL 2537	347.0895	-2.1864	346.446208	-2.457426	347.265087	3.085071	73.83613509	-54.91382092	56.4647	55368.5295486111	2010-06-21 12:42:33	55371.9946875	2010-06-24 23:52:21	805090010	124.8232	129	124.8472	124.8232	0	124.8472	2	2	0	2	1	0	0	108.3908	108.3908	281.2176	1	PROCESSED	57552.4996412037	2016-06-13 11:59:29	55772	2011-07-30 00:00:00	55403.4592361111	2010-07-26 11:01:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052007	Robust and precise mass measurements for a large number of galaxy clusters represent the single most important step to prepare for dark energy cluster surveys to be performed, e.g., with eROSITA. Robustness and precision can best be achieved by a comparative and combined analysis of independent techniques. Here, we propose to use measurements from Suzaku, APEX-SZ, and wide-field optical telescopes to determine cluster masses up to the virial radius. X-ray, SZ, and gravitational lensing reductions and analyses will all be performed by experts at a single location. We demonstrate that we have selected the optimal targets for this study. Further, we show promising results from our Suzaku analysis of cluster outskirts, from our lensing pipeline, as well as from our combined SZ/X-ray method.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	THOMAS REIPRICH		EUR	5	AO5	COMBINED SUZAKU/APEX-SZ/LENSING MASS MEASUREMENTS OF THE GALAXY CLUSTER A2537	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805090010/	Quick Look
134	TW HYA	165.4619	-34.7081	164.870404	-34.438931	182.672236	-37.188941	278.67685486	22.95004903	99.3673	54429.0615625	2007-11-25 01:28:39	54429.6946064815	2007-11-25 16:40:14	402089020	20.0096	11	20.0096	20.0176	0	20.0256	1	1	0	1	1	0	0	17.55	17.55	54.6879	2	PROCESSED	57540.5900115741	2016-06-01 14:09:37	54804	2008-12-04 00:00:00	54434.1387268518	2007-11-30 03:19:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	022007	We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra.	GALACTIC POINT SOURCES	4	B	JURGEN SCHMITT		EUR	2	AO2	ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402089020/	Quick Look
135	4U 1820-30	275.9316	-30.4206	275.12802	-30.447431	275.142418	-7.085697	2.73970623	-7.95024046	261.8755	55096.0447453704	2009-09-22 01:04:26	55096.8335416667	2009-09-22 20:00:18	404069030	29.2254	20	29.2254	29.2254	0	29.2254	2	1	0	2	1	0	0	25.9405	25.9405	68.148	1	PROCESSED	57548.6598726852	2016-06-09 15:50:13	55477	2010-10-08 00:00:00	55110.3989699074	2009-10-06 09:34:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069030/	Quick Look
136	4U 1735-44	264.7467	-44.4484	263.834293	-44.420689	265.97323	-21.080234	346.05710105	-6.99533469	268.9985	56917.7849884259	2014-09-17 18:50:23	56918.9988194444	2014-09-18 23:58:18	408043020	10.1772	60	10.1772	10.2016	0	10.3047	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5500925926	2016-08-16 13:12:08	57626	2016-08-26 00:00:00	56940.6296064815	2014-10-10 15:06:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082017	We propose to observe the bursting low-mass X-ray binary 4U 1735-44 with Suzaku for a total exposure time of 60 ks. We plan to investigate the broad-band X-ray spectrum by performing a detailed spectroscopic and timing analysis in the energy range 0.4-100 keV. The main scientific aims of this observation are to detect and study the iron Kalpha line at 6.4-7 keV, simultaneously with the expected iron edge at 7-9 keV, emission lines at lower energy (such as S, Ar and Ca at 2.62 keV, 3.31 keV and 3.90 keV, respectively), and either a Compton reflection hump at 20-40 keV or a hard tail at energy above 25 keV (depending of the state of the source), thanks to the broad-band capabilities of Suzaku. This will allow to infer and probe the origin of these components, which is still debated.	GALACTIC POINT SOURCES	4	A	ELISE EGRON		EUR	8	AO8	BROAD-BAND SPECTRAL ANALYSIS AND STUDY OF THE DISK REFLECTION COMPONENT IN 4U 1735-44 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408043020/	Quick Look
