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 998

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	E0102-72	15.9926	-72.0236	15.587314	-72.291594	314.630688	-65.030221	301.56327722	-45.07133229	226.8326	53720.0716203704	2005-12-16 01:43:08	53723.4377199074	2005-12-19 10:30:19	100044010	59.731	20	59.735	125.9195	59.731	59.737	3	3	3	3	1	0	0	115.3302	115.3302	290.8037	1	PROCESSED	57532.5803935185	2016-05-24 13:55:46	54247	2007-05-27 00:00:00	54119.7612615741	2007-01-19 18:16:13	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001097	We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	0	SWG	XIS FLIGHT CAIBRATION PLAN		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100044010/	Quick Look
2	ABELL 773	139.3092	51.8461	138.434684	52.055757	124.471508	34.139728	165.95348434	43.2527698	276.9988	55684.9096412037	2011-05-03 21:49:53	55685.7363541667	2011-05-04 17:40:21	806027040	49.8691	50	49.8805	49.8771	0	49.8691	2	2	0	2	1	0	0	44.1285	44.1285	71.422	1	PROCESSED	57601.942962963	2016-08-01 22:37:52	55652	2011-04-01 00:00:00	55697.3061458333	2011-05-16 07:20:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806027040/	Quick Look
3	GX 349+2	256.427	-36.366	255.587548	-36.298664	258.786235	-13.451096	349.14511841	2.78820606	85.6584	53808.5453240741	2006-03-14 13:05:16	53809.2216782407	2006-03-15 05:19:13	400003010	25.2308	50	25.2308	25.2332	25.2308	25.2308	1	1	1	1	1	0	0	20.0507	20.0507	58.434	2	PROCESSED	57533.2006365741	2016-05-25 04:48:55	54247	2007-05-27 00:00:00	54041.9132060185	2006-11-02 21:55:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001026	We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure.	GALACTIC POINT SOURCES	4	A	HIROMITSU TAKAHASHI		JAP	0	SWG	SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES)	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400003010/	Quick Look
4	SS CYG	325.6789	43.5736	325.187819	43.344381	350.451149	52.649921	90.55119171	-7.12024619	276.5788	53676.0503703704	2005-11-02 01:12:32	53676.9856944444	2005-11-02 23:39:24	400006010	39.4512	40	39.4512	39.4512	39.4512	39.4512	2	2	2	2	1	0	0	32.0472	32.0472	80.81	1	PROCESSED	57527.7175925926	2016-05-19 17:13:20	54247	2007-05-27 00:00:00	54036.9898148148	2006-10-28 23:45:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001043	Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst.	GALACTIC POINT SOURCES	4	A	MANABU ISHIDA		JAP	0	SWG	SS CYG OBSERVATION IN QUIESCENCE		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400006010/	Quick Look
5	X1630-472	248.4706	-47.343	247.550146	-47.238721	254.054156	-25.085181	336.93140696	0.30212129	69.0657	53781.9791087963	2006-02-15 23:29:55	53782.5474305556	2006-02-16 13:08:18	400010020	21.429	200	21.429	21.485	21.429	21.429	2	2	2	2	1	0	0	17.0223	17.0223	49.1019	0	PROCESSED	57533.0117592593	2016-05-25 00:16:56	54247	2007-05-27 00:00:00	54041.4892013889	2006-11-02 11:44:27	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001058	We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		JAP	0	SWG-TOO	FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010020/	Quick Look
6	JUPITER	226.5694	-16.1887	225.870685	-15.99606	228.664382	1.239883	343.96536778	35.7224308	118.4901	53790.7643402778	2006-02-24 18:20:39	53791.7940277778	2006-02-25 19:03:24	401001010	37.7594	36	37.7674	37.7594	37.7674	37.7674	2	2	2	2	1	0	0	32.8361	32.8361	88.9361	1	PROCESSED	57533.0781597222	2016-05-25 01:52:33	54401	2007-10-28 00:00:00	53905.533900463	2006-06-19 12:48:49	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011003	We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure.	GALACTIC POINT SOURCES	4	C	RONALD ELSNER		USA	1	AO1	JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001010/	Quick Look
7	COMET_8P_TUTTLE-P2_08	40.0642	-36.6693	39.55682	-36.883219	21.03457	-48.879704	242.2833952	-65.12116443	253.2206	54490.9649421296	2008-01-25 23:09:31	54491.0959953704	2008-01-26 02:18:14	502063080	3.5416	4	3.5496	3.5416	0	3.5576	2	2	0	2	1	0	0	3.564	3.564	11.3119	0	PROCESSED	57541.3990509259	2016-06-02 09:34:38	54912	2009-03-22 00:00:00	54546.1411689815	2008-03-21 03:23:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063080/	Quick Look
8	NGC 4051	180.8556	44.5807	180.217538	44.859022	159.275193	40.404023	148.68917976	70.06918189	135.3482	53684.8015509259	2005-11-10 19:14:14	53687.4315277778	2005-11-13 10:21:24	700004010	119.578	150	119.61	119.61	119.586	119.578	2	2	2	2	1	0	0	120.0047	120.0047	227.1918	3	PROCESSED	57528.0225810185	2016-05-20 00:32:31	54247	2007-05-27 00:00:00	54037.5713078704	2006-10-29 13:42:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001012	We propose to obtain a broad band spectrum of the narrow-line Seyfert 1 (NLS1) NGC 4051. NLS1s are often presumed that they host a relatively small black hole with a very high accretion rate. Such a class would have played an important role in the growth of black holes in a cosmological context. We will measure the intrinsic photon index, amount of reflection, and high energy cutoff for the first time to investigate an accretion disk under a high accretion rate and compare them with conventional broad-line Seyferts.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	0	SWG	THE ACCRETION IN THE NARROW-LINE SEYFERT 1 NGC 4051 PROBED BY A BROAD BAND SPECTRUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700004010/	Quick Look
9	HR 9024	357.4125	36.4308	356.782155	36.152799	14.165064	34.009987	109.27773456	-24.79729068	49.8624	53939.0616782407	2006-07-23 01:28:49	53940.6016087963	2006-07-24 14:26:19	401032010	58.7757	60	58.7997	58.7757	58.7837	58.7917	2	2	2	2	1	0	0	56.0116	56.0116	133.0398	1	PROCESSED	57535.042025463	2016-05-27 01:00:31	54401	2007-10-28 00:00:00	53950.2624074074	2006-08-03 06:17:52	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011022	Suzaku-XIS is the best available instrument to study the Fe fluorescence emission from late-type evolved stars. Fe fluorescence is produced by illumination of the photosphere by ionizing coronal X-rays and its intensity depends on the height of the X-ray source. We propose to observe Fe fluorescence in the single G-type giant HR 9024 and in the active RS CVn system II Peg to obtain a direct geometrical constraint on the scale height of their coronal structures. These two stars have the brightest Fe fluorescence features of all the late-type stars observed by the Chandra-HETGS and their different stellar parameters (stellar radius, gravity, multiplicity,..) and evolutionary stage will allow us to probe the typical coronal scale for significantly different conditions.	GALACTIC POINT SOURCES	4	B	PAOLA TESTA		USA	1	AO1	GEOMETRY DIAGNOSTICS FROM FE FLUORESCENT EMISSION IN LATE-TYPE EVOLVED STARS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401032010/	Quick Look
10	BETA LYR	282.5098	33.3716	282.047998	33.312385	288.857806	55.996493	63.19266924	14.79477853	53.4974	53867.1260185185	2006-05-12 03:01:28	53867.6252199074	2006-05-12 15:00:19	401036020	21.4962	20	21.4962	21.4962	21.4962	21.4962	1	1	1	1	1	0	0	19.1642	19.1642	43.1199	2	PROCESSED	57534.2764814815	2016-05-26 06:38:08	54401	2007-10-28 00:00:00	53914.2784143518	2006-06-28 06:40:55	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011031	The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse.	GALACTIC POINT SOURCES	4	A	RICHARD IGNACE		USA	1	AO1	AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036020/	Quick Look
11	4U 1705-44	257.2295	-44.1004	256.326357	-44.0367	260.194477	-21.092135	343.32321952	-2.34240238	264.0794	53976.2429166667	2006-08-29 05:49:48	53976.7731712963	2006-08-29 18:33:22	401046010	18.3155	20	18.3155	18.3155	18.3155	18.3155	2	2	2	2	1	0	0	15.3715	15.3715	45.8099	0	PROCESSED	57535.3889236111	2016-05-27 09:20:03	54526	2008-03-01 00:00:00	54021.306087963	2006-10-13 07:20:46	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011112	We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state.	GALACTIC POINT SOURCES	4	A	ANDREW YOUNG		USA	1	AO1	REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046010/	Quick Look
12	4U 1636-536	250.2262	-53.7541	249.22979	-53.657603	256.460667	-31.236861	332.91086545	-4.81751491	91.2457	54140.3877546296	2007-02-09 09:18:22	54140.99125	2007-02-09 23:47:24	401050010	24.232	19	24.232	24.232	0	24.232	2	1	0	2	1	0	0	21.6895	21.6895	52.136	0	PROCESSED	57537.3410069445	2016-05-29 08:11:03	54525	2008-02-29 00:00:00	54151.5052893518	2007-02-20 12:07:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011117	Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.	GALACTIC POINT SOURCES	4	A	JEROEN HOMAN		USA	1	AO1	THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050010/	Quick Look
13	IGRJ16195-4945	244.8541	-49.816	243.916706	-49.695602	251.909406	-27.940354	333.49117084	0.29973526	284.0301	53998.8508333333	2006-09-20 20:25:12	53999.7231481482	2006-09-21 17:21:20	401056010	39.1486	40	39.1486	39.1486	39.1486	39.1486	2	2	2	2	1	0	0	42.2652	42.2652	75.3579	1	PROCESSED	57535.652662037	2016-05-27 15:39:50	54526	2008-03-01 00:00:00	54020.9227199074	2006-10-12 22:08:43	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011132	INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	1	AO1	HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401056010/	Quick Look
14	CYGNUS X-1	299.6124	35.133	299.141904	34.996436	313.652571	54.178807	71.28577556	3.01567368	256.2202	54038.1501273148	2006-10-30 03:36:11	54038.8225	2006-10-30 19:44:24	401059010	27.7068	30	27.7068	27.7378	27.7068	27.7068	2	1	2	2	1	0	0	27.6892	27.6892	58.0839	0	PROCESSED	57535.9949768518	2016-05-27 23:52:46	54526	2008-03-01 00:00:00	54063.4924884259	2006-11-24 11:49:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011141	We request three, 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history.	GALACTIC POINT SOURCES	4	B	MICHAEL NOWAK		USA	1	AO1	ENHANCING THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401059010/	Quick Look
15	EV LAC	341.7127	44.3232	341.158134	44.059332	6.045133	46.919235	100.60502245	-13.08073089	256.1601	54432.9692013889	2007-11-28 23:15:39	54434.4655208333	2007-11-30 11:10:21	402032010	68.9493	100	68.9493	69.1333	0	69.1275	2	1	0	2	1	0	0	65.0113	65.0113	129.2328	2	PROCESSED	57540.7939236111	2016-06-01 19:03:15	54808	2008-12-08 00:00:00	54441.0876851852	2007-12-07 02:06:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021013	We propose a 100 ks Suzaku XIS observation of the dMe flare star EV Lac to measure coronal element abundances during quiescence and flares of different sizes. EV Lac undergoes frequent small flares, and is known to have undergone a very large flare at ~300 times the quiescent count rate in 2000. Coronal abundance changes shed light on the process of chromospheric evaporation under conditions different to those on the Sun. Depending on the size and spectrum of the flare, we may also be able to detect a hard burst of emission that would serve as a time marker for particle acceleration during the flare.	GALACTIC POINT SOURCES	4	C	UNA HWANG		USA	2	AO2	FLARE AND QUIESENT CONORAL ELEMENT ABUNDANCES IN EV LAC	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402032010/	Quick Look
16	VY AQR	318.0426	-8.8307	317.372404	-9.036659	317.753092	7.00586	41.59091784	-35.22055705	252.6652	54414.6528587963	2007-11-10 15:40:07	54415.3855787037	2007-11-11 09:15:14	402043010	25.4473	20	25.4473	25.4473	0	25.4473	2	2	0	2	1	0	0	22.3605	22.3605	63.2999	2	PROCESSED	57540.476712963	2016-06-01 11:26:28	54790	2008-11-20 00:00:00	54423.1702314815	2007-11-19 04:05:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021105	Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies.	GALACTIC POINT SOURCES	4	C	KOJI MUKAI		USA	2	AO2	BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402043010/	Quick Look
17	HOLMBERG IX X-1	149.4869	69.0752	148.468802	69.313718	119.773156	51.703341	141.91661656	41.06840873	124.5	56224.1252199074	2012-10-24 03:00:19	56226.4168981482	2012-10-26 10:00:20	707019030	106.9454	500	106.9454	106.9534	0	106.9614	2	2	0	2	1	0	0	105.0119	105.0119	197.9478	1	PROCESSED	57607.8725462963	2016-08-07 20:56:28	56018	2012-04-01 00:00:00	56240.5429050926	2012-11-09 13:01:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071251	Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy.	EXTRAGALACTIC COMPACT SOURCES	7	A	JON MILLER		USA	7	AO7	A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019030/	Quick Look
18	4U1705-44	257.2229	-44.1035	256.319735	-44.039768	260.189733	-21.095668	343.31790137	-2.34044351	107.4157	54543.8610532407	2008-03-18 20:39:55	54544.5210532407	2008-03-19 12:30:19	402051040	20.0744	15	20.0744	20.0744	0	20.0824	2	1	0	2	1	0	0	13.4113	13.4113	57.0179	1	PROCESSED	57541.899525463	2016-06-02 21:35:19	54922	2009-04-01 00:00:00	54553.1912268518	2008-03-28 04:35:22	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021113	We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability.	GALACTIC POINT SOURCES	4	A	RONALD REMILLARD		USA	2	AO2	X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402051040/	Quick Look
19	2S 0921-630	140.6655	-63.298	140.375275	-63.083061	195.139147	-68.890832	281.84446964	-9.33525426	8.3442	54335.887025463	2007-08-23 21:17:19	54336.9932175926	2007-08-24 23:50:14	402059010	43.131	40	43.131	43.131	0	43.131	2	2	0	2	1	0	0	37.1622	37.1622	95.5598	0	PROCESSED	57539.6661805556	2016-05-31 15:59:18	54721	2008-09-12 00:00:00	54350.5504861111	2007-09-07 13:12:42	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021118	2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		USA	2	AO2	PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402059010/	Quick Look
20	2S 0921-630	140.666	-63.2982	140.375774	-63.08326	195.139946	-68.890744	281.84477381	-9.33523447	8.344	54338.0511226852	2007-08-26 01:13:37	54339.16	2007-08-27 03:50:24	402060010	40.3423	40	40.3503	40.3423	0	40.3503	1	1	0	1	1	0	0	35.6464	35.6464	95.7999	2	PROCESSED	57539.6728703704	2016-05-31 16:08:56	54721	2008-09-12 00:00:00	54350.5629398148	2007-09-07 13:30:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021118	2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		USA	2	AO2	PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402060010/	Quick Look
21	IGR J17391-3021	264.795	-30.3419	263.992133	-30.314694	265.466386	-6.982553	358.06793122	0.44854091	89.216	54518.4950115741	2008-02-22 11:52:49	54519.3961226852	2008-02-23 09:30:25	402066010	36.4657	30	36.5457	36.5937	0	36.4657	2	2	0	2	1	0	0	31.2591	31.2591	77.8198	1	PROCESSED	57541.7105671296	2016-06-02 17:03:13	54892	2009-03-02 00:00:00	54525.5064699074	2008-02-29 12:09:19	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021122	We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities.	GALACTIC POINT SOURCES	4	B	JOHN TOMSICK		USA	2	AO2	LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402066010/	Quick Look
22	CIRCINUS X-1	230.1633	-57.1695	229.194668	-56.989293	244.120639	-37.250007	322.11384942	0.03740334	115.206	54530.1953240741	2008-03-05 04:41:16	54531.5523032407	2008-03-06 13:15:19	402070010	46.4113	43	46.4113	46.4113	0	46.4113	2	2	0	2	1	0	0	41.8213	41.8213	117.196	0	PROCESSED	57541.8053125	2016-06-02 19:19:39	54916	2009-03-26 00:00:00	54550.2459953704	2008-03-25 05:54:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021128	We propose a 100ks Suzaku observation of Circinus X-1 through the zero (dipping) phase to facilitate 2 important and independent science goals. (1) For the binary, we wish to better understand the viewing geometry, and investigate physical changes in the binary behavior as it relates to observed spectral changes through periastron passage. (2) Conduct a large angle scattering study of the X-ray halo surrounding Circinus X-1 to diagnose ISM grain properties (the line-of-sight position, size distribution, and grain density) near us, in complement with our Chandra halo studies at small angles on grain properties near the source.	GALACTIC POINT SOURCES	4	A	JULIA LEE		USA	2	AO2	CIRCINUS X-1 NEAR PERIASTRON: PROBING BINARY PHYSICS AND ISM GRAINS ALONG THE LINE OF SIGHT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402070010/	Quick Look
23	CYG X-1	299.5451	35.2618	299.075532	35.125519	313.637974	54.318601	71.3671857	3.12971485	59.9371	54237.8204050926	2007-05-17 19:41:23	54238.6480787037	2007-05-18 15:33:14	402072020	33.3568	30	33.3568	33.3649	0	33.3568	2	1	0	2	1	0	0	32.5637	32.5637	71.5039	1	PROCESSED	57538.696724537	2016-05-30 16:43:17	54695	2008-08-17 00:00:00	54245.0149884259	2007-05-25 00:21:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021133	We request two additional 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history.	GALACTIC POINT SOURCES	4	A	MICHAEL NOWAK		USA	2	AO2	CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402072020/	Quick Look
24	CAS A	350.8761	58.8091	350.310124	58.534509	27.390357	54.841399	111.74552355	-2.13963884	214.5537	53783.6003472222	2006-02-17 14:24:30	53783.9218055556	2006-02-17 22:07:24	100043020	14.155	10	14.155	14.155	14.155	14.155	1	1	1	1	1	0	0	17.3713	17.3713	27.768	0	PROCESSED	57533.0311805556	2016-05-25 00:44:54	54247	2007-05-27 00:00:00	54041.4627893518	2006-11-02 11:06:25	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001097	We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	0	SWG	XIS FLIGHT CAIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100043020/	Quick Look
25	TAU SCO	248.9736	-28.2151	248.194076	-28.113426	251.450456	-6.117318	351.53721955	12.80675658	279.3712	54723.4207291667	2008-09-14 10:05:51	54723.8119675926	2008-09-14 19:29:14	403034030	12.2902	10	12.2982	12.2982	0	12.2902	1	1	0	1	1	0	0	11.0282	11.0282	33.7999	0	PROCESSED	57543.8133564815	2016-06-04 19:31:14	55148	2009-11-13 00:00:00	54780.4631597222	2008-11-10 11:06:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031121	We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars.	GALACTIC POINT SOURCES	4	A	RICHARD IGNACE		USA	3	AO3	X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403034030/	Quick Look
26	ETA CARINAE	161.2297	-59.7314	160.743721	-59.468116	202.194195	-58.967017	287.60304523	-0.67930865	294	54627.0775	2008-06-10 01:51:36	54627.649525463	2008-06-10 15:35:19	403035010	35.4479	30	35.4639	35.4479	0	35.4639	2	2	0	2	1	0	0	27.2102	27.2102	49.4159	1	PROCESSED	57542.7628819445	2016-06-03 18:18:33	55003	2009-06-21 00:00:00	54637.2680092593	2008-06-20 06:25:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031124	X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009).	GALACTIC POINT SOURCES	4	A	KENJI HAMAGUCHI		USA	3	AO3	X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403035010/	Quick Look
27	ETA CARINAE	161.3639	-59.6742	160.876523	-59.410706	202.202933	-58.878505	287.63630523	-0.59715454	170.6228	54877.528287037	2009-02-15 12:40:44	54878.4119675926	2009-02-16 09:53:14	403038010	35.5525	30	35.5685	35.5525	0	35.5605	2	2	0	2	1	0	0	31.1193	31.1193	76.3239	1	PROCESSED	57545.5564814815	2016-06-06 13:21:20	55328	2010-05-12 00:00:00	54893.4307407407	2009-03-03 10:20:16	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031124	X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009).	GALACTIC POINT SOURCES	4	A	KENJI HAMAGUCHI		USA	3	AO3	X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403038010/	Quick Look