137	GRO J1008-57	152.4313	-58.2999	151.999865	-58.053533	193.901629	-61.317749	282.99773034	-1.83149103	115.5012	56660.6548148148	2014-01-03 15:42:56	56661.5897569444	2014-01-04 14:09:15	408044010	15.3374	20	15.3374	15.3479	0	15.3374	3	3	0	3	1	0	0	22.1794	22.1794	55.0379	1	PROCESSED	57613.7393981482	2016-08-13 17:44:44	57040	2015-01-18 00:00:00	56679.7652662037	2014-01-22 18:21:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082019	We propose to observe the transient XRB GRO J1008−57 for 20 ks during an outburst in 2014 January after the currently ongoing giant outburst. The source exhibits regular outbursts once per orbit. Several of these outbursts have been observed in the past showing that the spectral shape remains constant between outbursts. Since we were able to improve the orbital ephemeris it is possible to predict future outbursts of the source. The source is currently (MJD 56245) exhibiting a giant type II outburst showing that the companion has ejected large amounts of material. We therefore propose to observe the system after this outburst to check for spectral and temporal changes and to study the iron line complex to derive the amount and ionization state of the material.	GALACTIC POINT SOURCES	4	A	INGO KREYKENBOHM		EUR	8	AO8	MEASURING THE RESIDUAL MATERIAL IN GRO J1008−57 AFTER THE GIANT OUTBURST	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408044010/	Quick Look
138	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
139	A3526	191.5735	-40.3305	190.887021	-40.05737	208.034799	-32.201568	301.8706053	22.53064841	109.9984	55943.2367592593	2012-01-17 05:40:56	55943.6161574074	2012-01-17 14:47:16	806087010	14.4943	13	14.4943	14.4943	0	14.4943	2	2	0	2	1	0	0	10.3865	10.3865	32.7799	1	PROCESSED	57604.3860416667	2016-08-04 09:15:54	56332	2013-02-09 00:00:00	55964.1523148148	2012-02-07 03:39:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806087010/	Quick Look
140	A3526	191.429	-40.092	190.743483	-39.818735	207.789532	-32.040636	301.74515791	22.76656347	109.9976	55943.6166319444	2012-01-17 14:47:57	55943.9461111111	2012-01-17 22:42:24	806088010	15.0662	14	15.0702	15.0662	0	15.0662	2	2	0	2	1	0	0	14.8434	14.8434	28.458	1	PROCESSED	57604.3884490741	2016-08-04 09:19:22	56332	2013-02-09 00:00:00	55964.2169675926	2012-02-07 05:12:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806088010/	Quick Look
141	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
142	HYDRA A FAR SE	139.7	-12.375	139.09881	-12.163612	146.431142	-26.609663	243.28582967	25.05625041	300	56082.6736342593	2012-06-04 16:10:02	56083.9368981482	2012-06-05 22:29:08	807088010	40.939	40	40.947	40.939	0	40.947	2	2	0	2	1	0	0	37.9143	37.9143	109.1358	0	PROCESSED	57605.5894444444	2016-08-05 14:08:48	56464	2013-06-21 00:00:00	56096.2405208333	2012-06-18 05:46:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072020	Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DOMINIQUE ECKERT		EUR	7	AO7	MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807088010/	Quick Look
143	G115.7+17.5	336.6801	78.3035	336.566813	78.048018	59.497327	68.492125	115.72297849	17.51053762	214.3075	56311.7506712963	2013-01-19 18:00:58	56313.7419328704	2013-01-21 17:48:23	807093010	97.8732	100	97.8892	97.8732	0	97.8892	2	2	0	2	1	0	0	94.3977	94.3977	172.0079	1	PROCESSED	57608.5818634259	2016-08-08 13:57:53	56708	2014-02-20 00:00:00	56342.5694097222	2013-02-19 13:39:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072021	We propose to observe 4 galaxy clusters from the first all-sky blind Sunyaev Zeldovich (SZ) effect cluster catalogue produced by the Planck satellite. This catalogue has revealed a new population of clusters previously undetected by X-ray surveys. The Planck SZ selected cluster sample consists of hot, massive, morphologically disturbed clusters that are under-luminous in the soft X-ray band. This exciting population has implications not only for understanding the thermodynamic state of the intracluster medium, but also for cluster cosmology where it represents an important area of phase space in the cluster mass function; it is a pointer to the dynamics of how clusters form through mergers, and to the true spatial density of cluster-mass structures not represented in X-ray surveys.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ANNA SCAIFE		EUR	7	AO7	CONSTRAINING THE THERMODYNAMIC STATE OF NEW PLANCK GALAXY CLUSTERS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807093010/	Quick Look
144	PLCK G214.6-37.0	137.1752	14.6923	136.484307	14.895327	135.215425	-1.654352	214.5759479	36.9399481	287	56413.2455439815	2013-05-01 05:53:35	56416.322349537	2013-05-04 07:44:11	808101010	119.2637	120	119.2637	119.2637	0	119.2637	2	2	0	2	1	0	0	106.3127	106.3127	265.8039	5	PROCESSED	57611.2793981482	2016-08-11 06:42:20	56795	2014-05-18 00:00:00	56429.7933217593	2013-05-17 19:02:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082007	We propose a detailed investigation of the nature of PLCK G214.6-37.0, discovered in the Planck survey. We aim at constraining the presence and properties of filamentary structures connecting and surrounding the clusters. We will unveil the overall dynamics of this complex structure and establish its detailed pressure distribution that can be used for a better estimation of YX to be compared with YSZ. Thus, we will perform a direct search for structures in between identified supercluster components from a careful comparison with the Planck results. Furthermore, the distribution of the PLCK G214.6-37.0 components suggest that it is evolving accreting sub-clusters along the filaments. That makes this supercluster one of the to search for the WHIM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	LORENZO LOVISARI		EUR	8	AO8	TRACKING DOWN THE PLANCK SUPERCLUSTER PLCK G214.6-37.0	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808101010/	Quick Look
145	UGC03957 EAST	115.9739	55.4967	114.966906	55.616404	107.333122	33.607468	162.19834712	29.35111138	294.9944	56008.1335648148	2012-03-22 03:12:20	56009.1717476852	2012-03-23 04:07:19	806094010	46.6221	45	46.6221	46.6221	0	46.6221	2	2	0	2	1	0	0	45.2608	45.2608	89.6879	1	PROCESSED	57604.9930324074	2016-08-04 23:49:58	56434	2013-05-22 00:00:00	56068.628900463	2012-05-21 15:05:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062024	Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	BRENDA MIRANDA OCEJO		EUR	6	AO6	MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806094010/	Quick Look
146	A3528-S OFFSET 2	193.9782	-29.6501	193.300361	-29.379506	204.778966	-21.736125	304.09397791	33.21155179	289.0026	56501.5292476852	2013-07-28 12:42:07	56502.3981481482	2013-07-29 09:33:20	808105010	42.3	40	42.3	42.3078	0	42.316	2	2	0	2	1	0	0	42.5258	42.5258	75.0659	2	PROCESSED	57612.0639583333	2016-08-12 01:32:06	56955	2014-10-25 00:00:00	56587.7982523148	2013-10-22 19:09:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082018	We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	LORENZO LOVISARI		EUR	8	AO8	TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808105010/	Quick Look
147	M87N FAINT	187.6988	12.9392	187.066448	13.215269	181.818448	14.91295	283.11850774	75.01113844	297.6812	54625.626400463	2008-06-08 15:02:01	54627.068275463	2008-06-10 01:38:19	803069010	65.2474	60	65.2474	65.2714	0	65.2554	2	2	0	2	1	0	0	57.9068	57.9068	124.5638	0	PROCESSED	57542.7828587963	2016-06-03 18:47:19	55009	2009-06-27 00:00:00	54642.2950694444	2008-06-25 07:04:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032011	We propose to take advantage of Suzaku's low background and good collecting area to observe a strong surface brightness discontinuity, most likely a cold front, in the outskirts of M87. We will make accurate temperature and pressure profiles across this cold front, determine the energy associated with it, and compare this to the energy of known AGN-ICM interaction features in M87. With Suzaku's superior spectral redistribution function we will for the first time measure Mg and O in the M87 outskirts and improve constraints on relative contributions by SNIa and SNII. We will study abundance and abundance-ratio variations across the cold front and determine the role of gas sloshing in transporting metals produced by the central galaxy into the ICM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		EUR	3	AO3	THE ENERGETICS AND METAL ABUNDANCE PATTERNS IN THE OUTSKIRTS OF M87	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803069010/	Quick Look
148	ABELL 2877	17.5065	-45.9303	16.951425	-46.196287	351.939456	-47.942764	293.04607396	-70.83949903	47.4208	56809.9110532407	2014-06-01 21:51:55	56810.1181712963	2014-06-02 02:50:10	809100010	11.908	10	11.916	11.908	0	11.9306	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.1778240741	2016-08-15 04:16:04	57197	2015-06-24 00:00:00	56828.5915856482	2014-06-20 14:11:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809100010/	Quick Look
149	HYDRA A OUT	139.8502	-12.6235	139.249709	-12.411636	146.680072	-26.793484	243.60142222	25.01758475	300.0034	56085.1461574074	2012-06-07 03:30:28	56085.6667824074	2012-06-07 16:00:10	807091010	20.3276	20	20.3516	20.3436	0	20.3276	2	2	0	2	1	0	0	16.5403	16.5403	44.9779	0	PROCESSED	57605.607349537	2016-08-05 14:34:35	56491	2013-07-18 00:00:00	56120.2321296296	2012-07-12 05:34:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072020	Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DOMINIQUE ECKERT		EUR	7	AO7	MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807091010/	Quick Look