28	SS73 17	152.7399	-57.7545	152.30201	-57.507445	193.309145	-60.825813	282.81739372	-1.29143094	80.1552	54775.6877430556	2008-11-05 16:30:21	54776.3072453704	2008-11-06 07:22:26	403043010	24.907	20	24.907	24.907	0	24.907	2	2	0	2	1	0	0	20.8091	20.8091	53.5199	0	PROCESSED	57544.3629282407	2016-06-05 08:42:37	55157	2009-11-22 00:00:00	54791.6362847222	2008-11-21 15:16:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031145	SS73 17 was an innocuous Mira-type symbiotic star until INTEGRAL and Swift discovered its bright hard X-ray emission. Suzaku observations showed it emits three bright iron lines, with almost no emission in the 0.5-2 keV bandpass. The PI has an approved 100 ksec Chandra HETG observation in 2008 to determine the origin of the iron lines and measure any weak emission lines. With simultaneous Suzaku observations we will also measure the hard X-ray emission from the source, both to constrain the continuum and detect any non-thermal component. The effective areas of the XIS and HXD will constrain the broadband emission process much better than the HETG data. Combined with simultaneous optical observations of the Mira-type star we will determine the origin of this star's unusual emission.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	3	AO3	SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS OF THE SYMBIOTIC STAR SS73 17	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403043010/	Quick Look
29	1A1118-61	170.3215	-61.8847	169.770459	-61.610411	210.906306	-57.212373	292.5244731	-0.84831529	142.606	54859.2344328704	2009-01-28 05:37:35	54859.8925810185	2009-01-28 21:25:19	403050010	44.2125	45	44.2125	44.2125	0	44.2125	2	2	0	2	1	0	0	30.9154	30.9154	56.8599	0	PROCESSED	57545.3633680556	2016-06-06 08:43:15	55328	2010-05-12 00:00:00	54880.5326273148	2009-02-18 12:46:59	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031155	We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku AO3. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line in this system and to determine its broad band spectrum.	GALACTIC POINT SOURCES	4	A	KATJA POTTSCHMIDT		USA	3	AO3-TOO	SEARCHING FOR CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403050010/	Quick Look
30	CYG X-1	299.5797	35.2714	299.110135	35.134972	313.689122	54.31814	71.39012673	3.11059703	84.4565	54574.6816898148	2008-04-18 16:21:38	54575.4238425926	2008-04-19 10:10:20	403065010	33.9435	30	33.9435	33.9782	0	33.9703	1	1	0	2	1	0	0	28.9556	28.9556	64.118	0	PROCESSED	57542.3725231482	2016-06-03 08:56:26	54957	2009-05-06 00:00:00	54587.2117476852	2008-05-01 05:04:55	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031172	We request two 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku brings three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 100-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history.	GALACTIC POINT SOURCES	4	A	MICHAEL NOWAK		USA	3	AO3	CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN IN THE SUZAKU ERA	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403065010/	Quick Look
31	V773 TAU	63.5591	28.1916	62.7857	28.065974	66.717215	6.863448	168.22897578	-16.34488481	264.3183	55255.9666550926	2010-02-28 23:11:59	55258.750162037	2010-03-03 18:00:14	404037010	115.4057	120	115.4057	115.4057	0	115.4057	2	2	0	2	1	0	0	95.563	95.563	240.4667	1	PROCESSED	57550.8499189815	2016-06-11 20:23:53	55637	2011-03-17 00:00:00	55271.499537037	2010-03-16 11:59:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041203	Young stars display magnetic activity at the extreme of that produced in nearby active stars and the Sun, making them useful tools to probe the dominant physical processes controlling such activity. The unique features of V773 Tau's X-ray and radio properties (frequent X-ray flaring of highly energetic flares, extreme nonthermal radio emission) mark it as one of the most active young stars. We seek coordinated Suzaku and mm wavelength observations to probe the interplay between the hot plasma and the stellar environment. We focus on utilizing the unique capabilities of Suzaku, namely the spectral resolution and sensitivity at 5--10 keV, to elucidate the properties of its hot plasma and its potential effects on the stellar environment such as detecting Fe fluorescence.	GALACTIC POINT SOURCES	4	C	RACHEL OSTEN		USA	4	AO4	X-RAY EMISSION AND THE STELLAR ENVIRONMENT AROUND THE PRE-MAIN SEQUENCE BINARY V773 TAU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404037010/	Quick Look
32	ETA CARINAE	161.2575	-59.6351	160.770713	-59.371773	202.076586	-58.890955	287.57052339	-0.58758586	87.8919	55156.1883449074	2009-11-21 04:31:13	55157.3196643518	2009-11-22 07:40:19	404039010	49.3887	45	49.3887	49.3887	0	49.3887	2	2	0	2	1	0	0	34.2553	34.2553	97.7201	0	PROCESSED	57549.5287152778	2016-06-10 12:41:21	55542	2010-12-12 00:00:00	55176.3651388889	2009-12-11 08:45:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041204	The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements.	GALACTIC POINT SOURCES	4	A	KENJI HAMAGUCHI		USA	4	AO4	HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CAR	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404039010/	Quick Look
33	GRS 1758-258	270.2971	-25.679	269.522467	-25.678561	270.258372	-2.238361	4.56169204	-1.32563061	89.3817	55263.8983333333	2010-03-08 21:33:36	55266.0711111111	2010-03-11 01:42:24	404060010	82.6827	80	82.6827	82.6827	0	82.6827	2	2	0	2	1	0	0	71.1789	71.1789	187.7097	1	PROCESSED	57550.8664583333	2016-06-11 20:47:42	55647	2011-03-27 00:00:00	55279.5468402778	2010-03-24 13:07:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041244	We propose an 80 ks observation to obtain a broadband spectrum of the Galactic microquasar GRS 1758-258 while in the low-hard state with Suzaku. Here we aim to constrain the nature and geometry of the accretion flow via measurements of the various disc reflection features, which are detectable for the first time due to the unique capabilities of Suzaku. As this system is known to power large radio jets, its study will also aid our understanding of the conditions necessary for the formation of relativistic outflows and how these relate to the accretion geometry in the low-hard state.	GALACTIC POINT SOURCES	4	B	MARK REYNOLDS		USA	4	AO4	CONSTRAINING DISC REFLECTION IN THE MICROQUASAR GRS 1758-258	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404060010/	Quick Look
34	LMC X-1	84.947	-69.7479	85.058791	-69.772179	298.110491	-86.30257	280.20680376	-31.50316575	10.0004	55033.776724537	2009-07-21 18:38:29	55036.8953587963	2009-07-24 21:29:19	404061010	129.8679	120	129.8679	129.8679	0	129.8679	2	2	0	2	1	0	0	132.5976	132.5976	269.3956	4	PROCESSED	57548.0199537037	2016-06-09 00:28:44	55419	2010-08-11 00:00:00	55048.6509143518	2009-08-05 15:37:19	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041245	We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability.	GALACTIC POINT SOURCES	4	A	JEFFREY MCCLINTOCK		USA	4	AO4	MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404061010/	Quick Look
35	LMC X-3	84.7128	-64.0821	84.643099	-64.107952	45.920225	-86.688866	273.5746003	-32.09166858	184.4521	55186.5265162037	2009-12-21 12:38:11	55190.9105555556	2009-12-25 21:51:12	404062010	154.4242	150	154.434	154.434	0	154.4242	2	2	0	2	1	0	0	101.1721	101.1721	352.1458	2	PROCESSED	57550.1364930556	2016-06-11 03:16:33	55587	2011-01-26 00:00:00	55218.7384375	2010-01-22 17:43:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041245	We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability.	GALACTIC POINT SOURCES	4	C	JEFFREY MCCLINTOCK		USA	4	AO4	MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404062010/	Quick Look
36	EG AND	11.168	40.673	10.482613	40.399604	27.902454	32.653699	121.54657283	-22.18054863	225.2111	55597.6281018518	2011-02-05 15:04:28	55600.0030092593	2011-02-08 00:04:20	405034010	100.5333	100	100.5333	100.5413	0	100.5493	2	2	0	2	1	0	0	84.6589	84.6589	205.1719	3	PROCESSED	57600.9241666667	2016-07-31 22:10:48	55983	2012-02-26 00:00:00	55614.2972106482	2011-02-22 07:07:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051211	The goals of this proposal are to use Suzaku XIS observations to : 1) determine whether EG And, BX Mon, and BF Cyg are members of the recently recognized class of hard X-ray emitting symbiotic stars; and 2) if they are, compare the nature of any absorption, the optical depth of the boundary layer, and the accretion rate to those of the well established hard X-ray symbiotics. Understanding the accretion processes in symbiotic stars is a crucial step in determining the role they play as progenitors of type Ia supernovae.	GALACTIC POINT SOURCES	4	C	THOMAS NELSON		USA	5	AO5	EXPLORING THE ACCRETION DISK BOUNDARY LAYERS OF SYMBIOTIC STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405034010/	Quick Look
37	4U 1626-67	248.0734	-67.4643	246.814526	-67.35746	258.330198	-44.907314	321.7866399	-13.09493758	285.8172	55445.5409259259	2010-09-06 12:58:56	55446.2376273148	2010-09-07 05:42:11	405044010	20.0335	20	20.0335	20.0575	0	20.0457	2	2	0	2	1	0	0	19.5372	19.5372	60.1799	0	PROCESSED	57553.3082175926	2016-06-14 07:23:50	55822	2011-09-18 00:00:00	55456.2336574074	2010-09-17 05:36:28	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051234	Recent X-ray observations by Fermi/GBM and Swift/BAT of 4U 1626-67 discovered a new torque reversal of this source after 18 years of steady spinning down. Centered on Feb 4 2008, a dramatic increase in the X-ray flux was also observed. The lack of correlation between the X-ray flux and the torque applied to the neutron star before the transition, challenges our understanding of the physical mechanisms operating in this system. The main goal of this proposal is to look for changes in the long term flux behavior, energy spectra, pulse profile, line features and power spectra with the current evolution in 4U1626-67 s spin-up rate. In addition, we wish to determine whether the absence of the QPO observed just after the torque reversal persist.	GALACTIC POINT SOURCES	4	A	MARK FINGER		USA	5	AO5	THE ACCRETING X-RAY PULSAR 4U 1626-67 AFTER A NEW TORQUE REVERSAL	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405044010/	Quick Look
38	4U 1957+11	299.8589	11.6979	299.267976	11.560536	304.903477	31.592045	51.30303986	-9.34292333	251.3459	55501.8275462963	2010-11-01 19:51:40	55502.7001157407	2010-11-02 16:48:10	405057030	35.3491	35	35.3571	35.3491	0	35.3571	2	2	0	2	1	0	0	27.1697	27.1697	75.362	0	PROCESSED	57553.9520601852	2016-06-14 22:50:58	55881	2011-11-16 00:00:00	55515.3015046296	2010-11-15 07:14:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051254	We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind.	GALACTIC POINT SOURCES	4	B	MICHAEL NOWAK		USA	5	AO5	4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405057030/	Quick Look
39	TYCHO SNR HXD BKGD	9.2173	64.3076	8.488109	64.032592	44.61366	53.051862	121.35322514	1.48051733	84.2005	53915.6541782407	2006-06-29 15:42:01	53916.7606944444	2006-06-30 18:15:24	500025010	51.0088	50	51.0088	51.0088	51.0088	51.0088	2	2	2	2	1	0	0	48.7224	48.7224	95.5939	2	PROCESSED	57534.8010300926	2016-05-26 19:13:29	54302	2007-07-21 00:00:00	54052.5940509259	2006-11-13 14:15:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001099	We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		JAP	0	SWG	SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500025010/	Quick Look
40	HD162020	267.6631	-40.3218	266.786356	-40.308311	268.128314	-16.895672	350.73730077	-6.73005667	259.9987	55829.424212963	2011-09-25 10:10:52	55829.6543865741	2011-09-25 15:42:19	406038030	11.481	10	11.481	11.481	0	11.481	1	1	0	1	1	0	0	8.5402	8.5402	19.8799	0	PROCESSED	57603.2407638889	2016-08-03 05:46:42	56225	2012-10-25 00:00:00	55858.0790162037	2011-10-24 01:53:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061202	Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction.	GALACTIC POINT SOURCES	4	A	IGNAZIO PILLITTERI		USA	6	AO6	STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS.	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406038030/	Quick Look
41	4 DRA	187.5655	69.216	187.018636	69.492063	136.915856	61.202296	125.72551845	47.79722512	145.5318	55874.1707291667	2011-11-09 04:05:51	55875.0619328704	2011-11-10 01:29:11	406041010	42.258	40	42.258	42.258	0	42.258	2	2	0	2	1	0	0	39.7925	39.7925	76.998	2	PROCESSED	57603.7210532407	2016-08-03 17:18:19	56260	2012-11-29 00:00:00	55890.6961458333	2011-11-25 16:42:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061212	4 Dra is a weakly symbiotic star that exhibited strong variability in ROSAT observations. Our Suzaku Cycle 5 observation confirms it to be an absorbed hard X-ray source, powered by accretion. It is thus a nearby, lower accretion rate analogue of the hard X-ray bright symbiotic stars such as T CrB and CH Cyg. During Suzaku Cycle 6, 4 Dra is near apastron and near the inferior conjunction of the accreting white dwarf: both these should reduce the absorption due to the M giant, while absorption by the accretion flow near the white dwarf should remain roughly comparable. We therefore propose a second Suzaku observation of 4 Dra to constrain the relative contributions of these two X-ray absorbers, and to obtain a high signal-to-noise spectrum of a symbiotic star boundary layer near 1 keV.	GALACTIC POINT SOURCES	4	C	KOJI MUKAI		USA	6	AO6	A SUZAKU OBSERVATION OF 4 DRA NEAR INFERIOR CONJUNCTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406041010/	Quick Look
42	4U 1954+31	298.9334	32.0803	298.445315	31.946656	311.138232	51.470698	68.38077131	1.91321277	261.2562	55857.3373263889	2011-10-23 08:05:45	55858.7203009259	2011-10-24 17:17:14	406046010	60.216	60	60.224	60.232	0	60.216	3	2	0	2	1	0	0	57.9008	57.9008	119.4679	0	PROCESSED	57603.6159953704	2016-08-03 14:47:02	56241	2012-11-10 00:00:00	55874.1069328704	2011-11-09 02:33:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061226	We propose the first Suzaku observation of a symbiotic X-ray binary 4U 1954+31. This object has an extraordinarily long spin period, ~5 hour, attributed to the neutron star (NS) rotation, making 4U 1954+31 the slowest-rotating accreting NS binary. It raises a question about its binary evolution, since a slowly rotating NS orbiting an M-type giant is quite unique. As to its large variability, the popular clumpy wind model has not yet become a smoking-gun, and we propose an alternative hypothesis that the NS is a magnetar descendent captured by an M-type giant in their closer encounter. Known X-ray properties of 4U~1954+31 will be revisited in a view of gated accretion onto the strongly magnetized NS. A 60 ks Suzaku observation can examine these scenarios.	GALACTIC POINT SOURCES	4	B	TERUAKI ENOTO		USA	6	AO6	THE SLOWEST ROTATING PULSAR 4U 1954+31	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406046010/	Quick Look
43	BV CEN	202.8234	-54.9803	202.03184	-54.72288	225.050111	-41.512019	308.67903183	7.44609562	120.7167	56329.0246875	2013-02-06 00:35:33	56329.4856018518	2013-02-06 11:39:16	407047010	33.38	30	33.388	33.388	0	33.38	1	1	0	1	1	0	0	30.8692	30.8692	39.8159	0	PROCESSED	57610.5262268518	2016-08-10 12:37:46	56715	2014-02-27 00:00:00	56349.4846990741	2013-02-26 11:37:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071212	The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates?	GALACTIC POINT SOURCES	4	C	KOJI MUKAI		USA	7	AO7	DWARF NOVAE WITH EXTREME WHITE DWARF MASSES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407047010/	Quick Look
44	HERCULES X-1	254.4612	35.329	254.010606	35.404605	245.997214	57.479973	58.13300626	37.51795138	268.1998	56194.4317708333	2012-09-24 10:21:45	56195.0641087963	2012-09-25 01:32:19	407051030	23.5894	20	23.5931	23.5931	0	23.5894	2	2	0	2	1	0	0	23.4769	23.4769	54.634	0	PROCESSED	57607.1945601852	2016-08-07 04:40:10	56689	2014-02-01 00:00:00	56323.5148726852	2013-01-31 12:21:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071224	This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star.	GALACTIC POINT SOURCES	4	B	BRIAN GREFENSTETTE		USA	7	AO7	STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407051030/	Quick Look
45	4U1538-522	235.6015	-52.3857	234.665107	-52.226494	246.064673	-31.762519	327.42188954	2.16239803	275.2972	56149.0031134259	2012-08-10 00:04:29	56149.7349537037	2012-08-10 17:38:20	407068010	45.9554	40	45.9554	45.9554	0	45.9554	2	2	0	2	1	0	0	40.05	40.05	63.212	0	PROCESSED	57606.8269444444	2016-08-06 19:50:48	56640	2013-12-14 00:00:00	56272.688900463	2012-12-11 16:32:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071233	Observations of accreting pulsars in High Mass X-ray Binaries (HMXBs) provide us with important information about the physical processes in the stellar wind of the high mass donor star, the coupling between the accreting material and the neutron star's magnetic field, and the physics of the strongly magnetized accretion column above the neutron star. In this proposal we ask for a 40 ks observation of the accreting HMXB 4U1538-522 to conduct the most sensitive study to date of the wide range of characteristics of the broad band (0.1-100 keV) spectrum over a quarter of a binary orbit and with pulse phase. When one considers the ~50% duty cycle of Suzaku observations, the proposed observation will yield coverage of a quarter of the binary orbit.	GALACTIC POINT SOURCES	4	A	RICHARD ROTHSCHILD		USA	7	AO7	THE FIRST SUZAKU OBSERVATION OF 4U1538-522	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407068010/	Quick Look
46	SWIFT J2319.4+2619	349.8819	26.2473	349.265885	25.973522	2.029717	27.934963	98.48369948	-32.22425134	253.9963	56633.8796875	2013-12-07 21:06:45	56634.8786111111	2013-12-08 21:05:12	408030010	41.2758	40	41.2758	41.2758	0	41.2758	1	1	0	1	1	0	0	38.149	38.149	86.2879	2	PROCESSED	57613.5369328704	2016-08-13 12:53:11	57039	2015-01-17 00:00:00	56672.6300578704	2014-01-15 15:07:17	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081213	Polars are a subclass of magnetic cataclysmic variables in which a strongly magnetic white dwarf accretes matter from a late-type, Roche-lobe filling mass donor. They are usually soft X-ray bright and hard X-ray dim, due to either buried shocks or strong cyclotron cooling, depending on system parameters. However, a small subset of polars have been detected as bright hard X-ray sources in INTEGRAL and Swift BAT surveys. As a part of an effort to understand the hard-to-soft X-ray luminosity ratios of polars in general, and specifically to understand what combination of parameters make some polars hard X-ray bright, we propose Suzaku observations of two poorly studied BAT polars, Swift J2319.4+2619 and IW Eri, supported by ground-based observations including optical polarimetry.	GALACTIC POINT SOURCES	4	C	KOJI MUKAI		USA	8	AO8	THE HARD X-RAY BRIGHT POLARS SWIFT J2319.4+2619 AND IW ERI	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408030010/	Quick Look
47	SERPENS X-1	279.9874	5.0445	279.370748	4.997683	281.283069	28.094693	36.12473115	4.84817413	93.4997	56729.1215277778	2014-03-13 02:55:00	56731.6459606482	2014-03-15 15:30:11	408033020	1.2154	120	6.5666	24.0772	0	1.2154	2	2	0	2	1	0	0	82.3578	82.3578	218.0879	4	PROCESSED	57614.078912037	2016-08-14 01:53:38	57198	2015-06-25 00:00:00	56747.822037037	2014-03-31 19:43:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081222	Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs.	GALACTIC POINT SOURCES	4	B	EDWARD CACKETT		USA	8	AO8	THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408033020/	Quick Look
48	SERPENS X-1	279.9877	5.0424	279.371038	4.995582	281.28322	28.092576	36.12298663	4.84695852	81.3009	56757.3507060185	2014-04-10 08:25:01	56757.8959259259	2014-04-10 21:30:08	408033030	0.388	25	1.8071	6.4595	0	0.388	3	3	0	3	1	0	0	23.0266	23.0266	47.0979	0	PROCESSED	57614.2331481482	2016-08-14 05:35:44	57198	2015-06-25 00:00:00	56821.7352430556	2014-06-13 17:38:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081222	Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs.	GALACTIC POINT SOURCES	4	B	EDWARD CACKETT		USA	8	AO8	THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408033030/	Quick Look