150	G171.9-40.7	48.2433	8.3685	47.57264	8.181881	48.126521	-9.211403	171.97024112	-40.65556769	252.8031	56320.012025463	2013-01-28 00:17:19	56322.7126967593	2013-01-30 17:06:17	807092010	100.9825	100	100.9905	100.9825	0	100.9848	2	2	0	2	1	0	0	93.1617	93.1617	233.2957	0	PROCESSED	57608.6871527778	2016-08-08 16:29:30	56749	2014-04-02 00:00:00	56365.6023263889	2013-03-14 14:27:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072021	We propose to observe 4 galaxy clusters from the first all-sky blind Sunyaev Zeldovich (SZ) effect cluster catalogue produced by the Planck satellite. This catalogue has revealed a new population of clusters previously undetected by X-ray surveys. The Planck SZ selected cluster sample consists of hot, massive, morphologically disturbed clusters that are under-luminous in the soft X-ray band. This exciting population has implications not only for understanding the thermodynamic state of the intracluster medium, but also for cluster cosmology where it represents an important area of phase space in the cluster mass function; it is a pointer to the dynamics of how clusters form through mergers, and to the true spatial density of cluster-mass structures not represented in X-ray surveys.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ANNA SCAIFE		EUR	7	AO7	CONSTRAINING THE THERMODYNAMIC STATE OF NEW PLANCK GALAXY CLUSTERS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807092010/	Quick Look
151	A3528-S OFFSET 4	194.1847	-30.0435	193.505704	-29.773143	205.130736	-22.019409	304.29690153	32.8141993	288.9992	56503.6527199074	2013-07-30 15:39:55	56504.4071064815	2013-07-31 09:46:14	808107010	32.7752	30	32.7832	32.7752	0	32.7912	3	2	0	2	1	0	0	31.2585	31.2585	65.1599	0	PROCESSED	57612.0918634259	2016-08-12 02:12:17	56955	2014-10-25 00:00:00	56587.7238310185	2013-10-22 17:22:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	082018	We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	8	AO8	TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808107010/	Quick Look
152	ABELL 2151A	241.1446	17.7141	240.581846	17.849628	234.487601	37.662842	31.46236827	44.65865226	285.8808	56883.5616898148	2014-08-14 13:28:50	56883.843900463	2014-08-14 20:15:13	809098010	11.0268	10	11.0348	11.0348	0	11.0268	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.4947569444	2016-08-16 11:52:27	57270	2015-09-05 00:00:00	56910.6327893518	2014-09-10 15:11:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809098010/	Quick Look
153	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
154	ALGOL	47.0831	40.8965	46.267674	40.705521	56.181748	22.363141	149.0355551	-14.93487401	244.4771	54167.6197222222	2007-03-08 14:52:24	54169.6132986111	2007-03-10 14:43:09	401093010	102.1642	105	102.1642	102.1642	0	102.1642	2	2	0	2	1	0	0	102.4729	102.4729	172.1928	1	PROCESSED	57537.6825810185	2016-05-29 16:22:55	54736	2008-09-27 00:00:00	54186.3983564815	2007-03-27 09:33:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012024	Stellar and solar coronae reveal high-energy phenomena including the presence of accelerated electrons, explosive dissipation of magnetic energy, and heating to extreme temperatures. Many of these processes are likely to be physically related. We propose to use Suzaku's suite of instruments to observe the interplay between thermal and non-thermal high-energy processes in the active, eclipsing binary Algol. Our prime objective is the observation of hard X-rays above 10 keV, but also the appearance of an Fe fluorescence line that could be induced either by irradiation from flaring plasma or by electron beams. These models can be distinguished by correlating the emission with nonthermal hard X-rays as possibly detected by the HXD.	GALACTIC POINT SOURCES	4	C	MANUEL GUEDEL		EUR	1	AO1	A SYNOPTIC VIEW OF HIGH-ENERGY PHENOMENA IN THE CORONA OF ALGOL	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401093010/	Quick Look
155	HER X-1	254.4925	35.2707	254.041525	35.346159	246.065216	57.427888	58.06565994	37.48335671	250.2455	55468.7003356482	2010-09-29 16:48:29	55469.2258912037	2010-09-30 05:25:17	405058020	24.303	20	24.303	24.3223	0	24.4677	2	2	0	1	1	0	0	22.4837	22.4837	45.4059	0	PROCESSED	57553.5917476852	2016-06-14 14:12:07	55848	2011-10-14 00:00:00	55482.4726967593	2010-10-13 11:20:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052001	We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity?	GALACTIC POINT SOURCES	4	B	R DIGER STAUBERT		EUR	5	AO5	VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405058020/	Quick Look