49	ETA CARINAE	161.2798	-59.6805	160.793117	-59.417138	202.155622	-58.91379	287.60165846	-0.62249687	316.5996	56857.6091435185	2014-07-19 14:37:10	56859.2363425926	2014-07-21 05:40:20	409026010	53.2665	45	53.2665	56.7325	0	56.7485	2	2	0	2	1	0	0	28.9866	28.9866	138.1737	0	PROCESSED	57615.4364814815	2016-08-15 10:28:32	57264	2015-08-30 00:00:00	56898.3302777778	2014-08-29 07:55:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091202	Eta Carinae is an extremely massive binary system whose strong winds produce a variety of high-energy X-ray and possibly gamma-ray emission. Earlier XMM-Newton, Suzaku and INTEGRAL observations found interesting features in the extremely hard X-ray band: i) a flat spectral component above 9 keV toward the flux maximum; ii) strong 15-20 keV emission during an occultation of the wind-wind colliding plasma; iii) stable power-law emission above 25 keV. These features are signs of the highest energy processes yet detected in any colliding wind binary. Broad band X-ray observations around periastron are essential to understanding those features. We therefore propose Suzaku observations at 5 key phases around the next periastron passage of eta Carinae in 2014.6.	GALACTIC POINT SOURCES	4	A	KENJI HAMAGUCHI		USA	9	AO9	PROBING THE HIGHEST ENERGY PHENOMENA OF ETA CARINAE AROUND PERIASTRON IN 2014	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409026010/	Quick Look
50	M82 N2	148.2738	70.273	147.216273	70.508377	118.122269	52.466944	140.95732372	40.02876632	282.8972	57162.9827546296	2015-05-20 23:35:10	57164.434224537	2015-05-22 10:25:17	810043010	59.8084	60	59.8084	61.9021	0	61.9021	2	2	0	2	0	0	0	0	0	34.13	0	PROCESSED	57618.7218287037	2016-08-18 17:19:26	57548	2016-06-09 00:00:00	57177.3762847222	2015-06-04 09:01:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101442	We propose to carry out Suzaku observations of the starburst galaxy M82. We will search for X-ray emission from winds and shock heated clouds out to its possible outer boundary of ~45 kpc. We will also constrain the density and temperature profiles of the gas/wind emission out to large radii. These data can place important constraints on theoretical models of starburst galaxies and their environments. We will test models such as the Chevalier & Clegg adiabatic wind model, shocked clouds in a wind, etc. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	10	AO10	SEARCH FOR THE OUTER BOUNDARY OF THE STARBURST GALAXY: M82	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/810043010/	Quick Look
51	A1831	209.8007	27.9693	209.233208	28.211522	195.74505	37.218341	40.05378223	74.96810077	288.1207	53937.1181828704	2006-07-21 02:50:11	53937.5106481482	2006-07-21 12:15:20	801077010	18.0796	18	18.0796	18.0796	18.0796	18.0796	2	2	2	2	1	0	0	17.0891	17.0891	33.8979	1	PROCESSED	57535.0011805556	2016-05-27 00:01:42	54401	2007-10-28 00:00:00	53943.553599537	2006-07-27 13:17:11	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801077010/	Quick Look
52	VII ZW 403	172.0164	79.0077	171.163549	79.283023	114.484764	62.884943	127.82558857	37.31615306	108.8488	56627.0107638889	2013-12-01 00:15:30	56628.7884027778	2013-12-02 18:55:18	708039010	88.6616	87	88.6616	88.6616	0	88.6616	2	2	0	2	1	0	0	87.3974	87.3974	153.5578	1	PROCESSED	57613.4969328704	2016-08-13 11:55:35	57008	2014-12-17 00:00:00	56639.6396990741	2013-12-13 15:21:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081443	The source of energetic photons that reionized the early universe remains uncertain. Recently, it has been proposed that X-ray binaries in early galaxies made a significant contribution to reionization. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectra with the Suzaku XIS. These observations are important to our understanding of reionization and the formation of early galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	C	PHILIP KAARET		USA	8	AO8	X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708039010/	Quick Look
53	3C 390.3	280.4556	79.7798	281.326844	79.727189	82.097994	76.490616	111.44649344	27.08887917	37.561	56436.3002777778	2013-05-24 07:12:24	56438.6036921296	2013-05-26 14:29:19	708034010	100.3668	100	100.3668	100.3668	0	100.3668	2	2	0	2	1	0	0	109.3267	109.3267	198.9817	3	PROCESSED	57611.4065740741	2016-08-11 09:45:28	56816	2014-06-08 00:00:00	56449.7081365741	2013-06-06 16:59:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081431	We propose simultaneous Suzaku (100 ks) and NuSTAR observations of the broad-line radio galaxy 3C 390.3, to measure Fe K-alpha emission and Compton reflection from the accretion disk. This is crucial for understanding the geometry of the accretion disk and its relation to the production of a powerful, relativistic radio jet. The combination of accurate Compton reflection parameters measured with NuSTAR and a simultaneous estimate of the accretion disk inner radius from Fe K-alpha with Suzaku will place strong constraints on accretion disk models for radio loud AGNs.	EXTRAGALACTIC COMPACT SOURCES	7	B	PATRICK OGLE		USA	8	AO8	ACCRETION AND BLACK HOLE SPIN IN THE POWERFUL, RADIO-LOUD AGN 3C 390.3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708034010/	Quick Look
54	NEP #4	270.0449	66.5788	270.046703	66.578557	56.874538	89.977746	96.40481628	29.79358389	165.3654	55193.4146875	2009-12-28 09:57:09	55194.4579166667	2009-12-29 10:59:24	504076010	49.8491	50	49.8571	49.8571	0	49.8491	2	2	0	2	1	0	0	43.5039	43.5039	90.114	0	PROCESSED	57550.0085648148	2016-06-11 00:12:20	54922	2009-04-01 00:00:00	55246.2930787037	2010-02-19 07:02:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041101	We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe.	GALACTIC DIFFUSE EMISSION	5	A	STEVEN SNOWDEN		USA	4	AO4	OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504076010/	Quick Look
55	MRK 421 OFFSET	165.3836	38.6302	164.685253	38.899103	150.412438	29.624722	179.31913311	64.35556561	121.9647	55146.4480092593	2009-11-11 10:45:08	55148.3176388889	2009-11-13 07:37:24	504087010	86.0144	75	86.0144	86.0144	0	86.0144	2	2	0	2	1	0	0	64.8804	64.8804	161.5199	3	PROCESSED	57549.3389583333	2016-06-10 08:08:06	55531	2010-12-01 00:00:00	55160.2701041667	2009-11-25 06:28:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041324	The OVII, OVIII, and NeIX absorption lines at z~0 have been discovered in the Chandra/XMM spectra of several bright AGNs, but the location of these absorptions has been debated since their discoveries. Here we request Suzaku observations of the soft X-ray background emission in the vicinity of Mrk 421, to conduct a joint analysis of the emission data with the extensive Chandra absorption data. This analysis will naturally yield an effective length of the absorbing/emitting gas. We have performed pilot studies and obtained a scale length of several kpc for the hot absorbing/emitting gas toward LMC X-3 and Mrk 421. The requested Suzaku observations are particular important to check these results and to further test the models we have developed in our study.	GALACTIC DIFFUSE EMISSION	5	B	YANGSEN YAO		USA	4	AO4	A JOINT X-RAY ABSORPTION AND EMISSION STUDY OF THE HOT GAS TOWARD MRK 421	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504087010/	Quick Look
56	A1800	207.3618	28.0973	206.789109	28.345144	193.256107	36.394356	40.59651819	77.12066844	302.3644	53936.635625	2006-07-20 15:15:18	53937.1140509259	2006-07-21 02:44:14	801078010	20.0437	17	20.0473	20.0553	20.0553	20.0437	2	2	2	2	1	0	0	19.0003	19.0003	41.3319	0	PROCESSED	57535.0036458333	2016-05-27 00:05:15	54401	2007-10-28 00:00:00	53943.5299652778	2006-07-27 12:43:09	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801078010/	Quick Look
57	GX 301-2	186.689	-62.7212	185.98909	-62.444416	221.478022	-52.575765	300.10817936	0.01514837	109.0098	54836.4396296296	2009-01-05 10:33:04	54838.0419328704	2009-01-07 01:00:23	403044020	61.8136	50	61.8136	61.8136	0	61.8136	2	2	0	2	1	0	0	54.9922	54.9922	138.3981	2	PROCESSED	57545.1371064815	2016-06-06 03:17:26	55328	2010-05-12 00:00:00	54851.4303125	2009-01-20 10:19:39	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031152	We propose the first observation of the bright neutron star GX 301-2 with Suzaku. The aim of the proposed 60 ks observation is a study of the broadband spectrum of the source in unprecedented detail and quality. This will allow us to analyze the structure (including density and clumpiness) of the intense wind of the optical companion and the gas stream flowing from Wray 977 to the neutron star. Spectral data will be used to study the evolution of nH and the iron line with very high time resolution. Furthermore, we will perform phase resolved spectroscopy to study the spectral variation of the cyclotron line with pulse phase.	GALACTIC POINT SOURCES	4	A	RICHARD ROTHSCHILD		USA	3	AO3	BROAD-BAND STUDY OF GX 301-2	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403044020/	Quick Look
58	GX 339-4	255.7095	-48.7885	254.761689	-48.717523	259.577896	-25.861992	338.94163546	-4.32765826	281.8009	54733.942650463	2008-09-24 22:37:25	54736.0968055556	2008-09-27 02:19:24	403067010	104.994	100	105.018	104.994	0	104.994	2	2	0	2	1	0	0	114.7759	114.7759	186.0917	2	PROCESSED	57544.0505092593	2016-06-05 01:12:44	55148	2009-11-13 00:00:00	54780.5803935185	2008-11-10 13:55:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031174	Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with our multi-wavelength, radio to X-ray, program, Suzaku observations can constrain theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions.	GALACTIC POINT SOURCES	4	A	JOHN TOMSICK		USA	3	AO3-TOO	CONSTRAINING MODELS FOR BLACK HOLE ACCRETION IN THE HARD STATE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403067010/	Quick Look
59	COMET_8P_TUTTLE-P1-5	28.1493	7.0036	27.492979	6.757378	28.646774	-4.267305	148.58110255	-52.79544349	248.5006	54470.7825810185	2008-01-05 18:46:55	54470.8487384259	2008-01-05 20:22:11	502062050	1.6746	2	1.6746	1.6746	0	1.6746	1	1	0	1	1	0	0	1.703	1.703	5.6861	0	PROCESSED	57540.9980208333	2016-06-01 23:57:09	54908	2009-03-18 00:00:00	54542.2043055556	2008-03-17 04:54:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062050/	Quick Look
60	COMET_8P_TUTTLE-P2_13	40.3641	-37.3366	39.860845	-37.549577	20.8839	-49.581867	243.65335896	-64.71445889	253.6857	54491.6297106482	2008-01-26 15:06:47	54491.762662037	2008-01-26 18:18:14	502063130	6.5907	6.7	6.6147	6.5987	0	6.5907	1	1	0	1	1	0	0	5.0221	5.0221	11.4799	0	PROCESSED	57541.4103356482	2016-06-02 09:50:53	54912	2009-03-22 00:00:00	54546.2204861111	2008-03-21 05:17:30	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063130/	Quick Look
61	BULGE 2	270.6176	-29.5847	269.818763	-29.585758	270.530563	-6.144879	1.30042786	-3.49803376	83.2679	53801.7493981482	2006-03-07 17:59:08	53802.0689699074	2006-03-08 01:39:19	500002010	13.028	10	13.052	13.044	13.036	13.028	1	1	1	1	1	0	0	10.6741	10.6741	27.5999	1	PROCESSED	57533.1394444444	2016-05-25 03:20:48	54247	2007-05-27 00:00:00	54041.664525463	2006-11-02 15:56:55	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001014	Leading .	GALACTIC DIFFUSE EMISSION	5	A	DAN MCCAMMON		JAP	0	SWG	THE SOFT GALACTIC BULGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500002010/	Quick Look
62	URSA MINOR	227.2517	67.2307	227.099638	67.419875	158.023499	73.538029	104.9865755	44.80382561	40.7921	54195.7731944444	2007-04-05 18:33:24	54196.7557175926	2007-04-06 18:08:14	802052010	70.8823	67	70.8903	70.8823	0	70.8903	2	2	0	2	1	0	0	59.5872	59.5872	84.876	1	PROCESSED	57538.0737731482	2016-05-30 01:46:14	54695	2008-08-17 00:00:00	54203.3200462963	2007-04-13 07:40:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021405	We propose 50 ksec Suzaku observations of the Ursa Minor and Draco dwarf spheroidal galaxies. These dense, dark-matter-dominated systems are carefully selected as the strongest potential sources of line emission from radiatively decaying keV dark matter of any astrophysical object. The low-level, stable Suzaku background makes it the most sensitive instrument to-date for this purpose. At the very least, constraints that enter a significant new regime are derived: non-detections are still of great importance. In the best case, the long sought-after identity of dark matter will be discovered, pointing the way to physics beyond the Standard Model.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MICHAEL LOEWENSTEIN		USA	2	AO2	SEARCH FOR WARM DARK MATTER WITH SUZAKU OBSERVATIONS OF DWARF SPHEROIDAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802052010/	Quick Look
63	BOOTES GROUP 1	218.7136	35.7235	218.197903	35.941461	200.235171	47.529275	60.71261374	66.41229506	153.2269	54440.1222106482	2007-12-06 02:55:59	54441.2015972222	2007-12-07 04:50:18	802054010	42.2242	38	42.2242	42.2242	0	42.2242	2	2	0	2	1	0	0	41.3023	41.3023	93.254	0	PROCESSED	57540.8293518518	2016-06-01 19:54:16	54815	2008-12-15 00:00:00	54448.2273842593	2007-12-14 05:27:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021424	We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MARSHALL BAUTZ		USA	2	AO2	SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802054010/	Quick Look
64	A2665	357.7161	6.1352	357.076736	5.857083	0.350497	6.536022	96.94047732	-53.65177278	245.9817	54078.2252893518	2006-12-09 05:24:25	54078.562037037	2006-12-09 13:29:20	801076010	13.944	15	13.944	13.944	0	13.944	2	2	0	2	1	0	0	11.6073	11.6073	29.0879	0	PROCESSED	57536.2715393518	2016-05-28 06:31:01	54695	2008-08-17 00:00:00	54089.271412037	2006-12-20 06:30:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801076010/	Quick Look
65	PKS 1345+12	206.9131	12.3498	206.299989	12.598696	200.201065	21.844458	347.38894416	70.20282736	113.9421	54472.3082407407	2008-01-07 07:23:52	54473.6799768518	2008-01-08 16:19:10	702053010	52.9844	50	52.9844	52.9844	0	52.9844	2	2	0	2	1	0	0	45.2034	45.2034	118.5038	4	PROCESSED	57541.3141782407	2016-06-02 07:32:25	54854	2009-01-23 00:00:00	54483.4984375	2008-01-18 11:57:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021341	We wish to take advantage of the sensitivity of Suzaku above 10 keV to constrain the energy source -- starburst or black-hole driven activity -- in three of the brightest warm transitional ultraluminous infrared galaxies, PKS 1345+12, Mrk 463, and 3C 273. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short time scale variability, another signature of black-hole driven activity. These data will be combined with our A01 spectra and be part of S. Teng's PhD thesis at UMD.	EXTRAGALACTIC COMPACT SOURCES	7	C	SYLVAIN VEILLEUX		USA	2	AO2	SPECTRA OF THE BRIGHTEST WARM ULTRALUMINOUS INFRARED GALAXIES	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702053010/	Quick Look
66	HD162020	267.6599	-40.3316	266.783075	-40.318096	268.125938	-16.905511	350.72753331	-6.73286722	269.5018	55820.4672453704	2011-09-16 11:12:50	55820.6918634259	2011-09-16 16:36:17	406038020	8.896	10	8.896	8.896	0	8.896	1	1	0	1	1	0	0	7.8519	7.8519	19.3999	0	PROCESSED	57603.1676851852	2016-08-03 04:01:28	56218	2012-10-18 00:00:00	55851.4444097222	2011-10-17 10:39:57	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061202	Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction.	GALACTIC POINT SOURCES	4	A	IGNAZIO PILLITTERI		USA	6	AO6	STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS.	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406038020/	Quick Look
67	ABELL 3571	206.8624	-32.8524	206.14186	-32.603207	216.960537	-20.284209	316.31343933	28.55973438	103.8412	56666.0275	2014-01-09 00:39:36	56666.7772453704	2014-01-09 18:39:14	808094010	38.279	60	38.279	38.279	0	38.279	2	2	0	2	1	0	0	39.0047	39.0047	64.776	0	PROCESSED	57613.7763425926	2016-08-13 18:37:56	57096	2015-03-15 00:00:00	56730.4916435185	2014-03-14 11:47:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081531	Abell 3571 is one of the brightest cluster in the X-ray sky and one of the main clusters in the Shapley supercluster. We have recently found evidence that it may be passing through a violent (~2000 km/s) merger in the line of sight (los). If corroborated it would be the closest template for the systems of this kind allowing us to study and characterize los mergers. We request a short observation of 60 ksec to corroborate the velocity gradients found with Chandra for this cluster, using the improved spectral resolution and gain stability of Suzaku s XISs.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	RENATO DUPKE		USA	8	AO8	ABELL 3571. THE CLOSEST LINE OF SIGHT MERGER?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808094010/	Quick Look
68	COMET_8P_TUTTLE-P2_16	40.5411	-37.7213	40.040278	-37.933718	20.796624	-49.987507	244.42429467	-64.47300408	253.9693	54492.0297106482	2008-01-27 00:42:47	54492.162662037	2008-01-27 03:54:14	502063160	3.7705	4	3.7705	3.7705	0	3.7705	1	1	0	1	1	0	0	3.9881	3.9881	11.4799	0	PROCESSED	57541.4170833333	2016-06-02 10:00:36	54912	2009-03-22 00:00:00	54546.2311574074	2008-03-21 05:32:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063160/	Quick Look
69	A3376 WEST RELIC	90.0363	-39.9917	89.629297	-39.992531	90.071049	-63.433501	246.43145562	-26.38385089	126.3601	54034.3950231482	2006-10-26 09:28:50	54035.9176388889	2006-10-27 22:01:24	800011020	62.2648	60	62.2648	62.2648	62.2648	62.2648	2	2	2	2	1	0	0	55.5629	55.5629	131.5378	2	PROCESSED	57535.9705902778	2016-05-27 23:17:39	54694	2008-08-16 00:00:00	54090.2671643518	2006-12-21 06:24:43	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001039	We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA		JAP	0	SWG	SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800011020/	Quick Look
70	AO 0235+164	39.665	16.613	38.972105	16.397631	42.455706	1.088366	156.77598662	-39.11106084	252.4352	56310.722337963	2013-01-18 17:20:10	56311.7418634259	2013-01-19 17:48:17	707021010	43.1028	40	43.1108	43.1188	0	43.1028	2	2	0	2	1	0	0	38.3583	38.3583	88.0698	0	PROCESSED	57608.5604166667	2016-08-08 13:27:00	56709	2014-02-21 00:00:00	56342.5387731482	2013-02-19 12:55:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071402	We request observations of the variable blazar AO 0235+164, to be conducted simultaneously with Fermi and optical and radio telescopes, towards a multi-band campaign. This object has complex X-ray spectrum due to absorption by an intervening galaxy, and Suzaku will be essential in unraveling the effects and composition of that absorber, and for the first time, provide a robust measurement of the underlying blazar X-ray continuum, which, together with the Swift UVOT spectrum, will allow to verify the signature of the bulk-Compton component, due to cold electrons propagating in the relativistic jet. At the highest priority, we request 40 ks for a precise spectral measurement; at a lower priority, we wish to monitor the source for the total of 5 days, with the request of additional 160 ks.	EXTRAGALACTIC COMPACT SOURCES	7	B	GRZEGORZ MADEJSKI		USA	7	AO7	SUZAKU OBSERVATIONS OF THE GAMMA-RAY BLAZAR AO 0235+164	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707021010/	Quick Look
71	COMET_8P_TUTTLE-P1-8	28.3076	6.2429	27.652953	5.997039	28.526064	-5.034788	149.32011202	-53.43313536	248.4984	54470.9825	2008-01-05 23:34:48	54471.0487384259	2008-01-06 01:10:11	502062080	3.219	3.2	3.219	3.219	0	3.219	1	1	0	1	1	0	0	3.374	3.374	5.664	0	PROCESSED	57541.0065046296	2016-06-02 00:09:22	54908	2009-03-18 00:00:00	54542.2264583333	2008-03-17 05:26:06	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062080/	Quick Look
72	MARKARIAN 79	115.6357	49.8015	114.696355	49.919868	108.437878	27.988088	168.6115046	28.38007803	283.4884	54193.9134953704	2007-04-03 21:55:26	54195.7655439815	2007-04-05 18:22:23	702044010	83.7038	82	83.7118	83.7038	0	83.7118	2	2	0	2	1	0	0	82.1042	82.1042	160.0059	0	PROCESSED	57538.0894444444	2016-05-30 02:08:48	54695	2008-08-17 00:00:00	54203.4223842593	2007-04-13 10:08:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021313	Recently, deep observations of a number of Seyfert AGN with XMM-Newton and Suzaku have established variable and relativistic iron lines as robust features in roughly half of all deep Seyfert spectra. In these sources, the spin of the black hole can be constrained directly through fits to the relativistic iron line. A sample of excellent spectra from well-chosen AGN will facilitate a better understanding of the innermost regime near to black holes, and make correlations with parameters like radio luminosity, star formation rate, and galaxy and black hole mass possible for the first time. We propose to obtain observations of 4 under-exposed Seyfert AGN with promising evidence for broad lines to robustly constrain their spin parameters.	EXTRAGALACTIC COMPACT SOURCES	7	B	JON MILLER		USA	2	AO2	REVEALING BLACK HOLE SPIN IN RELATIVISTIC SEYFERT AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702044010/	Quick Look
73	ERIDANUS HOLE	67.1401	-17.0746	66.578414	-17.184035	61.759444	-38.302767	213.43674881	-39.09232011	64.2755	54311.0359606482	2007-07-30 00:51:47	54313.2161921296	2007-08-01 05:11:19	502076010	103.7523	100	103.7523	103.7523	0	103.7523	2	2	0	2	1	0	0	92.2091	92.2091	188.3518	2	PROCESSED	57539.4003356482	2016-05-31 09:36:29	54710	2008-09-01 00:00:00	54340.7341898148	2007-08-28 17:37:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021224	We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source.	GALACTIC DIFFUSE EMISSION	5	B	MASSIMILIANO GALEAZZI		USA	2	AO2	STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502076010/	Quick Look
74	RCS212414-6325.8	321.0509	-63.4275	320.054735	-63.642547	299.532953	-45.130077	330.62476764	-40.84164156	79.2319	55691.4113541667	2011-05-10 09:52:21	55691.979375	2011-05-10 23:30:18	806082010	36.3224	35	36.3304	36.3304	0	36.3224	2	2	0	2	1	0	0	26.914	26.914	49.0679	1	PROCESSED	57602.0065046296	2016-08-02 00:09:22	56068	2012-05-21 00:00:00	55701.1927546296	2011-05-20 04:37:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061533	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AMALIA HICKS		USA	6	AO6	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806082010/	Quick Look
75	GRB060105	297.6095	46.3384	297.227077	46.210211	319.460988	65.110067	80.2506255	9.98748628	191.1906	53740.5089351852	2006-01-05 12:12:52	53741.5002083333	2006-01-06 12:00:18	900001010	42.2208	40	42.2208	42.2208	42.2208	42.2208	2	2	2	2	1	0	0	37.718	37.718	85.6419	2	PROCESSED	57532.6415856482	2016-05-24 15:23:53	54247	2007-05-27 00:00:00	54039.776712963	2006-10-31 18:38:28	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001008	(i) Early break in lightcurve of X-ray afterglows using HXD. Recent Swift/XRT observations reveal that early X-ray afterglows of GRB has flat portion with very shallow decay. It may suggest continuous energy input from the central engine. The transition from its phase to general afterglow may display hard-to-soft evolution reflecting the cooling frequency. Thus multi wavelength observation will provide a key to the physics of central engine activity. (ii) Emission lines in the afterglows. The confirmation of line existence should be a matter of great importance because there remains unanswered questions. Some data may indicate a prominent iron line but others seem to suggest significant lower energy lines instead without iron lines.	EXTRAGALACTIC COMPACT SOURCES	9	A	TOSHIO MURAKAMI		JAP	0	SWG-TOO	TOO OBSERVATIONS OF GAMMA-RAY BURSTS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/900001010/	Quick Look
76	AB DOR	82.2835	-65.427	82.246883	-65.464502	16.282788	-86.671062	275.26967334	-33.00819219	154.6774	54060.0265277778	2006-11-21 00:38:12	54061.4586111111	2006-11-22 11:00:24	401031010	53.4517	80	53.4517	53.4597	0	53.4614	2	2	0	2	1	0	0	48.0334	48.0334	123.708	1	PROCESSED	57536.170462963	2016-05-28 04:05:28	54502	2008-02-06 00:00:00	54133.0222916667	2007-02-02 00:32:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011021	We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku.	GALACTIC POINT SOURCES	4	B	MARC AUDARD		USA	1	AO1	NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401031010/	Quick Look
77	ABELL 1795 Far North	207.223	26.9995	206.646903	27.247656	193.71055	35.352954	35.63943573	77.21561208	130.4264	53715.3208796296	2005-12-11 07:42:04	53715.9730092593	2005-12-11 23:21:08	800012030	30.6406	30	30.6486	30.6406	30.6639	30.6566	2	2	2	2	1	0	0	27.8833	27.8833	56.3379	1	PROCESSED	57532.4195833333	2016-05-24 10:04:12	54247	2007-05-27 00:00:00	54039.1003703704	2006-10-31 02:24:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012030/	Quick Look
78	RT CRU	188.7055	-64.6161	187.980233	-64.340558	224.663135	-53.421751	301.15157727	-1.80180428	281.609	54283.5270023148	2007-07-02 12:38:53	54284.2433333333	2007-07-03 05:50:24	402040010	50.8806	50	50.8806	50.8806	0	50.8806	2	2	0	2	1	0	0	42.8506	42.8506	61.8879	0	PROCESSED	57539.0744328704	2016-05-31 01:47:11	54695	2008-08-17 00:00:00	54328.4668055556	2007-08-16 11:12:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021102	Symbiotic stars are interacting binaries in which a white dwarf (WD) accretes from the wind of a red giant. Their X-ray emission is typically very soft. Recently, however, 4 symbiotics have been detected out to almost 100 keV. Suzaku observations of two of these sources revealed that the hard X-rays emanated from an extremely hot thermal plasma. One means of producing such hot gas is accretion onto a near Chandrasekhar-mass WD. We propose to use the unique capabilities of Suzaku to test this hypothesis. We will use broad-band X-ray spectral fitting to determine the temperature of the hot plasma, hard X-ray timing studies to search for or constrain rapid variations due to either magnetic or non-magnetic accretion, and Fe line diagnostics to investigate the role of scattering.	GALACTIC POINT SOURCES	4	B	JENNIFER SOKOLOSKI		USA	2	AO2	ARE HARD X-RAY SYMBIOTICS PROGENITORS OF TYPE IA SUPERNOVAE?	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402040010/	Quick Look
79	ASAS J002511+1217.2	6.2997	12.2847	5.652783	12.007819	10.667541	8.77612	112.91544003	-50.07604687	234.9156	54841.6813773148	2009-01-10 16:21:11	54842.5468055556	2009-01-11 13:07:24	403039010	33.256	30	33.256	33.256	0	33.256	2	2	0	2	1	0	0	29.873	29.873	74.752	1	PROCESSED	57545.1348726852	2016-06-06 03:14:13	55328	2010-05-12 00:00:00	54851.4143055556	2009-01-20 09:56:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031144	Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates.	GALACTIC POINT SOURCES	4	C	KOJI MUKAI		USA	3	AO3	BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403039010/	Quick Look
80	IRAS 00182-7112	5.1458	-70.9276	4.573856	-71.205097	312.979414	-61.496651	306.55074146	-45.98323945	33.8687	56050.171087963	2012-05-03 04:06:22	56052.8759143518	2012-05-05 21:01:19	707036010	93.959	90	93.967	93.959	0	93.959	2	2	0	2	1	0	0	86.5766	86.5766	233.6819	1	PROCESSED	57605.3998263889	2016-08-05 09:35:45	56435	2013-05-23 00:00:00	56068.6299537037	2012-05-21 15:07:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071441	We propose to observe with the Hard X-ray Detector onboard Suzaku the two Ultraluminous Infrared Galaxies IRAS 00182-7112 and IRAS 12127-1412, both of which are known to harbour very luminous and highly obscured active galactic nuclei (AGN). An AGN reflection component arising from ionized gas is clearly identified at 2 10 keV: the detection of the direct AGN emission above 10 keV and the measure of the reflection efficiency would provide fundamental information on both the physical structure of Compton-thick AGN embedded in a nuclear starburst and their feedback on the surrounding environment.	EXTRAGALACTIC COMPACT SOURCES	7	B	EMANUELE NARDINI		USA	7	AO7	THE PHYSICAL STRUCTURE OF COMPTON-THICK AGN/ULIRGS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707036010/	Quick Look
81	HD162020	267.6618	-40.3275	266.785008	-40.314005	268.127379	-16.901388	350.73183598	-6.73206134	259.9987	55824.6498958333	2011-09-20 15:35:51	55825.1632407407	2011-09-21 03:55:04	406037030	16.23	15	16.238	16.238	0	16.23	2	2	0	2	1	0	0	13.3784	13.3784	44.3459	1	PROCESSED	57603.1988078704	2016-08-03 04:46:17	56218	2012-10-18 00:00:00	55851.4474884259	2011-10-17 10:44:23	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061202	Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction.	GALACTIC POINT SOURCES	4	A	IGNAZIO PILLITTERI		USA	6	AO6	STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS.	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406037030/	Quick Look
82	J081618.99+482328.4	124.0768	48.3841	123.174595	48.53824	114.890427	27.844597	171.01809871	33.69777889	298.4793	54917.0925462963	2009-03-27 02:13:16	54919.0946643518	2009-03-29 02:16:19	703042010	90.9224	90	90.9224	90.9224	0	90.9224	2	2	0	2	1	0	0	81.0739	81.0739	172.9637	2	PROCESSED	57545.9726736111	2016-06-06 23:20:39	55329	2010-05-13 00:00:00	54930.3718055556	2009-04-09 08:55:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031337	We have discovered polar broad absorption-line quasars (BALQSOs) from their radio variabilities. We know their inclination angles. Our results derived from the archival Chandra data of one polar BALQSO indicate that the X-ray emissions are from the jet and the X-ray absorbing gas is located at tens of parsecs above the accretion disk corona. We want to confirm these results at high confidence level using better signal to noise ratio data from a big observatory, like SUZAKU. In addition, we propose to observe three more polar BALQSOs, which have wide range of radio/UV/X-ray properties. Our primary science goal of this proposal is to determine the radial distribution of the X-ray absorbing gas in 4 polar BALQSOs.	EXTRAGALACTIC COMPACT SOURCES	7	C	KAJAL GHOSH		USA	3	AO3	PROBING THE INNER STRUCTURE OF AGNS USING THE POLAR BALQSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703042010/	Quick Look
83	XTE J1946+274	296.4201	27.2906	295.90791	27.167842	305.811743	47.50074	63.14511565	1.35338176	267.925	55480.9086805556	2010-10-11 21:48:30	55482.2446064815	2010-10-13 05:52:14	405041010	50.7317	45	50.7317	50.7317	0	50.7317	2	2	0	2	1	0	0	46.5571	46.5571	115.3739	1	PROCESSED	57553.7260185185	2016-06-14 17:25:28	55867	2011-11-02 00:00:00	55491.1017476852	2010-10-22 02:26:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051231	We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum.	GALACTIC POINT SOURCES	4	A	KATJA POTTSCHMIDT		USA	5	AO5-TOO	CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405041010/	Quick Look
84	A2495	342.5777	10.9124	341.95313	10.647232	348.269753	16.897696	81.20126485	-41.9387619	237.1467	54061.4694097222	2006-11-22 11:15:57	54062.0787037037	2006-11-23 01:53:20	801080010	18.0313	18	18.0313	18.3673	0	18.1193	2	2	0	2	1	0	0	16.3891	16.3891	52.6339	3	PROCESSED	57536.1381365741	2016-05-28 03:18:55	54695	2008-08-17 00:00:00	54088.9563194444	2006-12-19 22:57:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080010/	Quick Look
85	BULGE 3	274.7046	-31.4846	273.893726	-31.505472	274.041648	-8.109784	1.3002625	-7.49777303	80.4025	53800.3437962963	2006-03-06 08:15:04	53801.7474421296	2006-03-07 17:56:19	500001010	51.8468	50	51.8548	51.8548	51.8548	51.8468	2	2	2	2	1	0	0	45.0783	45.0783	121.2459	0	PROCESSED	57533.1540972222	2016-05-25 03:41:54	54247	2007-05-27 00:00:00	54041.7128703704	2006-11-02 17:06:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001014	Leading .	GALACTIC DIFFUSE EMISSION	5	A	DAN MCCAMMON		JAP	0	SWG	THE SOFT GALACTIC BULGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500001010/	Quick Look
86	SN1006 NW	225.6364	-41.8003	224.819551	-41.604176	235.339658	-23.546444	327.59294648	14.70833496	115.0008	53766.4881365741	2006-01-31 11:42:55	53767.55375	2006-02-01 13:17:24	500017010	53.0194	50	53.0194	53.0277	53.0273	53.0273	2	2	2	2	1	0	0	60.4123	60.4123	92.0679	0	PROCESSED	57532.8347685185	2016-05-24 20:02:04	54247	2007-05-27 00:00:00	54040.7669675926	2006-11-01 18:24:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001062	We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		JAP	0	SWG	THE EJECTA IN SN1006	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500017010/	Quick Look
87	FG25	234.9579	30.7058	234.452539	30.866616	221.876556	48.458584	48.772653	53.18955534	294.6599	56136.7541898148	2012-07-28 18:06:02	56137.0821875	2012-07-29 01:58:21	807049010	10.6393	10	10.6393	10.6393	0	10.6393	2	2	0	2	1	0	0	11.074	11.074	28.3281	0	PROCESSED	57606.6807523148	2016-08-06 16:20:17	56527	2013-08-23 00:00:00	56161.2376736111	2012-08-22 05:42:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071511	Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ELENA D'ONGHIA		USA	7	AO7	SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807049010/	Quick Look
88	A 2218 OFFSETB	249.9091	65.2119	249.835523	65.307656	180.044789	81.713752	96.37864193	38.09205953	233.3309	53670.1916319444	2005-10-27 04:35:57	53670.4620833333	2005-10-27 11:05:24	800020010	14.9215	15	14.9375	14.9335	14.9215	14.9415	2	2	2	2	1	0	0	14.1931	14.1931	23.3561	0	PROCESSED	57527.6596180556	2016-05-19 15:49:51	54247	2007-05-27 00:00:00	54036.8343981482	2006-10-28 20:01:32	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001096	To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI		JAP	0	SWG	SEARCH FOR OXYGEN LINES FROM WARM IGM		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800020010/	Quick Look
89	SMC X-1	19.2828	-73.4495	18.951598	-73.712645	312.330174	-66.477022	300.41169288	-43.55280074	39.2778	55706.0851851852	2011-05-25 02:02:40	55706.6745833333	2011-05-25 16:11:24	706030050	17.8463	18	17.8463	18.1823	0	18.1001	2	2	0	1	1	0	0	16.6829	16.6829	50.9139	0	PROCESSED	57602.111099537	2016-08-02 02:39:59	56092	2012-06-14 00:00:00	55725.1651736111	2011-06-13 03:57:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030050/	Quick Look
90	COMA NW5	194.3037	29.1454	193.700799	29.41548	180.283789	32.183117	91.00313756	87.61452721	319.9965	55733.4693865741	2011-06-21 11:15:55	55734.0682407407	2011-06-22 01:38:16	806042010	21.0972	20	21.1201	21.1132	0	21.0972	2	2	0	2	1	0	0	20.4401	20.4401	51.724	0	PROCESSED	57602.3799537037	2016-08-02 09:07:08	55652	2011-04-01 00:00:00	55768.342025463	2011-07-26 08:12:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806042010/	Quick Look
91	COMA SW5.5	193.6448	27.0863	193.037174	27.357142	180.762937	30.083449	29.67661506	89.29968791	314.5983	55735.866400463	2011-06-23 20:47:37	55736.3037037037	2011-06-24 07:17:20	806048010	15.2345	15	15.245	15.2345	0	15.2345	2	2	0	2	1	0	0	16.4375	16.4375	37.776	0	PROCESSED	57602.4025347222	2016-08-02 09:39:39	55652	2011-04-01 00:00:00	55794.9965625	2011-08-21 23:55:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806048010/	Quick Look
92	RXCJ0605	91.7111	-35.2772	91.267409	-35.26998	92.696732	-58.702768	241.82465393	-23.81756849	309.9841	55323.0313194444	2010-05-07 00:45:06	55323.8550810185	2010-05-07 20:31:19	805065030	42.4239	40	42.4319	42.4319	0	42.4239	2	2	0	2	1	0	0	39.146	39.146	71.1619	0	PROCESSED	57551.4298263889	2016-06-12 10:18:57	55287	2010-04-01 00:00:00	55341.5040393518	2010-05-25 12:05:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805065030/	Quick Look
93	MRK 766	184.6154	29.8184	183.986779	30.095968	171.206094	28.943476	190.63186084	82.27243688	133.2599	54055.0242361111	2006-11-16 00:34:54	54057.363900463	2006-11-18 08:44:01	701035010	97.8693	150	98.1756	97.8693	0	98.1676	2	2	0	2	1	0	0	96.8931	96.8931	202.1299	2	PROCESSED	57536.189525463	2016-05-28 04:32:55	54800	2008-11-30 00:00:00	54132.8396990741	2007-02-01 20:09:10	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011328	X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components	EXTRAGALACTIC COMPACT SOURCES	7	B	TRACEY TURNER		USA	1	AO1	DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701035010/	Quick Look
94	MRK 1	19.06	33.0289	18.361574	32.765252	30.564721	23.029207	128.90716196	-29.55492804	249.7486	54111.5318171296	2007-01-11 12:45:49	54114.5836111111	2007-01-14 14:00:24	701047010	126.4441	120	126.4441	126.4441	0	126.4441	2	2	0	2	1	0	0	126.0122	126.0122	263.6237	2	PROCESSED	57637.5831944445	2016-09-06 13:59:48	54702	2008-08-24 00:00:00	54133.1552314815	2007-02-02 03:43:32	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011336	The supermassive black holes of active galactic nuclei (AGN) are fundamentally connected to the stars of their host galaxies, but it is not clear whether this relationship is evident at X-ray energies. We will test the prediction that prolific star formation is responsible for the soft X-ray emission from a Compton thick AGN that also contains a powerful circumnuclear starburst. The AGN's deep obscuration facilitates the soft X-ray measurements, and Compton thick AGN are generally significant, both as a large fraction of the local AGN population and for their contribution to the X-ray background. Furthermore, we will use the direct measurement of the intrinsic AGN luminosity to test unified AGN models and the validity of indirect luminosity indicators.	EXTRAGALACTIC COMPACT SOURCES	7	B	NANCY LEVENSON		USA	1	AO1	TESTING THE STARBURST-AGN CONNECTION AND MEASURING DEEPLY OBSCURED AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701047010/	Quick Look
95	CAS A	350.8729	58.8094	350.30695	58.534812	27.388607	54.842749	111.74406014	-2.13880346	214.7372	53768.5363657407	2006-02-02 12:52:22	53768.833599537	2006-02-02 20:00:23	100043010	0	10	0	0	0	0	0	0	0	0	1	0	0	10.3268	10.3268	25.6739	1	PROCESSED	57532.8451736111	2016-05-24 20:17:03	54247	2007-05-27 00:00:00	54040.7488888889	2006-11-01 17:58:24	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001097	We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	0	SWG	XIS FLIGHT CAIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100043010/	Quick Look
96	NGC 1365	53.3976	-36.1412	52.920229	-36.30818	36.797911	-53.03906	237.95777124	-54.60123537	60.7695	55392.8956597222	2010-07-15 21:29:45	55399.3676273148	2010-07-22 08:49:23	705031020	302.1753	450	302.1753	302.1833	0	302.1833	2	2	0	2	1	0	0	251.0612	251.0612	425.5339	2	PROCESSED	57552.8844791667	2016-06-13 21:13:39	55287	2010-04-01 00:00:00	55413.8216435185	2010-08-05 19:43:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051112	We propose 3 observations (~4 days each) of the Seyfert galaxy NGC 1365, at 2-week intervals. We aim to use eclipses to unambiguously identify the broad Fe K line, examine variability of the HXD/PIN excess, and to search for changes in the physical properties of the ionized absorber in this bright, nearby AGN. Shorter observations of this galaxy with XMM-Newton, Chandra and Suzaku showcase several remarkable physical traits: (1) FeXXV and FeXXVI K-shell absorption lines (the highest s/n detection so far among AGN), (2) rapidly varying cold absorption, (3) a highly significant relativistic Fe K emission line, and (4) a factor ~4 excess flux at high energies. The proposed observations will provide legacy spectra for what is arguably the single most physically-revealing obscured AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	LAURA BRENNEMAN		USA	5	AO5	A LONG LOOK AT NGC 1365: DISC TOMOGRAPHY, IONIZED ABSORPTION AND HIGH ENERGY EXCESS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705031020/	Quick Look
97	ESO 511-G030	214.8456	-26.6457	214.126189	-26.416188	221.40386	-12.022179	326.23004886	32.21661925	292.391	56156.7622337963	2012-08-17 18:17:37	56157.7960416667	2012-08-18 19:06:18	707023030	51.9172	270	51.9252	51.9252	0	51.9172	3	2	0	2	1	0	0	52.011	52.011	89.3158	3	PROCESSED	57606.8813194444	2016-08-06 21:09:06	56640	2013-12-14 00:00:00	56272.6998148148	2012-12-11 16:47:44	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071413	The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		USA	7	AO7	MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707023030/	Quick Look