156	SGR 1806-20	272.166	-20.4729	271.421316	-20.481616	272.022208	2.952663	9.94279657	-0.27364584	269.9473	53987.9261921296	2006-09-09 22:13:43	53989.1668287037	2006-09-11 04:00:14	401092010	48.9155	50	48.9155	48.9235	48.9315	48.9315	1	1	1	1	1	0	0	55.4085	55.4085	107.1759	1	PROCESSED	57535.5272453704	2016-05-27 12:39:14	54526	2008-03-01 00:00:00	54021.1112615741	2006-10-13 02:40:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012017	The soft gamma-ray repeater SGR 1806-20 has recently emitted the most powerful giant flare ever observed from these sources. This probably involved a large scale restructuring of the magnetosphere, leading to observable variations in the properties of its persistent emission, from IR to hard X-rays. We propose to observe SGR 1806-20 with Suzaku considering the unique opportunity offered by this satellite to study the spectrum of this source simultaneously both in the soft and hard X-ray bands. We also suggest to coordinate this observation with a simultaneous XMM-Newton one, in order to obtain a significantly better determination of the broad band spectral parameters.	GALACTIC POINT SOURCES	4	B	SANDRO MEREGHETTI		EUR	1	AO1	COORDINATED SUZAKU AND XMM-NEWTON OBSERVATIONS OF SGR 1806-20 AFTER THE GIANT FLARE	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401092010/	Quick Look
157	IGR J08408-4503	130.2449	-45.0216	129.817019	-44.842502	154.934869	-59.72126	264.03123634	-1.90203871	133.4432	55176.7452199074	2009-12-11 17:53:07	55179.5002199074	2009-12-14 12:00:19	404070010	92.566	100	92.646	92.566	0	92.63	2	2	0	2	1	0	0	69.4344	69.4344	237.9898	2	PROCESSED	57549.8697222222	2016-06-10 20:52:24	55567	2011-01-06 00:00:00	55200.3941550926	2010-01-04 09:27:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042007	We propose a 100 ks Suzaku observation of a Supergiant Fast X-ray Transient (SFXT) displaying periodic outbursts, IGRJ08408-4503, with the main aim of searching for cyclotron lines in its spectrum.This would be the first direct measurement of the neutron star magnetic field in this recently discovered class of HMXBs, and would be crucial in discriminating between different models for the outburst mechanisms, involving highly magnetized neutron stars (1E14 G) versus more typical magnetic fields of 1E12 G.The source is a SFXT displaying recurrent outbursts on short timescales (flaring every about 11 and 24 days).Because in most SFXTs the outbursts are not predictable, fast and difficult to observe,the SFXT we are proposing is a key system to understand the physical properties of this class.	GALACTIC POINT SOURCES	4	C	LARA SIDOLI		EUR	4	AO4	SEARCH FOR CYCLOTRON LINES IN THE X-RAY SPECTRUM OF THE SUPERGIANT FAST X-RAY TRANSIENT IGRJ08408-4503	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404070010/	Quick Look
158	SN 1987A	83.9013	-69.2655	83.9928	-69.294887	307.391677	-86.458548	279.69660922	-31.92548266	330.0004	53894.6930555556	2006-06-08 16:38:00	53895.6683449074	2006-06-09 16:02:25	801090010	39.6464	40	39.6464	39.6464	39.6464	39.6464	2	2	2	2	1	0	0	39.2519	39.2519	84.2399	0	PROCESSED	57534.6267592593	2016-05-26 15:02:32	54400	2007-10-27 00:00:00	53928.1346527778	2006-07-12 03:13:54	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012006	In an early Suzaku observation during the SWG time in November 2005 we have already obtained an excellent XIS spectrum. The flux of SN 1987A continues to rise exponentially with an e-folding time of ~800 days. The abundances in the ejecta could be measured with unprecedented accuracy. We confirm that Oxygen and Iron are significantly underabundant with respect to other elements, indicating the formation of dust, maybe even black rust grains (Fe3O4). We propose to monitor the chemical evolution of SN 1987A with Suzaku for 40 ksec in AO-1, where we expect about twice the previous flux. The exponential brightening and the chemical abundance is expected to change, when the full inner ring is engulfed. Simultaneously we can search for a periodic hard signal from the putative pulsar.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	G NTHER HASINGER		EUR	1	AO1	SN 1987A - A RUSTY REMNANT?	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801090010/	Quick Look
159	VELAFRAGG TAIL	125.0448	-47.7009	124.65466	-47.541789	151.337516	-63.864294	264.09848727	-6.37839252	263.1844	55658.0366898148	2011-04-07 00:52:50	55658.8565162037	2011-04-07 20:33:23	506057010	49.3543	50	49.3703	49.3543	0	49.3703	3	2	0	2	1	0	0	43.9581	43.9581	70.8259	1	PROCESSED	57601.4287268518	2016-08-01 10:17:22	56043	2012-04-26 00:00:00	55673.1976736111	2011-04-22 04:44:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062021	The Vela supernova remnant (SNR) displays remarkable features which appear to be ejecta ``shrapnel'' visible beyond the main shell. One of these shrapnel (A) is distinct from the others in that its X-ray spectrum exhibits a high Si abundance, while the other shrapnel exhibit enhanced O, Ne, and Mg abundances. One unexplored ejecta shrapnel (G) is located on the opposite side of the remnant from shrapnel A, suggesting that the SN explosion may have resulted in a jet-counterjet Si-rich structure, reminiscent of Cas A. We propose to observe this shrapnel for the first time to determine if it is also Si-rich like shrapnel A. If this is the case, the Vela SNR may be the first direct evidence of a jet-induced SN explosion.	GALACTIC DIFFUSE EMISSION	5	A	FABRIZIO BOCCHINO		EUR	6	AO6	ASYMMETRIC SN EXPLOSION IN VELA SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506057010/	Quick Look
160	3C400.2 NW	294.5044	17.3912	293.942879	17.276968	300.273195	38.29194	53.66788209	-2.01364052	81.5888	56770.4644907407	2014-04-23 11:08:52	56770.9410763889	2014-04-23 22:35:09	509068010	21.47	20	21.4853	21.486	0	21.47	2	2	0	2	1	0	0	20.9678	20.9678	41.1719	0	PROCESSED	57614.9785416667	2016-08-14 23:29:06	57152	2015-05-10 00:00:00	56789.6036805556	2014-05-12 14:29:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092010	Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances.	GALACTIC DIFFUSE EMISSION	5	A	JACCO VINK		EUR	9	AO9	THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509068010/	Quick Look
161	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
162	LMC X-3	84.7483	-64.0713	84.678356	-64.09698	46.246737	-86.69028	273.56080053	-32.07680965	285.8008	56379.6769444445	2013-03-28 16:14:48	56382.4793634259	2013-03-31 11:30:17	407086010	101.809	100	101.817	101.825	0	101.809	2	2	0	2	1	0	0	92.7246	92.7246	242.1019	1	PROCESSED	57611.0169560185	2016-08-11 00:24:25	56757	2014-04-10 00:00:00	56391.8067592593	2013-04-09 19:21:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072002	We propose a 100 ksec triggered Suzaku observation of the low/hard state of the black hole LMC X-3. This will constrain the disc emission and Fe line profile in this state, both of which are currently very controversial. LMC X-3 has very low interstellar absorption, so gives the best view of the low temperature/low luminosity disc component in this state. Its moderate flux means it can be observed in standard imaging modes without pileup (further enhancing visibility of the disc as these modes are well calibrated down to 0.4 keV) and making the Fe line profile analysis straightforward. Historically LMC X-3 enters a low/hard state on average once a year. Suzaku will be triggered based on an alert from our Swift monitoring program that the source has entered the low/hard state.	GALACTIC POINT SOURCES	4	A	MARI KOLEHMAINEN		EUR	7	AO7-TOO	A TOO OF LMC X-3: IS THE DISC TRUNCATED IN THE LOW/HARD STATE OF BLACK HOLE BINARIES?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407086010/	Quick Look
163	A76 EAST	10.1332	6.8374	9.486956	6.563068	11.989309	2.27755	118.09579875	-55.93191571	260.0024	55183.3444212963	2009-12-18 08:15:58	55183.8752199074	2009-12-18 21:00:19	804087010	23.621	15	23.637	23.621	0	23.629	1	1	0	1	1	0	0	18.6401	18.6401	45.8559	0	PROCESSED	57549.8965393518	2016-06-10 21:31:01	55575	2011-01-14 00:00:00	55209.4624652778	2010-01-13 11:05:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042018	In our flux limited survey of galaxy clusters in the ROSAT All-Sky Atlas we find that about 5 - 10 percent of the galaxy clusters have a diffuse, low X-ray surface brightness. These objects could possibly be explained as dynamically very young clusters, which have not yet formed a central core. Three such clusters in our XMM-Newton study of an unbiased sub-sample of 33 galaxy clusters, REXCESS, show suprisingly high entropies in their centers which does not readily support the early formation stage. To shed more light on the nature of these clusters we propose to observe two extremely low surface brightness clusters at low redshift, for which we also have detailed optical data. SUZAKU with its low background is ideally suited for this study.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	HANS BOEHRINGER		EUR	4	AO4	SHEDDING LIGHT ON THE NATURE OF EXTREMELY LOW SURFACE BRIGHTNESS CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804087010/	Quick Look