98	PUP A : INTERIOR	125.5916	-42.8951	125.161363	-42.733897	147.106586	-59.478577	260.333956	-3.34905821	276.8883	53842.5813541667	2006-04-17 13:57:09	53842.9127199074	2006-04-17 21:54:19	501088010	20.2709	20	20.2924	20.2949	20.2789	20.2709	1	1	1	1	1	0	0	19.9519	19.9519	28.6239	0	PROCESSED	57533.5042476852	2016-05-25 12:06:07	54401	2007-10-28 00:00:00	53906.8948611111	2006-06-20 21:28:36	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501088010/	Quick Look
99	OFF-FIELD2	312.2284	-9.8925	311.551158	-10.078408	311.903273	7.617962	37.42106637	-30.55240738	73.668	56784.946724537	2014-05-07 22:43:17	56787.0627314815	2014-05-10 01:30:20	509043010	80.156	80	80.156	80.156	0	80.156	2	2	0	2	1	0	0	69.6142	69.6142	182.8079	1	PROCESSED	57615.1427430556	2016-08-15 03:25:33	56748	2014-04-01 00:00:00	56861.5828240741	2014-07-23 13:59:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091321	Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma.	GALACTIC DIFFUSE EMISSION	5	A	ANJALI GUPTA		USA	9	AO9	CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509043010/	Quick Look
100	A 2218 CENTER	249.0052	66.205	248.955095	66.304813	172.75657	81.615548	97.72589248	38.11630228	233.3294	53669.4904050926	2005-10-26 11:46:11	53670.1905555556	2005-10-27 04:34:24	800019010	31.9354	35	31.9434	31.9434	31.9354	31.9434	2	2	2	2	1	0	0	28.9371	28.9371	60.4879	1	PROCESSED	57527.6471990741	2016-05-19 15:31:58	54247	2007-05-27 00:00:00	54036.9596990741	2006-10-28 23:01:58	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001096	To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI		JAP	0	SWG	SEARCH FOR OXYGEN LINES FROM WARM IGM		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800019010/	Quick Look
101	ABELL 2259	260.1834	27.7413	259.686949	27.789931	256.20097	50.711544	50.50845469	31.05916058	109.9997	57082.4117476852	2015-03-01 09:52:55	57083.6002199074	2015-03-02 14:24:19	809081020	42.5928	42.5	42.5928	43.0168	0	43.0568	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.687650463	2016-08-17 16:30:13	57465	2016-03-18 00:00:00	57097.407037037	2015-03-16 09:46:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091526	Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	9	AO9	REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809081020/	Quick Look
102	SPT-CL J0000-5748	0.2511	-57.8123	359.609856	-58.090789	327.861661	-51.025666	315.62746494	-58.05556131	46.7517	55694.989849537	2011-05-13 23:45:23	55696.1169097222	2011-05-15 02:48:21	806074010	50.3986	50	50.3986	50.3986	0	50.3986	2	2	0	2	1	0	0	42.4563	42.4563	97.3498	0	PROCESSED	57602.0636921296	2016-08-02 01:31:43	56072	2012-05-25 00:00:00	55705.1979166667	2011-05-24 04:45:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061531	We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ERIC MILLER		USA	6	AO6	THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806074010/	Quick Look
103	ETA CARINAE	161.2306	-59.7313	160.744613	-59.468015	202.194654	-58.966617	287.60339978	-0.67900846	291.9998	54992.8234143518	2009-06-10 19:45:43	54994.2918865741	2009-06-12 07:00:19	404038010	51.2259	45	51.2259	51.2339	0	51.2339	2	2	0	2	1	0	0	49.1186	49.1186	126.8398	0	PROCESSED	57547.5667361111	2016-06-08 13:36:06	55378	2010-07-01 00:00:00	55006.2447569444	2009-06-24 05:52:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041204	The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements.	GALACTIC POINT SOURCES	4	A	KENJI HAMAGUCHI		USA	4	AO4	HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CAR	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404038010/	Quick Look
104	Z235	10.9622	24.4059	10.298374	24.132304	19.875378	18.073678	120.72614401	-38.43334342	59.0539	53944.0060185185	2006-07-28 00:08:40	53944.6148032407	2006-07-28 14:45:19	801083010	20.0335	20	20.0415	20.0415	20.0415	20.0335	2	2	2	2	1	0	0	19.5263	19.5263	52.5899	1	PROCESSED	57535.0666782407	2016-05-27 01:36:01	54401	2007-10-28 00:00:00	53955.6800925926	2006-08-08 16:19:20	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801083010/	Quick Look
105	CYGNUS X-1	299.5777	35.2112	299.107757	35.074782	313.651801	54.261993	71.33781217	3.08063246	52.2303	57169.4748148148	2015-05-27 11:23:44	57170.7827893518	2015-05-28 18:47:13	410018010	11.0177	50	11.0177	12.2057	0	11.7469	4	3	0	3	1	0	0	26.1315	26.1315	110.7598	0	PROCESSED	57618.8568171296	2016-08-18 20:33:49	57626	2016-08-26 00:00:00	57183.6630902778	2015-06-10 15:54:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101725	We propose to observe Cygnus X-1 with NuSTAR (for 30 ks) and Suzaku (for 50 ks) in any spectral state in order to measure the reflection component and constrain the properties of the inner accretion disk, including the location of the inner radius, the geometry of the hard X-ray source, and the inclination. Observations made in the first two years of the NuSTAR mission have raised the interesting possibility that the inner disk inclination may differ from the orbital inclination, and this could occur if the black hole spin is misaligned. The proposed NuSTAR/Suzaku observation would be at the orbital phase where absorption due to stellar wind material is at a minimum, providing a clean measurement of the iron line profile and a significant improvement over the existing observations.	GALACTIC POINT SOURCES	4	A	JOHN TOMSICK		USA	10	AO10	THE INNER ACCRETION DISK AROUND THE RAPIDLY ROTATING BLACK HOLE IN CYGNUS X-1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410018010/	Quick Look
106	NGC 2992	146.4207	-14.2696	145.81924	-14.038457	154.003817	-26.061971	249.65504756	28.81616071	88.7924	53693.8781597222	2005-11-19 21:04:33	53694.9759722222	2005-11-20 23:25:24	700005020	37.4935	120	37.6565	39.6915	37.4935	37.8205	1	1	1	1	1	0	0	33.8991	33.8991	94.8479	1	PROCESSED	57528.0334490741	2016-05-20 00:48:10	54247	2007-05-27 00:00:00	54037.7316087963	2006-10-29 17:33:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001013	NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability.	EXTRAGALACTIC COMPACT SOURCES	7	A	YUICHI TERASHIMA		JAP	0	SWG	THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700005020/	Quick Look
107	SWIFTJ1010.1-5747	152.7309	-57.8539	152.293849	-57.606865	193.450641	-60.897616	282.8705066	-1.37559689	290.7012	53891.2175	2006-06-05 05:13:12	53891.5544560185	2006-06-05 13:18:25	401055010	19.1717	20	19.1717	19.1717	19.1717	19.1717	2	2	2	2	1	0	0	17.8778	17.8778	29.0879	0	PROCESSED	57534.4906944444	2016-05-26 11:46:36	54401	2007-10-28 00:00:00	53926.1075347222	2006-07-10 02:34:51	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011132	INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	1	AO1	HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401055010/	Quick Look
108	A3376 WEST RELIC	90.0415	-39.9946	89.634521	-39.995405	90.079962	-63.436398	246.43569548	-26.38071178	132.0018	53681.5938078704	2005-11-07 14:15:05	53684.7883912037	2005-11-10 18:55:17	800011010	126.9969	150	126.9969	127.1809	127.0769	127.0289	2	2	2	2	1	0	0	112.9113	112.9113	230.9397	3	PROCESSED	57528.0013541667	2016-05-20 00:01:57	54247	2007-05-27 00:00:00	54037.6050231482	2006-10-29 14:31:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001039	We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KAZUHIRO NAKAZAWA		JAP	0	SWG	SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800011010/	Quick Look
109	E0102-72	16.027	-72.0223	15.622199	-72.290248	314.64413	-65.039289	301.54815221	-45.07189388	294.0751	53768.8467592593	2006-02-02 20:19:20	53769.4065393518	2006-02-03 09:45:25	100044030	20.8277	20	20.8357	20.8437	20.8437	20.8277	2	2	2	2	1	0	0	20.2688	20.2688	48.36	1	PROCESSED	57532.8615740741	2016-05-24 20:40:40	54247	2007-05-27 00:00:00	53905.6764351852	2006-06-19 16:14:04	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001097	We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	0	SWG	XIS FLIGHT CAIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100044030/	Quick Look
110	ETA CARINAE	161.248	-59.6859	160.761598	-59.422588	202.142	-58.929196	287.58997588	-0.63475906	156.124	53769.4163194444	2006-02-03 09:59:30	53769.9481944444	2006-02-03 22:45:24	100045010	21.3678	20	21.3678	21.3678	21.3678	21.3678	2	2	2	2	1	0	0	18.1458	18.1458	45.9459	1	PROCESSED	57532.9369907407	2016-05-24 22:29:16	54247	2007-05-27 00:00:00	54040.9846643518	2006-11-01 23:37:55	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001097	We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	0	SWG	XIS FLIGHT CAIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100045010/	Quick Look
111	BULGE 6	282.6839	-33.8925	281.860158	-33.951684	280.687841	-10.9215	1.99857856	-14.59644221	88.3467	53802.7373032407	2006-03-08 17:41:43	53803.0466087963	2006-03-09 01:07:07	500003010	14.2617	10	14.2617	14.2617	14.2617	14.2617	2	2	2	2	1	0	0	11.414	11.414	26.7159	1	PROCESSED	57533.1570833333	2016-05-25 03:46:12	54247	2007-05-27 00:00:00	54041.7424305556	2006-11-02 17:49:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001014	Leading .	GALACTIC DIFFUSE EMISSION	5	A	DAN MCCAMMON		JAP	0	SWG	THE SOFT GALACTIC BULGE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500003010/	Quick Look
112	X1630-472	248.4772	-47.3405	247.556757	-47.236251	254.058584	-25.081993	336.93627828	0.30053306	75.5959	53794.9708333333	2006-02-28 23:18:00	53795.6968055556	2006-03-01 16:43:24	400010030	21.5216	200	21.5216	21.5216	21.5216	21.5216	2	2	2	2	1	0	0	19.0328	19.0328	62.718	0	PROCESSED	57533.1079050926	2016-05-25 02:35:23	54247	2007-05-27 00:00:00	54041.5956018518	2006-11-02 14:17:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001058	We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		JAP	0	SWG-TOO	FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010030/	Quick Look
113	JUPITER	226.5948	-16.1928	225.896045	-16.000249	228.688969	1.24261	343.98613419	35.70433361	118.4906	53791.7941319445	2006-02-25 19:03:33	53792.7940277778	2006-02-26 19:03:24	401001020	37.704	36	37.704	37.704	37.704	37.704	1	1	1	1	1	0	0	32.7781	32.7781	86.36	1	PROCESSED	57533.0943981482	2016-05-25 02:15:56	54401	2007-10-28 00:00:00	53905.5035416667	2006-06-19 12:05:06	3.0.22.43	6	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011003	We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure.	GALACTIC POINT SOURCES	4	C	RONALD ELSNER		USA	1	AO1	JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001020/	Quick Look
114	SIGMA^2 CRB	243.6552	33.7881	243.181435	33.91264	231.394365	53.752123	54.56402364	46.14689859	281.1207	53969.4764467593	2006-08-22 11:26:05	53972.1925231482	2006-08-25 04:37:14	401034010	109.1604	110	109.1904	109.1604	109.1684	109.1764	2	2	2	2	1	0	0	98.8376	98.8376	234.6539	3	PROCESSED	57535.3877777778	2016-05-27 09:18:24	54526	2008-03-01 00:00:00	54021.2578587963	2006-10-13 06:11:19	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011025	Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission from RS CVn binaries. We propose to obtain 110 ksec (3 day elapsed time) observations of the RS CVn systems Sigma^2 CrB (F6V + G0V) and Sigma Gem (K0III +?). Our goals are i) to better characterize their hard (> 10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, and iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability in the 10-25 keV region provided by HXD.	GALACTIC POINT SOURCES	4	B	ALEXANDER BROWN		USA	1	AO1	SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL EMISSION ON THE RS CVN BINARIES SIGMA^2 CRB AND SIGMA GEM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401034010/	Quick Look
115	4U 1820-30	275.9207	-30.3623	275.117497	-30.389079	275.135384	-7.027059	2.78792233	-7.91550172	265.9754	53992.9234606482	2006-09-14 22:09:47	53993.6605902778	2006-09-15 15:51:15	401047010	25.7008	37	25.7008	25.8109	25.7239	25.7148	2	1	2	2	1	0	0	31.8782	31.8782	63.6339	1	PROCESSED	57535.6012962963	2016-05-27 14:25:52	54526	2008-03-01 00:00:00	54021.2227083333	2006-10-13 05:20:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011113	The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme.	GALACTIC POINT SOURCES	4	B	JON MILLER		USA	1	AO1	A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401047010/	Quick Look
116	4U 1636-536	250.2259	-53.7533	249.229501	-53.656802	256.460315	-31.236099	332.911352	-4.8168543	100.7755	54188.4720717593	2007-03-29 11:19:47	54188.7856944445	2007-03-29 18:51:24	401050050	12.2418	38	12.2498	12.2418	0	12.2498	2	1	0	2	1	0	0	11.804	11.804	27.088	0	PROCESSED	57537.9973148148	2016-05-29 23:56:08	54695	2008-08-17 00:00:00	54200.4687731482	2007-04-10 11:15:02	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011117	Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.	GALACTIC POINT SOURCES	4	A	JEROEN HOMAN		USA	1	AO1	THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050050/	Quick Look
117	4U1907+09	287.4013	9.8378	286.806482	9.755913	290.334973	32.058259	43.74739314	0.48531727	60.2599	53857.2580324074	2006-05-02 06:11:34	53858.7322222222	2006-05-03 17:34:24	401057010	58.4403	60	58.4403	58.4563	58.4483	58.4563	2	2	2	2	1	0	0	38.8215	38.8215	127.3539	1	PROCESSED	57533.6690509259	2016-05-25 16:03:26	54401	2007-10-28 00:00:00	53913.4367476852	2006-06-27 10:28:55	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011133	We propose 60ksec of Suzaku observations of the high mass X-ray binary 4U1907+09, to study the little known spectrum of the source below 2keV and to measure its behavior during its frequent dips, where matter ceases to accrete onto the magnetic poles of the neutron star. Making use of Suzaku's unique broad band capabilities, we will also perform pulse phase spectroscopy of the cyclotron line and study the parameters of the fundamental and first harmonic cyclotron lines, as 4U1907+09 is one of the few accreting neutron stars where two cyclotron lines lie within the energy range of the XIS and HXD-PIN detectors. The scientific aims of this proposal address questions within NASA's Goals and Research Focus Area ``Structure and Evolution of the Universe''.	GALACTIC POINT SOURCES	4	A	KATJA POTTSCHMIDT		USA	1	AO1	THE BROAD BAND SPECTRUM OF 4U1907+09	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401057010/	Quick Look
118	BZ UMA	133.4243	57.801	132.45894	57.99062	117.906758	38.491504	159.01672768	38.83001001	307.4767	54549.9926388889	2008-03-24 23:49:24	54550.4446064815	2008-03-25 10:40:14	402046010	29.7466	20	29.7546	29.7546	0	29.7466	2	2	0	2	1	0	0	24.9212	24.9212	39.0459	0	PROCESSED	57541.9622106482	2016-06-02 23:05:35	54933	2009-04-12 00:00:00	54566.2225231482	2008-04-10 05:20:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021105	Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies.	GALACTIC POINT SOURCES	4	C	KOJI MUKAI		USA	2	AO2	BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402046010/	Quick Look
119	4U1705-44	257.2347	-44.0965	256.331587	-44.032824	260.198067	-21.087901	343.32858118	-2.34307771	294.8341	54381.763275463	2007-10-08 18:19:07	54382.2015509259	2007-10-09 04:50:14	402051020	21.9713	15	21.9793	21.981	0	21.9713	1	1	0	1	1	0	0	15.688	15.688	37.856	1	PROCESSED	57540.198125	2016-06-01 04:45:18	54770	2008-10-31 00:00:00	54402.6586226852	2007-10-29 15:48:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021113	We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability.	GALACTIC POINT SOURCES	4	A	RONALD REMILLARD		USA	2	AO2	X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402051020/	Quick Look
120	AQL X-1	287.8179	0.5789	287.179626	0.495179	289.378971	22.828716	35.71351779	-4.14685757	277.9777	54376.9927777778	2007-10-03 23:49:36	54377.3516087963	2007-10-04 08:26:19	402053020	15.1326	15	15.1406	15.1423	0	15.1326	1	1	0	1	1	0	0	11.8908	11.8908	30.9999	1	PROCESSED	57540.1490277778	2016-06-01 03:34:36	54771	2008-11-01 00:00:00	54403.9157175926	2007-10-30 21:58:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021114	We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data.	GALACTIC POINT SOURCES	4	A	RONALD REMILLARD		USA	2	AO2-TOO	X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402053020/	Quick Look
121	IGR J16207-5129	245.1891	-51.5041	244.232474	-51.385129	252.515963	-29.556446	332.45561032	-1.05025433	89.5006	54526.8661111111	2008-03-01 20:47:12	54527.7502199074	2008-03-02 18:00:19	402065020	32.6127	30	32.7095	32.7133	0	32.6127	2	2	0	2	1	0	0	28.3312	28.3312	76.3759	0	PROCESSED	57541.7496180556	2016-06-02 17:59:27	54901	2009-03-11 00:00:00	54535.208599537	2008-03-10 05:00:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021122	We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities.	GALACTIC POINT SOURCES	4	B	JOHN TOMSICK		USA	2	AO2	LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402065020/	Quick Look
122	KT PER	24.2933	50.9468	23.514247	50.69234	43.593687	37.546222	130.24865907	-11.27406186	260.9001	54843.8957060185	2009-01-12 21:29:49	54844.5334953704	2009-01-13 12:48:14	403041010	29.1957	20	29.1957	29.1957	0	29.1957	2	2	0	2	1	0	0	28.1658	28.1658	55.0899	0	PROCESSED	57545.1649537037	2016-06-06 03:57:32	55328	2010-05-12 00:00:00	54854.0547916667	2009-01-23 01:18:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031144	Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates.	GALACTIC POINT SOURCES	4	C	KOJI MUKAI		USA	3	AO3	BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403041010/	Quick Look
123	IGRJ16393-4643	249.7688	-46.7009	248.852096	-46.602507	254.906032	-24.312906	338.00177501	0.07896045	111.6627	55267.9865740741	2010-03-12 23:40:40	55269.4508564815	2010-03-14 10:49:14	404056010	50.54	50	50.564	50.54	0	50.564	2	2	0	2	1	0	0	42.2565	42.2565	126.4678	1	PROCESSED	57550.8754166667	2016-06-11 21:00:36	55647	2011-03-27 00:00:00	55279.4686689815	2010-03-24 11:14:53	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041234	Stellar winds play a critical role in several as yet poorly understood astrophysical processes. One of the best laboratories for studying winds is in wind fed Supergiant High Mass X-ray binaries. Using the neutron star (NS) as a backlight, variable absorption in X-rays measures column density variations in the secondary star wind. A recent explosion in the number of known HMXBs has defined two additional subclasses of HMXBs, potentially related through geometry and wind properties: 1) heavily obscured sources and 2) so-called Supergiant Fast X-ray Transients (SFXTs). We propose observations of 2 obscured sgHMXBs and 2 SFXTs to monitor the column density. This will test wind models and probe whether these subclasses are related to one another and to classical HMXBs through wind parameters.	GALACTIC POINT SOURCES	4	C	DAVID MORRIS		USA	4	AO4	PROBING DONOR STAR WIND STRUCTURE IN HMXBS THROUGH VARIABLE ABSORPTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404056010/	Quick Look
124	LOCKMANHOLE	163.4063	57.6108	162.636897	57.876997	137.149157	45.549363	148.98193179	53.14624927	119.611	53688.2372337963	2005-11-14 05:41:37	53689.8300694444	2005-11-15 19:55:18	100046010	76.9806	100	76.9806	77.0446	77.0126	77.0206	2	2	2	2	1	0	0	94.5107	94.5107	137.6079	3	PROCESSED	57528.0048148148	2016-05-20 00:06:56	54247	2007-05-27 00:00:00	54037.5889814815	2006-10-29 14:08:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001098	We propose a 100 ks observation of LockmanHole with Suzaku. The main purpose is to obtain a template dataset of HXD background.	CALIBRATION	1	A	MOTOHIDE KOKUBUN		JAP	0	SWG	BACKGROUND ESTABLISHMENT OF HXD	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100046010/	Quick Look
125	CH UMA	151.7457	67.5324	150.779554	67.776446	122.251575	50.881841	142.91256562	42.65793237	289.9979	56048.5009490741	2012-05-01 12:01:22	56049.4815046296	2012-05-02 11:33:22	407043010	45.2045	40	45.2045	45.2045	0	45.2045	2	2	0	2	1	0	0	43.3751	43.3751	84.6981	0	PROCESSED	57605.3249652778	2016-08-05 07:47:57	56435	2013-05-23 00:00:00	56068.6246180556	2012-05-21 14:59:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071212	The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates?	GALACTIC POINT SOURCES	4	A	KOJI MUKAI		USA	7	AO7	DWARF NOVAE WITH EXTREME WHITE DWARF MASSES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407043010/	Quick Look