164	A3526	192.0509	-41.0558	191.361267	-40.783129	208.811762	-32.67802	302.27518183	21.81182444	109.9986	55942.2296990741	2012-01-16 05:30:46	55942.6807291667	2012-01-16 16:20:15	806084010	16.9645	10	16.9645	16.9645	0	16.9645	2	2	0	2	1	0	0	12.6605	12.6605	38.9639	0	PROCESSED	57604.361875	2016-08-04 08:41:06	56331	2013-02-08 00:00:00	55960.1781712963	2012-02-03 04:16:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	062001	Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ANDREW FABIAN		EUR	6	AO6	TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806084010/	Quick Look
165	HYDRA A FAR N	139.5397	-11.7599	138.936601	-11.549023	146.034406	-26.083857	242.64361193	25.31151573	300.0007	56083.9377430556	2012-06-05 22:30:21	56085.1452662037	2012-06-07 03:29:11	807089010	41.276	40	41.284	41.284	0	41.276	2	2	0	2	1	0	0	38.1727	38.1727	104.3117	1	PROCESSED	57605.6201851852	2016-08-05 14:53:04	56465	2013-06-22 00:00:00	56098.4661689815	2012-06-20 11:11:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072020	Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DOMINIQUE ECKERT		EUR	7	AO7	MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807089010/	Quick Look
166	MKW8	220.1793	3.4582	219.549704	3.671881	216.616533	18.149831	355.49716412	54.76401984	291.2239	56859.4682986111	2014-07-21 11:14:21	56859.7009259259	2014-07-21 16:49:20	809101010	10.412	10	10.412	10.488	0	10.4956	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57615.4174305556	2016-08-15 10:01:06	57239	2015-08-05 00:00:00	56873.5532523148	2014-08-04 13:16:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092015	Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	LORENZO LOVISARI		EUR	9	AO9	SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809101010/	Quick Look
167	3C400.2 NE	294.7841	17.3445	294.222174	17.229031	300.592872	38.189932	53.75798011	-2.26924911	81.5891	56770.0289351852	2014-04-23 00:41:40	56770.4640162037	2014-04-23 11:08:11	509071010	20.231	20	20.239	20.239	0	20.231	1	1	0	1	1	0	0	18.505	18.505	37.5838	0	PROCESSED	57614.9798148148	2016-08-14 23:30:56	57152	2015-05-10 00:00:00	56789.6056712963	2014-05-12 14:32:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	092010	Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances.	GALACTIC DIFFUSE EMISSION	5	A	JACCO VINK		EUR	9	AO9	THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509071010/	Quick Look
168	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
169	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
170	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
171	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
172	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
173	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
174	J2218.2-0350	334.573	-3.8385	333.923892	-4.08927	335.019924	6.258076	58.63251599	-46.67973864	268.0005	56260.6621527778	2012-11-29 15:53:30	56261.0523148148	2012-11-30 01:15:20	807084010	15.7671	15	15.7751	15.7671	0	15.7831	2	2	0	2	1	0	0	11.9145	11.9145	33.7079	0	PROCESSED	57608.1412384259	2016-08-08 03:23:23	56644	2013-12-18 00:00:00	56275.6610300926	2012-12-14 15:51:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072018	We propose to observe the three clusters of galaxies J2218.2-0350, J2218.6-0346 and J2218.8-0258 with exposure times of 15, 25 and 35 ks respectively. These clusters are part of a structure of four linearly aligned clusters, separated from each other by 4 to 10 Mpc. We will accurately determine their masses and orientation. This will allow us to fully map the tidal force field of the structure, which is the prime force behind the formation of filaments in the cosmic web. We will study the effects of cluster mass, separation and mutual orientation on the filamentary structure of the cosmic web and on the evolution of galaxies therein.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	E.G. PATRICK BOS		EUR	7	AO7	CLUSTERS AND THE COSMIC WEB	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807084010/	Quick Look
175	G276.2-7.7	135.4479	-58.0976	135.120843	-57.899721	179.6274	-67.871169	276.2324482	-7.68832918	319.4197	56102.2534722222	2012-06-24 06:05:00	56102.610625	2012-06-24 14:39:18	507066010	10.2994	10	10.2994	10.2994	0	10.2994	1	1	0	1	1	0	0	11.6275	11.6275	30.8559	0	PROCESSED	57605.7340972222	2016-08-05 17:37:06	56582	2013-10-17 00:00:00	56219.6536458333	2012-10-19 15:41:15	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072014	We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed.	GALACTIC DIFFUSE EMISSION	5	A	TOBIAS PRINZ		EUR	7	AO7	IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507066010/	Quick Look