126	A2572B	349.6066	18.7294	348.98329	18.45586	358.210513	21.259827	94.21850787	-38.90117923	59.1565	53922.7742939815	2006-07-06 18:34:59	53923.3002199074	2006-07-07 07:12:19	801073010	24.0595	21	24.0755	24.0595	24.0675	24.0755	2	2	2	2	1	0	0	21.4951	21.4951	45.3979	1	PROCESSED	57534.8583912037	2016-05-26 20:36:05	54401	2007-10-28 00:00:00	53930.6043055556	2006-07-14 14:30:12	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801073010/	Quick Look
127	COMA W SHOCK1	194.1832	28.2738	193.578654	28.544023	180.637957	31.358455	77.58391557	88.36116739	275.406	56475.3084143518	2013-07-02 07:24:07	56475.66125	2013-07-02 15:52:12	808090010	16.692	15	16.692	16.716	0	16.7	2	2	0	2	1	0	0	13.638	13.638	30.4759	1	PROCESSED	57611.6582407407	2016-08-11 15:47:52	56897	2014-08-28 00:00:00	56524.6518518518	2013-08-20 15:38:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081529	Our analysis of Suzaku data of the Coma Cluster revealed an intriguing correlation between the outer edge of its radio halo and the thermodynamic properties of the gas. This correlation seems to be the most pronounced in the western direction where the temperature drops from about 10keV in the annulus spanning 35'-41' to only 1.7keV in the annulus spanning 50'-60'. The Planck Collaboration found a marked local steepening of the radial gradient of the SZ signal at this location and interpret this feature as a shock with a Mach number of about 2. Unfortunately, we currently lack X-ray coverage towards the W in this critical range of 41'-50'. We therefore propose two additional pointings with a total exposure time of 30ks, that will allow us to resolve the temperature gradient in this region.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AURORA SIMIONESCU		USA	8	AO8	THE MISSING PUZZLE PIECE IN THE COMA SHOCK FRONT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808090010/	Quick Look
128	AE AQUARII	310.0612	-0.931	309.416636	-1.108991	312.236832	16.82972	45.23545862	-24.46836188	250.6241	54033.2319907407	2006-10-25 05:34:04	54034.3829282407	2006-10-26 09:11:25	400001020	47.9743	50	47.9743	48.5956	48.1316	48.3103	2	2	2	2	1	0	0	45.5384	45.5384	99.4239	1	PROCESSED	57526.8238773148	2016-05-18 19:46:23	54526	2008-03-01 00:00:00	54109.7083449074	2007-01-09 17:00:01	3.0.22.43	9	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001004	We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku.	GALACTIC POINT SOURCES	4	A	YUKIKATSU TERADA		JAP	0	SWG	SEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKU	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400001020/	Quick Look
129	GX 349+2	256.4194	-36.3657	255.579957	-36.298328	258.779942	-13.451385	349.14166441	2.79326977	78.9359	53813.9267708333	2006-03-19 22:14:33	53814.6043402778	2006-03-20 14:30:15	400003020	28.1177	50	28.1177	28.1317	28.1204	28.1204	2	2	2	2	1	0	0	25.6573	25.6573	58.538	0	PROCESSED	57533.2767939815	2016-05-25 06:38:35	54247	2007-05-27 00:00:00	54042.1657407407	2006-11-03 03:58:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001026	We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure.	GALACTIC POINT SOURCES	4	A	HIROMITSU TAKAHASHI		JAP	0	SWG	SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES)	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400003020/	Quick Look
130	IW ERIDANI	66.4802	-19.763	65.931423	-19.87535	60.255555	-40.808034	216.43667954	-40.61449502	63.2719	56870.0005092593	2014-08-01 00:00:44	56870.9730902778	2014-08-01 23:21:15	409030010	39.4581	40	39.4581	39.8021	0	39.8341	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.4481134259	2016-08-16 10:45:17	57270	2015-09-05 00:00:00	56902.7186574074	2014-09-02 17:14:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091211	Cataclysmic variables (CVs) detected in the INTEGRAL and Swift BAT hard X-ray surveys are predominantly magnetic systems of the intermediate polar subtype. However, as the survey sensitivity improves, an increasing number of polars are also detected as hard X-ray sources, even though the majority of polars are soft X-ray bright and hard X-ray faint. Over the long term, we hope to understand why most polars are soft X-ray dominated, and why a subset is hard X-ray bright. Here we propose Suzaku observations of four poorly studied BAT-detected polars, 1RXS J032540.0-081442, Swift J2319.4+2619, IW Eri, and IGR J14536-5522, supported by ground-based observations including optical polarimetry, to determine their system parameters.	GALACTIC POINT SOURCES	4	A	KOJI MUKAI		USA	9	AO9	HARD X-RAY BRIGHT POLARS: WHY ARE THEY DIFFERENT?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409030010/	Quick Look
131	XB1916-053	289.7007	-5.2492	289.035593	-5.341539	290.517676	16.79898	31.34828117	-8.46968862	261.8039	56944.6811574074	2014-10-14 16:20:52	56948.5140740741	2014-10-18 12:20:16	409032010	155.8851	300	155.8851	155.8851	0	155.8851	2	2	0	2	1	0	0	8.7968	8.7968	19.7276	0	PROCESSED	57616.6949768518	2016-08-16 16:40:46	56748	2014-04-01 00:00:00	57017.41125	2014-12-26 09:52:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091221	XB1916-053 is a prototypical dipping low mass X-ray binary (LMXB) with a dip recurrence period of 3000.6+-0.2s. However, extensive optical observations also show a longer stable period of 3027s. The former is most likely the orbital period, and the latter the superhump period caused by the precession of an elliptical accretion disk at a period of 3.9 days, representing the beat period between optical and X-ray periods. The morphology of the X-ray dips does indeed change dramatically over several days, but existing data suggest a somewhat longer period for the dip morphology cycle of 4.7 days. Here we propose a 300ks Suzaku observation of XB1916-053 with as few interruptions as possible, to conduct a definitive timing and spectroscopic study of its disk emission and dipping activity.	GALACTIC POINT SOURCES	4	B	ALAN SMALE		USA	9	AO9	THE PRECESSING DISK IN THE DIPPING X-RAY BINARY XB1916-053	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409032010/	Quick Look
132	SCT X-1	278.8598	-7.62	278.182099	-7.661259	279.107067	15.540876	24.33170335	0.06100641	260.9954	56952.1146412037	2014-10-22 02:45:05	56953.1389814815	2014-10-23 03:20:08	409033020	38.5811	34	38.5811	38.6687	0	38.6767	3	3	0	3	0	0	0	0	0	0	0	PROCESSED	57616.6602314815	2016-08-16 15:50:44	57373	2015-12-17 00:00:00	57006.4003240741	2014-12-15 09:36:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091222	We propose to observe the accreting 112s pulsar Scutum X-1 with Suzaku for 50ks. The optical companion is a late type giant or supergiant, making this a rare, persistent, non-OB-type wind accreting, Symbiotic X-ray Binary (SyXB). After initial flaring in the 1970s, the source generally exhibited low flux levels and has only rarely been observed. We will constrain the broadband spectrum, check for signs of wind accretion (variable absorption, log-normal count rate distribution), search for an iron fluorescence line, update the pulse period evolution, and compare to other Suzaku observations of SyXBs, especially to a quiescent observation of the prototype SyXB 4U 1954+31.	GALACTIC POINT SOURCES	4	A	KATJA POTTSCHMIDT		USA	9	AO9	THE SYMBIOTIC X-RAY BINARY SCUTUM X-1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409033020/	Quick Look
133	X1630-472	248.4828	-47.3401	247.56235	-47.235876	254.062648	-25.080987	336.93914719	0.29801709	78.3341	53774.6318981482	2006-02-08 15:09:56	53775.1390972222	2006-02-09 03:20:18	400010010	22.1902	200	22.1902	22.1902	22.1902	22.1902	1	1	1	1	1	0	0	22.247	22.247	43.816	0	PROCESSED	57532.9380787037	2016-05-24 22:30:50	54247	2007-05-27 00:00:00	54040.9540856482	2006-11-01 22:53:53	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001058	We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		JAP	0	SWG-TOO	FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010010/	Quick Look
134	MRK 509	311.0374	-10.7203	310.356339	-10.901854	310.541946	7.132317	35.97290357	-29.85106035	73.7532	57143.3705671296	2015-05-01 08:53:37	57144.6814930556	2015-05-02 16:21:21	410017010	54.2728	50	54.2757	54.2757	0	54.2728	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.0659722222	2016-08-18 01:35:00	57593	2016-07-24 00:00:00	57225.3881944445	2015-07-22 09:19:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101708	We propose combined Suzaku 50~ks and NuSTAR 200~ks observations of the bright Seyfert 1 galaxy Mrk~509 for the purpose of making a detailed study of the spectrum of radiation reflected from the accretion disk. Our chief aim is to constrain both the spin of the black hole and the properties of the corona that illuminates the disk. The combination of NuSTAR's high-sensitivity in the hard X-ray band, the soft-band coverage of Suzaku, and our state-of-the-art relativistic reflection models will allow us to break degeneracies between different scenarios currently proposed to explain the broadband spectrum of this exceptionally bright and much-studied source.	GALACTIC POINT SOURCES	4	A	JAVIER GARCIA		USA	10	AO10	OBSERVING THE STRONG-FIELD REGION OF THE AGN IN MRK~509	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410017010/	Quick Look
135	73P/SW3	279.6627	33.4734	279.203358	33.427762	284.650097	56.423756	62.35168426	17.03145652	46.5564	53862.4804282407	2006-05-07 11:31:49	53862.5419444444	2006-05-07 13:00:24	500012020	3.248	5	3.248	3.248	3.248	3.248	1	1	1	1	1	0	0	2.1119	2.1119	5.2799	0	PROCESSED	57533.7332407407	2016-05-25 17:35:52	54256	2007-06-05 00:00:00	54042.2282175926	2006-11-03 05:28:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500012020/	Quick Look
136	73P/SW3	316.717	24.6807	316.164001	24.478965	328.484877	39.12074	71.53645371	-15.07849931	72.7087	53868.1752314815	2006-05-13 04:12:20	53868.2085532407	2006-05-13 05:00:19	500013010	2.353	20	2.353	2.353	2.353	2.353	1	1	1	1	1	0	0	2.595	2.595	2.8719	0	PROCESSED	57534.2831597222	2016-05-26 06:47:45	54256	2007-06-05 00:00:00	54042.2312268518	2006-11-03 05:32:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013010/	Quick Look
137	73P/SW3	317.1042	24.5187	316.549923	24.315676	328.827114	38.838912	71.64340536	-15.45205291	72.7099	53868.2091666667	2006-05-13 05:01:12	53868.2752199074	2006-05-13 06:36:19	500013020	3.225	20	3.225	3.225	3.225	3.225	1	1	1	1	1	0	0	3.467	3.467	5.7039	0	PROCESSED	57534.2879398148	2016-05-26 06:54:38	54256	2007-06-05 00:00:00	54042.2634027778	2006-11-03 06:19:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013020/	Quick Look
138	73P/SW3	319.1503	23.6322	318.589279	23.422515	330.602424	37.314629	72.21442919	-17.44595626	72.7095	53868.5425	2006-05-13 13:01:12	53868.6085532407	2006-05-13 14:36:19	500013070	3.0624	20	3.0624	3.0624	3.0624	3.0624	1	1	1	1	1	0	0	2.088	2.088	5.688	1	PROCESSED	57534.3049074074	2016-05-26 07:19:04	54256	2007-06-05 00:00:00	54042.3037268518	2006-11-03 07:17:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013070/	Quick Look
139	73P/SW3	17.8447	-9.1515	17.217751	-9.416998	12.842123	-15.443966	138.54867442	-71.41609802	59.3994	53893.7363888889	2006-06-07 17:40:24	53893.8023032407	2006-06-07 19:15:19	500014020	3.2369	35	3.2369	3.2369	3.2369	3.2369	1	1	1	1	1	0	0	2.478	2.478	5.6879	0	PROCESSED	57534.5816435185	2016-05-26 13:57:34	54267	2007-06-16 00:00:00	54052.5079861111	2006-11-13 12:11:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014020/	Quick Look
140	73P/SW3	18.0085	-9.2093	17.381763	-9.474557	12.972897	-15.560645	139.0853548	-71.43220951	59.4015	53893.9358333333	2006-06-07 22:27:36	53894.0023032407	2006-06-08 00:03:19	500014050	3.235	35	3.235	3.235	3.235	3.235	1	1	1	1	1	0	0	2.5041	2.5041	5.7359	0	PROCESSED	57534.5878125	2016-05-26 14:06:27	54267	2007-06-16 00:00:00	54052.5317361111	2006-11-13 12:45:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014050/	Quick Look
141	73P/SW3	18.1094	-9.2436	17.482792	-9.508708	13.054019	-15.631304	139.41528011	-71.44015907	59.3996	53894.0691666667	2006-06-08 01:39:36	53894.1356365741	2006-06-08 03:15:19	500014070	2.2209	35	2.2209	2.2209	2.2209	2.2209	1	1	1	1	1	0	0	1.939	1.939	5.7359	1	PROCESSED	57534.589849537	2016-05-26 14:09:23	54267	2007-06-16 00:00:00	54052.5472800926	2006-11-13 13:08:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014070/	Quick Look
142	73P/SW3	18.2503	-9.299	17.623885	-9.563897	13.164284	-15.736856	139.88257526	-71.45759255	59.3985	53894.2691435185	2006-06-08 06:27:34	53894.3356134259	2006-06-08 08:03:17	500014100	1.3121	35	1.3121	1.3121	1.3121	1.3121	1	1	1	1	1	0	0	1.322	1.322	5.742	0	PROCESSED	57534.5960185185	2016-05-26 14:18:16	54267	2007-06-16 00:00:00	54052.5405324074	2006-11-13 12:58:22	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014100/	Quick Look
143	73P/SW3	18.435	-9.3697	17.808837	-9.63432	13.309685	-15.873419	140.49459076	-71.47695116	59.4003	53894.5358333333	2006-06-08 12:51:36	53894.6016087963	2006-06-08 14:26:19	500014140	1.977	35	1.977	1.977	1.977	1.977	1	1	1	1	1	0	0	1.951	1.951	5.6719	0	PROCESSED	57534.60375	2016-05-26 14:29:24	54267	2007-06-16 00:00:00	54052.5450231482	2006-11-13 13:04:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014140/	Quick Look
144	MBM12	44.0042	19.487	43.295962	19.285573	47.250431	2.610049	159.18888296	-34.46916863	253.4644	53769.9600578704	2006-02-03 23:02:29	53772.6460416667	2006-02-06 15:30:18	500015010	102.9371	100	102.9371	102.9371	102.9371	102.9371	2	2	2	2	1	0	0	93.6709	93.6709	232.0499	1	PROCESSED	57532.9850694444	2016-05-24 23:38:30	54247	2007-05-27 00:00:00	54041.1327662037	2006-11-02 03:11:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001059	Suzaku can potentially determine the time since the nearby supernova that created (or reheated) the Local Hot Bubble (LHB) by measuring the ratio of the O VII/O VIII lines emitted by the LHB. The LHB temperature is ~10^6 K, and in equilibrium we would expect no O VIII emission. However, the LHB is almost certainly not in equilibrium, and it is quite possible that significant O^{+7} is still recombining (and emitting O VIII) following its creation in the most recent local supernova 2-4 Myr ago. We propose to measure these lines from the LHB using the nearby molecular cloud MBM12 as a curtain to shadow more distant emission. Even if O VIII is not detected, the O VII measurement will be the first unambiguous measurement of a line from the LHB.	GALACTIC DIFFUSE EMISSION	5	A	RANDALL SMITH		JAP	0	SWG	DATING THE LOCAL HOT BUBBLE WITH SUZAKU	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500015010/	Quick Look
145	CYGNUS LOOP NE4	313.5005	32.369	312.987812	32.178281	329.006135	47.302265	75.72495347	-7.98937114	221.2023	53704.2368287037	2005-11-30 05:41:02	53704.7661342593	2005-11-30 18:23:14	500023010	25.0049	20	25.0049	25.2689	25.0067	25.0689	2	2	2	2	1	0	0	25.1249	25.1249	45.726	1	PROCESSED	57532.3510763889	2016-05-24 08:25:33	54247	2007-05-27 00:00:00	54038.67625	2006-10-30 16:13:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001093	We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	0	SWG	CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500023010/	Quick Look
146	G156.2+5.7NW	74.223	52.4174	73.2357	52.339427	79.010107	29.577951	155.48379099	5.80912082	273.883	54147.6530902778	2007-02-16 15:40:27	54148.7558333333	2007-02-17 18:08:24	501075010	50.5468	50	50.5468	50.5468	0	50.5468	2	2	0	2	1	0	0	46.1958	46.1958	95.2599	0	PROCESSED	57537.3885763889	2016-05-29 09:19:33	54695	2008-08-17 00:00:00	54153.2775	2007-02-22 06:39:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011235	G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target.	GALACTIC DIFFUSE EMISSION	5	C	ROBERT PETRE		USA	1	AO1	A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501075010/	Quick Look
147	SNR G93.3+6.9 CENTER	312.9805	55.373	312.634427	55.183848	352.046818	66.979241	93.25121789	6.97467523	40.9208	53905.2215509259	2006-06-19 05:19:02	53905.6480787037	2006-06-19 15:33:14	501079010	20.5372	20	20.5452	20.5452	20.5452	20.5372	2	2	2	2	1	0	0	20.008	20.008	36.8159	0	PROCESSED	57534.7200347222	2016-05-26 17:16:51	54401	2007-10-28 00:00:00	53926.792962963	2006-07-10 19:01:52	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501079010/	Quick Look
148	SNR G93.3+6.9 S1	313.1088	55.5284	312.76382	55.338789	352.457306	67.040407	93.41888838	7.01647125	40.6424	53905.6486458333	2006-06-19 15:34:03	53905.9696064815	2006-06-19 23:16:14	501080010	15.875	15	15.875	15.8902	15.891	15.883	1	1	1	1	1	0	0	12.7588	12.7588	27.7279	1	PROCESSED	57534.7111805556	2016-05-26 17:04:06	54401	2007-10-28 00:00:00	53926.199212963	2006-07-10 04:46:52	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501080010/	Quick Look
149	SNR G93.3+6.9 S4	312.7524	55.2472	312.406034	55.058863	351.58456	66.978212	93.07038921	6.99620044	39.4008	53906.7271296296	2006-06-20 17:27:04	53907.0550347222	2006-06-21 01:19:15	501083010	15.3662	15	15.3662	15.3662	15.3662	15.3662	2	2	2	2	1	0	0	14.4694	14.4694	28.3279	1	PROCESSED	57534.7341550926	2016-05-26 17:37:11	54401	2007-10-28 00:00:00	53926.117662037	2006-07-10 02:49:26	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501083010/	Quick Look
150	X1630-472	248.5405	-47.3458	247.619879	-47.241836	254.106265	-25.080324	336.96147829	0.2654214	120.3	53817.4260300926	2006-03-23 10:13:29	53817.9313425926	2006-03-23 22:21:08	400010060	21.6541	200	21.6621	21.6541	21.6541	21.6541	2	1	2	2	1	0	0	22.7619	22.7619	43.6559	1	PROCESSED	57533.3033796296	2016-05-25 07:16:52	54247	2007-05-27 00:00:00	54042.1043287037	2006-11-03 02:30:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001058	We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		JAP	0	SWG-TOO	FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010060/	Quick Look
151	COMET_8P_TUTTLE-P1-9	28.3593	5.9969	27.705197	5.751157	28.487543	-5.283181	149.56477648	-53.63811023	248.4989	54471.0491666667	2008-01-06 01:10:48	54471.1154050926	2008-01-06 02:46:11	502062090	3.2186	3.2	3.2186	3.2186	0	3.2186	1	1	0	1	1	0	0	2.439	2.439	5.664	0	PROCESSED	57541.0088425926	2016-06-02 00:12:44	54908	2009-03-18 00:00:00	54542.2348611111	2008-03-17 05:38:12	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062090/	Quick Look
152	COMET_8P_TUTTLE-P1-11	28.4619	5.5053	27.808889	5.259792	28.409931	-5.779338	150.05998726	-54.04643055	248.5015	54471.1825	2008-01-06 04:22:48	54471.2487384259	2008-01-06 05:58:11	502062110	3.219	3.2	3.219	3.219	0	3.219	1	1	0	1	1	0	0	2.0356	2.0356	5.688	0	PROCESSED	57541.2689699074	2016-06-02 06:27:19	54908	2009-03-18 00:00:00	54542.2871990741	2008-03-17 06:53:34	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062110/	Quick Look
153	COMET_8P_TUTTLE-P1-12	28.5143	5.2526	27.861852	5.007213	28.369731	-6.034275	150.31791041	-54.25562458	248.4993	54471.2491666667	2008-01-06 05:58:48	54471.3154050926	2008-01-06 07:34:11	502062120	3.2196	3.2	3.2196	3.2196	0	3.2196	1	1	0	1	1	0	0	2.162	2.162	5.696	0	PROCESSED	57541.268587963	2016-06-02 06:26:46	54908	2009-03-18 00:00:00	54542.261400463	2008-03-17 06:16:25	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062120/	Quick Look
154	COMET_8P_TUTTLE-P2_03	39.7649	-35.9737	39.253357	-36.188553	21.195094	-48.151161	240.80897167	-65.5250468	257.7596	54490.2964351852	2008-01-25 07:06:52	54490.4293287037	2008-01-25 10:18:14	502063030	6.0389	6	6.0549	6.0389	0	6.0549	2	2	0	2	1	0	0	6.6011	6.6011	11.4639	0	PROCESSED	57541.3810532407	2016-06-02 09:08:43	54912	2009-03-22 00:00:00	54546.1040046296	2008-03-21 02:29:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063030/	Quick Look
155	COMET_8P_TUTTLE-P2_04	39.8249	-36.1145	39.31419	-36.329166	21.162848	-48.298537	241.11100541	-65.44459708	257.8515	54490.4297106482	2008-01-25 10:18:47	54490.562662037	2008-01-25 13:30:14	502063040	6.6876	6.7	6.6876	6.7191	0	6.6876	1	1	0	1	1	0	0	7.3887	7.3887	11.4799	0	PROCESSED	57541.3859375	2016-06-02 09:15:45	54912	2009-03-22 00:00:00	54546.1129513889	2008-03-21 02:42:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063040/	Quick Look
156	COMET_8P_TUTTLE-P2_05	39.8852	-36.2545	39.375324	-36.468978	21.131041	-48.445251	241.40935004	-65.36366996	257.9439	54490.5630439815	2008-01-25 13:30:47	54490.6959953704	2008-01-25 16:42:14	502063050	6.6974	6.7	6.6976	6.6976	0	6.6974	1	1	0	1	1	0	0	6.1619	6.1619	11.4799	0	PROCESSED	57541.3887847222	2016-06-02 09:19:51	54912	2009-03-22 00:00:00	54546.126712963	2008-03-21 03:02:28	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063050/	Quick Look
157	COMET_8P_TUTTLE-P2_10	40.1849	-36.9375	39.679167	-37.15104	20.975454	-49.162155	242.83840601	-64.95862507	253.4045	54491.2297106482	2008-01-26 05:30:47	54491.362662037	2008-01-26 08:42:14	502063100	5.7304	5	5.7384	5.7384	0	5.7304	2	2	0	2	1	0	0	6.2091	6.2091	11.4739	0	PROCESSED	57541.4028472222	2016-06-02 09:40:06	54912	2009-03-22 00:00:00	54546.1949884259	2008-03-21 04:40:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063100/	Quick Look
158	COMET_8P_TUTTLE-P2_12	40.3045	-37.2045	39.80042	-37.417664	20.914316	-49.442898	243.38522043	-64.79583615	253.5926	54491.4963773148	2008-01-26 11:54:47	54491.6293287037	2008-01-26 15:06:14	502063120	6.6082	6.7	6.6082	6.6082	0	6.6242	1	1	0	1	1	0	0	6.4698	6.4698	11.4799	0	PROCESSED	57541.4099884259	2016-06-02 09:50:23	54912	2009-03-22 00:00:00	54546.2619675926	2008-03-21 06:17:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063120/	Quick Look
159	COMET_8P_TUTTLE-P2_14	40.423	-37.4668	39.920562	-37.679591	20.853678	-49.718838	243.91615364	-64.63380941	253.7796	54491.7630439815	2008-01-26 18:18:47	54491.8959953704	2008-01-26 21:30:14	502063140	6.5627	6.7	6.5627	6.5867	0	6.5627	1	1	0	1	1	0	0	3.833	3.833	11.4799	0	PROCESSED	57541.4134143518	2016-06-02 09:55:19	54912	2009-03-22 00:00:00	54546.2568518518	2008-03-21 06:09:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063140/	Quick Look
160	COMET_8P_TUTTLE-P2_15	40.4836	-37.5961	39.981983	-37.8087	20.825541	-49.855587	244.17467378	-64.55180166	253.8725	54491.8963773148	2008-01-26 21:30:47	54492.0293287037	2008-01-27 00:42:14	502063150	3.4717	4	3.4797	3.4717	0	3.4877	1	1	0	1	1	0	0	2.3461	2.3461	11.4799	1	PROCESSED	57541.4238657407	2016-06-02 10:10:22	54912	2009-03-22 00:00:00	54546.2153587963	2008-03-21 05:10:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063150/	Quick Look
161	G332.5-5.6 CENTER	250.7335	-54.5135	249.725841	-54.419293	256.94436	-31.940577	332.53119736	-5.54004522	262.5079	54330.694224537	2007-08-18 16:39:41	54331.8731944444	2007-08-19 20:57:24	502066010	70.1488	80	70.1488	70.1488	0	70.1568	1	1	0	1	1	0	0	71.4907	71.4907	101.8399	0	PROCESSED	57539.62875	2016-05-31 15:05:24	54721	2008-09-12 00:00:00	54354.4910300926	2007-09-11 11:47:05	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021216	We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova.	GALACTIC DIFFUSE EMISSION	5	B	STEPHEN REYNOLDS		USA	2	AO2	G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502066010/	Quick Look
162	B1920+10(1)	293.0298	10.9618	292.438521	10.854204	297.004439	32.268855	47.34140504	-3.87470613	252.2888	54772.350462963	2008-11-02 08:24:40	54774.137662037	2008-11-04 03:18:14	503090010	73.6033	70	73.6124	73.6033	0	73.6113	2	2	0	2	1	0	0	66.6682	66.6682	154.4039	3	PROCESSED	57544.3491550926	2016-06-05 08:22:47	55154	2009-11-19 00:00:00	54788.4472337963	2008-11-18 10:44:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031204	A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps.	GALACTIC DIFFUSE EMISSION	5	C	ZDENKA MISANOVIC		USA	3	AO3	STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503090010/	Quick Look
163	HESS J1023-575	155.5616	-57.7533	155.104313	-57.500238	195.408014	-59.737737	284.06754503	-0.45248582	284.3289	54617.1411458333	2008-05-31 03:23:15	54617.4515509259	2008-05-31 10:50:14	503092010	13.826	10	13.826	13.826	0	13.826	1	1	0	1	1	0	0	11.0573	11.0573	26.8159	1	PROCESSED	57542.6773842593	2016-06-03 16:15:26	54999	2009-06-17 00:00:00	54633.6961458333	2008-06-16 16:42:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031207	We propose to search the neighborhood of two extended TeV sources to determine if there are X-ray sources that are potentially pulsar wind nebulae powering them. One source is near the colliding wind binary RCW 49, which has been suggested as the accelerator, and would therefore represent a new source class if there is no other plausible accelerator in the neighborhood. The other is a very bright source first detected by MILAGRO in the Galactic plane, which has been shown to be a large, extended source by HESS. While there is in each case a proposed X-ray counterpart, only a part of each nebula has been imaged in hard X-rays, and so it is unknown if there are other, more plausible counterparts.	GALACTIC DIFFUSE EMISSION	5	B	MALLORY ROBERTS		USA	3	AO3	SEARCHING FOR X-RAY COUNTERPARTS OF TWO GALACTIC TEV SOURCES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503092010/	Quick Look
164	GCL2	264.8888	-28.9255	264.094972	-28.898771	265.497098	-5.564174	359.31035513	1.13376438	106.9569	54905.2789467593	2009-03-15 06:41:41	54905.9169444444	2009-03-15 22:00:24	503100010	25.7179	25	25.7179	25.7179	0	25.7179	1	1	0	1	1	0	0	24.146	24.146	55.1199	1	PROCESSED	57545.8116666667	2016-06-06 19:28:48	55329	2010-05-13 00:00:00	54917.3744675926	2009-03-27 08:59:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031234	We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity.	GALACTIC DIFFUSE EMISSION	5	B	FARHAD YUSEF-ZADEH		USA	3	AO3	A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503100010/	Quick Look
165	GCL3	265.2728	-28.8569	264.479303	-28.83203	265.832305	-5.484097	359.5469331	0.88519	106.9023	54906.6133912037	2009-03-16 14:43:17	54907.3252777778	2009-03-17 07:48:24	503101010	33.8911	25	33.8991	33.8991	0	33.8911	2	2	0	2	1	0	0	30.8309	30.8309	61.4979	0	PROCESSED	57545.8349652778	2016-06-06 20:02:21	55329	2010-05-13 00:00:00	54917.3115393518	2009-03-27 07:28:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031234	We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity.	GALACTIC DIFFUSE EMISSION	5	B	FARHAD YUSEF-ZADEH		USA	3	AO3	A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503101010/	Quick Look
166	NEP #2	270.0521	66.5655	270.053494	66.565223	19.553337	89.984047	96.38949161	29.79071779	194.6438	55172.5015162037	2009-12-07 12:02:11	55173.6411342593	2009-12-08 15:23:14	504072010	48.6977	50	48.6977	48.6977	0	48.6977	2	2	0	2	1	0	0	38.4582	38.4582	98.456	1	PROCESSED	57549.730775463	2016-06-10 17:32:19	54922	2009-04-01 00:00:00	55190.01875	2009-12-25 00:27:00	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041101	We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe.	GALACTIC DIFFUSE EMISSION	5	A	STEVEN SNOWDEN		USA	4	AO4	OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504072010/	Quick Look
167	HESS J1809-193A	273.0012	-19.0034	272.264617	-19.016192	272.836277	4.407781	11.60922783	-0.25253702	270.0939	55083.2051967593	2009-09-09 04:55:29	55084.4828009259	2009-09-10 11:35:14	504077010	52.1109	50	52.1745	52.1908	0	52.1109	3	3	0	3	1	0	0	44.109	44.109	110.376	1	PROCESSED	57548.5474189815	2016-06-09 13:08:17	55475	2010-10-06 00:00:00	55109.4207638889	2009-10-05 10:05:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041303	We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background.	GALACTIC DIFFUSE EMISSION	5	A	OLEG KARGALTSEV		USA	4	AO4	CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504077010/	Quick Look
168	G156.2+5.7 (S)	74.9073	51.0204	73.935792	50.94566	79.297666	28.139899	156.85145441	5.28162006	265.6871	55259.9832407407	2010-03-04 23:35:52	55261.1495833333	2010-03-06 03:35:24	504080010	52.6413	50	52.6493	52.6413	0	52.6493	2	2	0	2	1	0	0	47.6566	47.6566	100.7578	0	PROCESSED	57550.7899189815	2016-06-11 18:57:29	55689	2011-05-08 00:00:00	55323.2891666667	2010-05-07 06:56:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041311	The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks.	GALACTIC DIFFUSE EMISSION	5	C	SATORU KATSUDA		USA	4	AO4	REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504080010/	Quick Look
169	330.2+1.0	240.2338	-51.5878	239.290441	-51.447552	249.060918	-30.286354	330.14022152	0.98429318	285.0004	55081.4851273148	2009-09-07 11:38:35	55082.1453472222	2009-09-08 03:29:18	504083020	30.8896	30	30.8896	30.8896	0	30.8971	2	2	0	2	1	0	0	27.0764	27.0764	57.0379	0	PROCESSED	57548.4451736111	2016-06-09 10:41:03	55458	2010-09-19 00:00:00	55092.1620949074	2009-09-18 03:53:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041312	Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity.	GALACTIC DIFFUSE EMISSION	5	B	GLENN ALLEN		USA	4	AO4	MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504083020/	Quick Look
170	NGC 6888	302.9954	38.2382	302.538596	38.087534	320.045193	56.092572	75.36419968	2.38310331	253.873	55139.4126388889	2009-11-04 09:54:12	55141.3127777778	2009-11-06 07:30:24	504085010	77.349	75	77.461	77.349	0	77.461	3	2	0	2	1	0	0	62.1002	62.1002	164.1558	0	PROCESSED	57549.1334837963	2016-06-10 03:12:13	55518	2010-11-18 00:00:00	55152.1455671296	2009-11-17 03:29:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041321	Fast winds from massive stars create large cavities in the surrounding interstellar medium filled with hot gas, known as Wind-Blown Bubbles (WBB). We propose to obtain XIS imaging spectroscopy of the prototype WBB NGC 6888. Thanks to the XIS excellent sensitivity and energy resolution in the soft X-ray band, we will: (i) obtain a high quality CCD spectrum which can be used to constrain the temperature of the hot plasma and the efficiency of thermal conduction across the bubble wall, (ii) determine the spatial distribution and properties of X-ray emitting plasma, (iii) therefore, test and refine shock physics models of bubbles by a direct confrontation of their results with observations.	GALACTIC DIFFUSE EMISSION	5	A	SVETOZAR ZHEKOV		USA	4	AO4	X-RAYS FROM THE PROTOTYPE WIND-BLOWN BUBBLE NGC 6888	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504085010/	Quick Look
171	MRK 421 OFFSET	166.8026	37.7335	166.111285	38.004105	152.017379	29.315723	180.50489089	65.69633084	129.0398	55144.0655092593	2009-11-09 01:34:20	55145.8091087963	2009-11-10 19:25:07	504086010	75.2595	75	75.2675	75.2595	0	75.2675	2	2	0	2	1	0	0	51.94	51.94	150.6288	2	PROCESSED	57549.2648148148	2016-06-10 06:21:20	55542	2010-12-12 00:00:00	55176.2291319444	2009-12-11 05:29:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041324	The OVII, OVIII, and NeIX absorption lines at z~0 have been discovered in the Chandra/XMM spectra of several bright AGNs, but the location of these absorptions has been debated since their discoveries. Here we request Suzaku observations of the soft X-ray background emission in the vicinity of Mrk 421, to conduct a joint analysis of the emission data with the extensive Chandra absorption data. This analysis will naturally yield an effective length of the absorbing/emitting gas. We have performed pilot studies and obtained a scale length of several kpc for the hot absorbing/emitting gas toward LMC X-3 and Mrk 421. The requested Suzaku observations are particular important to check these results and to further test the models we have developed in our study.	GALACTIC DIFFUSE EMISSION	5	B	YANGSEN YAO		USA	4	AO4	A JOINT X-RAY ABSORPTION AND EMISSION STUDY OF THE HOT GAS TOWARD MRK 421	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504086010/	Quick Look
172	0548-70.4	86.9619	-70.4173	87.103378	-70.431737	284.612052	-85.985846	280.90214015	-30.75163284	12.6051	55378.8779861111	2010-07-01 21:04:18	55381.6286689815	2010-07-04 15:05:17	505065010	103.6746	100	103.6746	103.6746	0	103.6746	2	2	0	2	1	0	0	156.9716	156.9716	237.6358	1	PROCESSED	57552.5583912037	2016-06-13 13:24:05	55287	2010-04-01 00:00:00	55434.3854513889	2010-08-26 09:15:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051102	Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors.	GALACTIC DIFFUSE EMISSION	5	B	KAZIMIERZ BORKOWSKI		USA	5	AO5	TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505065010/	Quick Look
173	VELA SNR CB2	130.2058	-44.7742	129.776213	-44.595251	154.639113	-59.522265	263.81853128	-1.77251278	293.5729	55318.5746412037	2010-05-02 13:47:29	55318.9238425926	2010-05-02 22:10:20	505069010	19.3805	20	19.4125	19.4045	0	19.3805	1	1	0	1	1	0	0	18.8298	18.8298	30.1679	0	PROCESSED	57551.3535763889	2016-06-12 08:29:09	55696	2011-05-15 00:00:00	55330.2121643518	2010-05-14 05:05:31	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051304	The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	5	AO5	IRON-RICH EJECTA BULLET IN THE VELA SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505069010/	Quick Look
174	VELA PWN E5	130.8405	-45.4455	130.413883	-45.264192	156.083116	-59.869195	264.62375514	-1.83200273	304.5067	55712.7368402778	2011-05-31 17:41:03	55712.9570601852	2011-05-31 22:58:10	506048010	15.9196	15	15.9196	15.9196	0	15.9436	1	1	0	1	1	0	0	11.9129	11.9129	19.0159	0	PROCESSED	57602.1724305556	2016-08-02 04:08:18	56093	2012-06-15 00:00:00	55726.0610185185	2011-06-14 01:27:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506048010/	Quick Look
175	VELA PWN E7	131.6969	-45.5129	131.268004	-45.328458	157.17001	-59.613979	265.05012769	-1.40367097	303.5042	55713.2300925926	2011-06-01 05:31:20	55713.4688310185	2011-06-01 11:15:07	506050010	13.0454	15	13.0494	13.0454	0	13.0534	1	1	0	1	1	0	0	11.0751	11.0751	20.622	0	PROCESSED	57602.181875	2016-08-02 04:21:54	56093	2012-06-15 00:00:00	55726.0999768518	2011-06-14 02:23:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506050010/	Quick Look
176	G236+38 OFF	149.4117	1.4719	148.767122	1.710754	151.004118	-10.298746	237.07053965	41.11953464	293.1755	55719.6375462963	2011-06-07 15:18:04	55721.2780092593	2011-06-09 06:40:20	506056010	70.8135	70	70.8215	70.8295	0	70.8135	2	2	0	2	1	0	0	64.4444	64.4444	141.7278	0	PROCESSED	57602.2364583333	2016-08-02 05:40:30	56127	2012-07-19 00:00:00	55757.6968518518	2011-07-15 16:43:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061321	Interstellar clouds cast shadows in the soft X-ray background (SXRB). Observations of these shadows enable us to disentangle the various components of the SXRB. Unfortunately, to date, shadowing observations with XMM or Suzaku have only been published for three directions, all in the southern Galactic hemisphere. We propose two new pairs of on- and off-cloud shadowing observations, in order to sample the northern Galactic hemisphere. Our particular goal is to obtain accurate X-ray spectra of the Galactic halo, which we will compare with the predictions of models of galactic fountains and infalling extragalactic material.	GALACTIC DIFFUSE EMISSION	5	B	DAVID HENLEY		USA	6	AO6	UNDERSTANDING THE ORIGIN OF THE GALACTIC HALO USING SHADOWING OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506056010/	Quick Look
177	RX J1713 SOUTHEAST	258.9281	-40.015	258.058505	-39.959445	261.147328	-16.912866	347.36958165	-0.95677146	84	56711.6431018518	2014-02-23 15:26:04	56713.2190046296	2014-02-25 05:15:22	508067010	80.0774	80	80.0854	80.0854	0	80.0774	2	2	0	2	1	0	0	74.9291	74.9291	118.0069	0	PROCESSED	57613.9112152778	2016-08-13 21:52:09	57173	2015-05-31 00:00:00	56806.6951851852	2014-05-29 16:41:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081313	Detecting thermal emission and determining the ambient density are the missing keys to constrain hadronic acceleration in X-ray synchrotron-dominated SNRs. In the prototypical CR accelerator RX J1713.7-3946, X-ray thermal emission has been sought for over a decade, without success. Deep Suzaku observations will constrain either the conditions of the ambient medium in which the SNR is evolving, or the SN progenitor type (core-collapse or thermonuclear) and nucleosynthesis yield.	GALACTIC DIFFUSE EMISSION	5	A	FABIO ACERO		USA	8	AO8	STUDY OF THE THERMAL EMISSION IN THE SYNCHROTRON DOMINATED SNR RX J1713.7-3946	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508067010/	Quick Look
178	MBM36-OFF	238.9304	-1.7878	238.282545	-1.642781	237.109098	18.17526	7.39248129	37.0792042	270.0134	56533.8916319444	2013-08-29 21:23:57	56535.9634606482	2013-08-31 23:07:23	508074010	74.1565	80	74.1645	74.1645	0	74.1565	3	2	0	2	1	0	0	64.2521	64.2521	178.982	1	PROCESSED	57612.4561574074	2016-08-12 10:56:52	56970	2014-11-09 00:00:00	56603.6967476852	2013-11-07 16:43:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081322	We propose the observation of three off-cloud targets near the targets of the Solar Wind Charge Exchange (SWCX) Key Project to study the properties of the Diffuse X-ray Background below 1 keV, with particular focus on the characterization of the Galactic Halo. The Key Project targets are at a distance of a few hundreds pc from the Sun and their high density portions shields about 90% of X-rays at the O VII energy, our proposed targets, instead, shield only about 50% of the Galactic Halo emission. The contrast between on- and off-cloud allows us to disentangle the foreground and background emissions. In particular we will focus on the properties of the galactic halo, which dominates the oxygen background emission.	GALACTIC DIFFUSE EMISSION	5	A	EUGENIO URSINO		USA	8	AO8	PROPERTIES OF THE GALACTIC HALO THROUGH SHADOW OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508074010/	Quick Look
179	HB9-EAST	75.4362	46.2793	74.514835	46.207153	79.087021	23.389602	160.82107477	2.65100841	76.7663	56929.6809722222	2014-09-29 16:20:36	56930.7918518518	2014-09-30 19:00:16	509033010	51.0581	50	51.0581	51.0581	0	51.0581	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.6020949074	2016-08-16 14:27:01	57358	2015-12-02 00:00:00	56986.4031481482	2014-11-25 09:40:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091312	We propose to conduct two pointed observations of the Galactic supernova remnant (SNR) HB9 (G160.9+2.6) with Suzaku. HB9 is a member of the class of Galactic SNRs which are distinguished by their contrasting radio and X-ray morphologies. Prior X-ray observations of HB9 have suggested that the SNR may have a hard component to its X-ray emission, but the true nature of this emission and its origin (a background AGN, intercluster gas associated with the cluster that harbors the AGN or the SNR itself) remains elusive. Our proposed observations will help identify the true nature of the hard emission as well as search for spectral variations (and possible overionization) in the properties of the X-ray emitting plasma associated with the SNR.	GALACTIC DIFFUSE EMISSION	5	A	THOMAS PANNUTI		USA	9	AO9	SUZAKU OBSERVATIONS OF THE GALACTIC SUPERNOVA REMNANT HB9 (G160.9+2.6)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509033010/	Quick Look
180	G93.3+6.9 SE RIM	313.3308	55.275	312.981985	55.084608	352.240038	66.77051	93.30192448	6.7583673	52.5	56812.4202314815	2014-06-04 10:05:08	56814.806412037	2014-06-06 19:21:14	509039010	108.0493	100	108.0493	108.0493	0	108.0493	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.2124074074	2016-08-15 05:05:52	57205	2015-07-02 00:00:00	56835.7633912037	2014-06-27 18:19:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091316	We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN.	GALACTIC DIFFUSE EMISSION	5	C	MICHAEL STAGE		USA	9	AO9	G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509039010/	Quick Look