176	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
177	XB 1916-053	289.7027	-5.2415	289.037629	-5.333849	290.520863	16.806325	31.35614078	-8.46800846	250.2538	54047.242974537	2006-11-08 05:49:53	54048.1119791667	2006-11-09 02:41:15	401095010	38.4647	40	39.0967	39.0887	38.4647	39.0967	2	2	2	2	1	0	0	37.4857	37.4857	75.082	2	PROCESSED	57536.0684259259	2016-05-28 01:38:32	54735	2008-09-26 00:00:00	54088.866087963	2006-12-19 20:47:10	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	012038	We propose Suzaku observations of the dipping low mass X-ray binaries XB1916-053, XB1323-619, EXO0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been recently demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the photoionised absorbers and reliably determine the values of the ionization parameter for each source, and the simultaneous spectra of HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components and to extend the photoionized absorber fits to higher energies. This will test the validity of the ionized absorber model also >10 keV.	GALACTIC POINT SOURCES	4	A	MARIA DIAZ TRIGO		EUR	1	AO1	BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401095010/	Quick Look
178	4U 1820-30	275.9205	-30.4212	275.116914	-30.447977	275.132756	-7.085901	2.7347979	-7.94197311	270.4164	55124.2356134259	2009-10-20 05:39:17	55124.7925810185	2009-10-20 19:01:19	404069070	24.0566	100	24.0567	24.0726	0	24.0566	3	1	0	2	1	0	0	18.9035	18.9035	48.1079	0	PROCESSED	57548.9193981482	2016-06-09 22:03:56	55503	2010-11-03 00:00:00	55134.2427314815	2009-10-30 05:49:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	042004	Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		EUR	4	AO4	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404069070/	Quick Look
179	HER X-1	254.4936	35.2712	254.042629	35.346654	246.066668	57.428555	58.06646448	37.48255114	250.0637	55467.7830208333	2010-09-28 18:47:33	55468.2362962963	2010-09-29 05:40:16	405058010	21.3567	20	21.3567	21.3567	0	21.5034	2	2	0	1	1	0	0	18.9323	18.9323	39.1599	0	PROCESSED	57553.5804050926	2016-06-14 13:55:47	55843	2011-10-09 00:00:00	55477.2237152778	2010-10-08 05:22:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	052001	We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity?	GALACTIC POINT SOURCES	4	B	R DIGER STAUBERT		EUR	5	AO5	VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405058010/	Quick Look
180	V2129 OPH	246.9149	-24.3651	246.158782	-24.254235	249.041959	-2.587504	353.29078542	16.72506486	88.3342	54866.0202430556	2009-02-04 00:29:09	54866.5821296296	2009-02-04 13:58:16	403074010	21.0335	20	21.0335	21.0335	0	21.0335	2	2	0	2	1	0	0	16.5331	16.5331	48.5339	0	PROCESSED	57545.4470833333	2016-06-06 10:43:48	55329	2010-05-13 00:00:00	54880.5317708333	2009-02-18 12:45:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	032022	We propose to observe the classical T Tauri stars CS Cha, MN Lup, V2129 Oph and XZ Tau with the Suzaku XIS to investigate accretion induced X-ray emission in CTTS as evidenced by the presence of excess emission in the soft X-ray regime. Specifically we intend to utilize Suzaku's sensitivity, low background and the capability of the XIS to resolve the OVIII Ly-alpha line from the OVII triplet. XMM-Newton and Chandra grating spectra provide strong evidence for the presence of accretion induced X-ray emission in CTTS, however, due to low SNR and the presence of absorption an accretion scenario often cannot be probed within reasonable exposure times. With the proposed observations we want to investigate a sample of these CTTS showing additional exceptional properties.	GALACTIC POINT SOURCES	4	B	JAN ROBRADE		EUR	3	AO3	ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403074010/	Quick Look
181	HYDRA A SE	139.5641	-12.2366	138.96256	-12.025643	146.239045	-26.524458	243.07517911	25.03717361	300.0006	56085.6674421296	2012-06-07 16:01:07	56086.2926388889	2012-06-08 07:01:24	807087010	21.4898	20	21.4898	21.4898	0	21.4898	2	2	0	2	1	0	0	20.3651	20.3651	54.012	0	PROCESSED	57605.6279976852	2016-08-05 15:04:19	56465	2013-06-22 00:00:00	56099.0036921296	2012-06-21 00:05:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	072020	Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DOMINIQUE ECKERT		EUR	7	AO7	MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807087010/	Quick Look

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