181	OFF-FIELD3	339.5497	30.5758	338.966926	30.315472	354.778732	35.902508	91.73533627	-24.10496467	65.4693	56819.1115625	2014-06-11 02:40:39	56821.2502199074	2014-06-13 06:00:19	509044010	97.3343	80	97.3343	97.3343	0	97.3343	2	2	0	2	1	0	0	38.618	38.618	77.04	0	PROCESSED	57615.247974537	2016-08-15 05:57:05	56748	2014-04-01 00:00:00	56834.8146527778	2014-06-26 19:33:06	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091321	Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma.	GALACTIC DIFFUSE EMISSION	5	C	ANJALI GUPTA		USA	9	AO9	CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509044010/	Quick Look
182	FERMI_JET_COCOON_3	314.5039	-35.288	313.721159	-35.481827	306.823334	-17.363917	8.28342789	-40.13197139	258.2411	56980.5600694445	2014-11-19 13:26:30	56980.9689583333	2014-11-19 23:15:18	509049010	18.6742	20	18.6742	18.6742	0	18.6742	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7925347222	2016-08-16 19:01:15	57362	2015-12-06 00:00:00	56995.6103240741	2014-12-04 14:38:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091322	The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way.	GALACTIC DIFFUSE EMISSION	5	C	MATTHEW MILLER		USA	9	AO9	OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509049010/	Quick Look
183	FERMI_JET_COCOON_4	313.0188	-30.9125	312.254939	-31.101111	306.880758	-12.815318	13.57103518	-38.16097703	249.0341	56968.206412037	2014-11-07 04:57:14	56968.8473958333	2014-11-07 20:20:15	509050010	21.6767	20	21.6767	21.8127	0	21.8207	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7496412037	2016-08-16 17:59:29	57358	2015-12-02 00:00:00	56982.4333333333	2014-11-21 10:24:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091322	The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way.	GALACTIC DIFFUSE EMISSION	5	C	MATTHEW MILLER		USA	9	AO9	OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509050010/	Quick Look
184	FERMI_JET_COCOON_6	319.6218	-32.8375	318.863263	-33.048426	311.821395	-16.319347	12.30967968	-44.01160773	252.671	56969.3646296296	2014-11-08 08:45:04	56970.0259375	2014-11-09 00:37:21	509052010	21.3583	20	21.3583	21.3583	0	21.3583	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7516782407	2016-08-16 18:02:25	57358	2015-12-02 00:00:00	56982.4382407407	2014-11-21 10:31:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091322	The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way.	GALACTIC DIFFUSE EMISSION	5	C	MATTHEW MILLER		USA	9	AO9	OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509052010/	Quick Look
185	DIFFUSE1B	201.171	8.6653	200.545653	8.925438	196.184358	16.273856	327.54408522	69.93225444	119.3004	57014.7841898148	2014-12-23 18:49:14	57015.2196759259	2014-12-24 05:16:20	509059010	20.7335	20	20.7335	20.7415	0	20.7335	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.558275463	2016-08-17 13:23:55	57475	2016-03-28 00:00:00	57107.4265162037	2015-03-26 10:14:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091324	In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them.	GALACTIC DIFFUSE EMISSION	5	C	JOEL BREGMAN		USA	9	AO9	UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509059010/	Quick Look
186	3C120	68.2993	5.3535	67.634764	5.249056	67.434072	-16.404208	190.3755878	-27.39480435	262.4873	53789.4598726852	2006-02-23 11:02:13	53790.8748958333	2006-02-24 20:59:51	700001030	40.9073	160	40.9073	40.9073	40.9073	40.9073	2	2	2	2	1	0	0	38.4817	38.4817	77.876	2	PROCESSED	57533.073900463	2016-05-25 01:46:25	54247	2007-05-27 00:00:00	54041.5149189815	2006-11-02 12:21:29	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001003	Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	0	SWG	BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001030/	Quick Look
187	MCG-6-30-15	203.9713	-34.2978	203.254904	-34.042659	215.172989	-22.546967	313.28925681	27.67845448	102.4359	53762.928275463	2006-01-27 22:16:43	53765.368275463	2006-01-30 08:50:19	700007030	96.6919	300	96.6919	96.6919	96.6999	96.6999	2	2	2	2	1	0	0	89.8194	89.8194	210.8019	5	PROCESSED	57532.8529861111	2016-05-24 20:28:18	54247	2007-05-27 00:00:00	54040.8156828704	2006-11-01 19:34:35	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001035	The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales .	EXTRAGALACTIC COMPACT SOURCES	7	A	ANDREW FABIAN		JAP	0	SWG	REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700007030/	Quick Look
188	0836+714	130.267	70.829	129.006808	71.006559	109.318804	50.076677	143.62710847	34.4182022	294.8268	53809.7578125	2006-03-15 18:11:15	53810.5836111111	2006-03-16 14:00:24	700010010	55.6261	50	55.6341	55.6341	55.6261	55.6341	2	2	2	2	1	0	0	47.4058	47.4058	71.3419	1	PROCESSED	57533.2238541667	2016-05-25 05:22:21	54247	2007-05-27 00:00:00	54041.9651851852	2006-11-02 23:09:52	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001061	We propose two 50 ks observations, one for each of two EGRET blazars, 1510-089 (OR -017) and 0836+710 (4C +71.07). Both objects show extremely hard X-ray spectra, with photon indices about 1.3. The blazar 1510-089 ($z = 0.361$) is among a few OVV quasars showing prominent soft X-ray excess. The blazar 0836+710 ($z = 2.172)$ is the brightest X-ray source among the high redshift ($z>2$) quasars, and its very hard X-ray spectrum extends down to soft X-rays. Studying spectral shape and variability in the soft X-ray band relative to variability in the mid X-ray and optical bands can help to reveal nature of the soft X-ray excess of unknown origin, and multifrequency variability studies can provide constraints on the structure of jets on subparsec scales.	EXTRAGALACTIC COMPACT SOURCES	7	A	GREG MADEJSKI		JAP	0	SWG	TESTING THE SHOCK-IN-JET MODEL FOR NONTHERMAL FLARES IN BLAZARS VIA SUZAKU OBSERVATIONS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700010010/	Quick Look
189	SWIFT J0746.3+2548	116.6142	25.8792	115.852151	26.002245	113.853224	4.615293	194.5201067	22.91801121	97.0095	53678.357974537	2005-11-04 08:35:29	53680.5862847222	2005-11-06 14:04:15	700011010	99.4284	100	99.5235	100.4524	99.4284	99.7235	2	2	2	2	1	0	0	87.6995	87.6995	192.472	4	PROCESSED	57527.9575694445	2016-05-19 22:58:54	54247	2007-05-27 00:00:00	54037.5799074074	2006-10-29 13:55:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001087	Recently the BAT gamma-ray detector onboard Swift satellite has discovered very flat hard X-ray sources with photon index ~ 1.5 above 100 keV. The x-ray spectrum obtained with the XRT on Swiftis highly variable on time scales < 90 minutes. This variability and flat continuum spectrum suggests that this source is classified as a blazar. If this association is real, we have a precious chance to obtain spectrum upto several hundred keV in the source frame of the source. This wide range is of particularly importanceto study the blazar spectrum, or the electron distribution.	EXTRAGALACTIC COMPACT SOURCES	7	A	TADAYUKI TAKAHASHI		JAP	0	SWG	SUZAKU OBSERVATION OF A HIGH REDSHIFT BLAZAR RECENTLY DISCOVERED BY THE BAT ON SWIFT		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700011010/	Quick Look
190	BO 375	11.4476	41.6573	10.75946	41.384162	28.671168	33.427051	121.80050832	-21.20204189	232.9596	54135.3691666667	2007-02-04 08:51:36	54135.7592476852	2007-02-04 18:13:19	701028010	12.7798	13	12.7798	12.7798	0	12.7798	1	1	0	1	1	0	0	12.8386	12.8386	33.664	1	PROCESSED	57536.9599189815	2016-05-28 23:02:17	54695	2008-08-17 00:00:00	54151.4930324074	2007-02-20 11:49:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011120	There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	A	ALBERT KONG		USA	1	AO1	PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028010/	Quick Look
191	BO 375	11.4497	41.6556	10.761554	41.382464	28.671878	33.424815	121.80214792	-21.2037783	231.6187	54137.6100810185	2007-02-06 14:38:31	54137.9737731482	2007-02-06 23:22:14	701028020	15.5371	13	15.5371	15.5371	0	15.5371	1	1	0	1	1	0	0	14.942	14.942	31.4159	0	PROCESSED	57537.3176967593	2016-05-29 07:37:29	54695	2008-08-17 00:00:00	54151.4987731482	2007-02-20 11:58:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011120	There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	A	ALBERT KONG		USA	1	AO1	PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028020/	Quick Look
192	BO 375	11.4497	41.6556	10.761554	41.382464	28.671878	33.424815	121.80214792	-21.2037783	231.4176	54142.8248032407	2007-02-11 19:47:43	54143.2167824074	2007-02-12 05:12:10	701028030	15.0878	13	15.0878	15.0878	0	15.0878	2	2	0	2	1	0	0	15.7164	15.7164	33.8379	1	PROCESSED	57537.3535069444	2016-05-29 08:29:03	54695	2008-08-17 00:00:00	54153.1806828704	2007-02-22 04:20:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011120	There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies.	EXTRAGALACTIC COMPACT SOURCES	7	A	ALBERT KONG		USA	1	AO1	PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028030/	Quick Look
193	NGC 3783	174.7611	-37.7364	174.141196	-37.45925	192.677729	-36.170962	287.45850943	22.95048745	293.6402	53910.7726388889	2006-06-24 18:32:36	53912.8571412037	2006-06-26 20:34:17	701033010	75.7193	75	75.7193	75.7193	75.7193	75.7193	2	2	2	2	1	0	0	68.2993	68.2993	180.0237	0	PROCESSED	57534.7899652778	2016-05-26 18:57:33	54401	2007-10-28 00:00:00	53926.8847453704	2006-07-10 21:14:02	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011325	We propose a 75 ksec Suzaku observation of the bright Seyfert 1 NGC 3783. Absorption due to photo-ionized material in the line of sight is well-established in this source, but can lead to degeneracy during modeling: is 3-6 keV continuum curvature due to photo-ionized absorption or a relativistically broad Fe K component? The simultaneous broadband XIS/HXD coverage is needed to define the continuum emission over a wide bandpass and disentangle the various emitting and absorbing components. We can then study the ionized absorber components, establish whether or not broad Fe K emission exists, and constrain reflection components, including the Compton shoulder.	EXTRAGALACTIC COMPACT SOURCES	7	B	ALEX MARKOWITZ		USA	1	AO1	PROBING FE K EMISSION AND IONIZED ABSORPTION IN NGC 3783	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701033010/	Quick Look
194	MRK 273	206.1319	55.8192	205.671114	56.069559	168.560084	59.024421	108.09580624	59.75355315	290.8776	53923.3108333333	2006-07-07 07:27:36	53925.3356481482	2006-07-09 08:03:20	701050010	79.9046	80	79.9126	79.9046	79.9206	79.9206	2	2	2	2	1	0	0	82.8076	82.8076	174.9059	3	PROCESSED	57534.931400463	2016-05-26 22:21:13	54401	2007-10-28 00:00:00	53930.7076851852	2006-07-14 16:59:04	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011341	We wish to take advantage of the unprecedented sensitivity of Suzaku Observatory to very hard X-rays (> 10 keV) to constrain the energy source -- starburst or black-hole driven activity -- in two of the nearest and brightest ultraluminous infrared galaxies, Mrk 273 and F05189-2524. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short timescale variability, another signature of black-hole driven activity. These data will be part of S. Teng's PhD thesis at Maryland.	EXTRAGALACTIC COMPACT SOURCES	7	A	SYLVAIN VEILLEUX		USA	1	AO1	THE DOMINANT ENERGY SOURCE OF ULTRALUMINOUS INFRARED GALAXIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701050010/	Quick Look
195	APM 08279+5255	127.9265	52.7635	126.994318	52.932793	116.239859	32.72128	165.74397918	36.24189551	118.0523	54020.1580902778	2006-10-12 03:47:39	54022.3134143518	2006-10-14 07:31:19	701057010	102.3328	100	102.3408	102.3408	102.3328	102.3408	2	2	2	2	1	0	0	96.0187	96.0187	186.1858	3	PROCESSED	57535.8953125	2016-05-27 21:29:15	54702	2008-08-24 00:00:00	54053.9467013889	2006-11-14 22:43:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011353	Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	1	AO1	VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057010/	Quick Look
196	1ES 1101-232	165.8976	-23.5471	165.286971	-23.277424	177.035323	-27.087344	273.21266184	33.02701002	279.8544	53880.6859606482	2006-05-25 16:27:47	53882.2161921296	2006-05-27 05:11:19	701071010	62.4327	55	62.4407	62.4407	62.4407	62.4327	2	2	2	2	1	0	0	50.1033	50.1033	132.1939	0	PROCESSED	57534.4584027778	2016-05-26 11:00:06	54401	2007-10-28 00:00:00	53927.4165393518	2006-07-11 09:59:49	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011376	Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra.	EXTRAGALACTIC COMPACT SOURCES	7	A	ANITA REIMER		USA	1	AO1	CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701071010/	Quick Look
197	NGC5548	214.4933	25.1285	213.926392	25.358693	201.994196	36.40686	31.9338138	70.49848107	305.6607	54289.4186921296	2007-07-08 10:02:55	54290.1182175926	2007-07-09 02:50:14	702042040	30.6996	30	30.6996	30.6996	0	30.6996	1	1	0	1	1	0	0	28.8279	28.8279	60.4319	1	PROCESSED	57539.1330324074	2016-05-31 03:11:34	54695	2008-08-17 00:00:00	54328.4843402778	2007-08-16 11:37:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021307	We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	2	AO2	NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042040/	Quick Look
198	NGC5548	214.4959	25.1277	213.928994	25.357885	201.997272	36.407089	31.932758	70.49602002	293.6791	54296.5817013889	2007-07-15 13:57:39	54297.4168865741	2007-07-16 10:00:19	702042050	30.0197	30	30.0277	30.0357	0	30.0197	2	2	0	2	1	0	0	26.3004	26.3004	58.971	1	PROCESSED	57539.274849537	2016-05-31 06:35:47	54707	2008-08-29 00:00:00	54340.3894328704	2007-08-28 09:20:47	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021307	We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	2	AO2	NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042050/	Quick Look
199	NGC5548	214.4979	25.1264	213.930994	25.35658	201.999984	36.406639	31.92993093	70.49400067	281.7605	54317.0262268518	2007-08-05 00:37:46	54318.0211111111	2007-08-06 00:30:24	702042080	38.7757	210	38.7837	38.7917	0	38.7757	1	1	0	1	1	0	0	32.6497	32.6497	85.9519	0	PROCESSED	57539.4187037037	2016-05-31 10:02:56	54714	2008-09-05 00:00:00	54347.3528472222	2007-09-04 08:28:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021307	We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	2	AO2	NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042080/	Quick Look
200	FAIRALL 9	20.9481	-58.8141	20.470954	-59.074601	340.57309	-59.156739	295.06951561	-57.81752905	48.1772	54258.155462963	2007-06-07 03:43:52	54260.5766666667	2007-06-09 13:50:24	702043010	167.7983	164	167.7983	167.8063	0	167.8143	2	2	0	2	1	0	0	136.4834	136.4834	209.1758	2	PROCESSED	57538.9238425926	2016-05-30 22:10:20	54773	2008-11-03 00:00:00	54265.5470717593	2007-06-14 13:07:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021313	Recently, deep observations of a number of Seyfert AGN with XMM-Newton and Suzaku have established variable and relativistic iron lines as robust features in roughly half of all deep Seyfert spectra. In these sources, the spin of the black hole can be constrained directly through fits to the relativistic iron line. A sample of excellent spectra from well-chosen AGN will facilitate a better understanding of the innermost regime near to black holes, and make correlations with parameters like radio luminosity, star formation rate, and galaxy and black hole mass possible for the first time. We propose to obtain observations of 4 under-exposed Seyfert AGN with promising evidence for broad lines to robustly constrain their spin parameters.	EXTRAGALACTIC COMPACT SOURCES	7	A	JON MILLER		USA	2	AO2	REVEALING BLACK HOLE SPIN IN RELATIVISTIC SEYFERT AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702043010/	Quick Look
201	NGC 1052	40.2309	-8.2134	39.616406	-8.42693	35.027708	-22.668341	181.91154484	-57.92833515	49.7745	54297.4313888889	2007-07-16 10:21:12	54299.87875	2007-07-18 21:05:24	702058010	100.6691	100	100.6691	100.6691	0	100.6691	2	2	0	2	1	0	0	83.4998	83.4998	211.4278	2	PROCESSED	57539.327037037	2016-05-31 07:50:56	54707	2008-08-29 00:00:00	54339.9136458333	2007-08-27 21:55:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021355	Accretion onto supermassive black holes is thought to play a major role in the production of relativistic jets. Our understanding of jet production remains elusive, however, because we cannot image the accretion flow. Fortunately, the Fe K line offers a direct probe of accretion. As part of a multi-mission monitoring program of the radio loud AGN NGC 1052, we propose two 100 ksec Suzaku observations to obtain best-quality X-ray spectra at two epochs to determine the true continuum shape and thus probe the relativistic iron line, determine line and continuum variability patterns and possibly investigate how the structure of the accretion disk changes when there are jet ejection events. Our aim is to determine what leads supermassive black holes to launch powerful jets.	EXTRAGALACTIC COMPACT SOURCES	7	A	KIMBERLY WEAVER		USA	2	AO2	PROBING THE DISK-JET CONNECTION IN AGN WITH AN INTENSIVE MULTIWAVELENGTH MONITORING CAMPAIGN OF NGC 1052	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702058010/	Quick Look
202	Q1946+7658	296.1546	77.0965	296.596903	76.972833	64.242641	76.919523	109.22346589	23.50098326	3.7704	54294.4255902778	2007-07-13 10:12:51	54294.6432175926	2007-07-13 15:26:14	702060010	13.1636	13	13.1636	13.1636	0	13.1636	1	1	0	1	1	0	0	13.9282	13.9282	18.7759	0	PROCESSED	57539.2591782407	2016-05-31 06:13:13	54706	2008-08-28 00:00:00	54339.4067824074	2007-08-27 09:45:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021361	The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars.	EXTRAGALACTIC COMPACT SOURCES	7	C	GEORGE CHARTAS		USA	2	AO2	AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702060010/	Quick Look
203	Q1334-0033	204.1954	-0.819	203.55335	-0.564423	202.702904	8.620784	326.07775276	59.99926461	306.9566	54295.3551736111	2007-07-14 08:31:27	54295.7084953704	2007-07-14 17:00:14	702067010	13.9621	15	13.9621	13.9621	0	13.9621	1	1	0	1	1	0	0	13.0064	13.0064	30.5199	0	PROCESSED	57539.262337963	2016-05-31 06:17:46	54710	2008-09-01 00:00:00	54340.4777430556	2007-08-28 11:27:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021361	The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars.	EXTRAGALACTIC COMPACT SOURCES	7	C	GEORGE CHARTAS		USA	2	AO2	AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702067010/	Quick Look
204	Q1548+0917	237.6002	9.1581	236.997547	9.308492	232.970531	28.527987	18.5566992	44.16075413	106.1242	54513.4560763889	2008-02-17 10:56:45	54514.16	2008-02-18 03:50:24	702068010	32.1133	23	32.1213	32.1213	0	32.1133	1	1	0	1	1	0	0	29.4756	29.4756	60.8159	0	PROCESSED	57541.5745601852	2016-06-02 13:47:22	54889	2009-02-27 00:00:00	54522.1462731482	2008-02-26 03:30:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021361	The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars.	EXTRAGALACTIC COMPACT SOURCES	7	C	GEORGE CHARTAS		USA	2	AO2	AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702068010/	Quick Look
205	MRK 417	162.3659	22.9016	161.688757	23.166381	154.921054	14.241178	214.84390845	62.11471123	281.9359	54238.6593402778	2007-05-18 15:49:27	54239.5730555556	2007-05-19 13:45:12	702078010	41.5066	40	41.5066	41.5066	0	41.5066	2	2	0	2	1	0	0	39.3385	39.3385	78.9239	0	PROCESSED	57538.6952662037	2016-05-30 16:41:11	54695	2008-08-17 00:00:00	54245.0002430556	2007-05-25 00:00:21	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021374	Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702078010/	Quick Look
206	NGC 1142	43.7827	-0.1295	43.142852	-0.331581	41.283841	-16.101856	175.79604248	-49.86350093	73.9096	54302.4506481482	2007-07-21 10:48:56	54303.4308333333	2007-07-22 10:20:24	702079010	40.5697	40	40.5697	40.5697	0	40.5697	2	2	0	2	1	0	0	36.5404	36.5404	84.6799	1	PROCESSED	57539.2980902778	2016-05-31 07:09:15	54706	2008-08-28 00:00:00	54339.1106828704	2007-08-27 02:39:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021374	Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702079010/	Quick Look
207	MCG +04-48-002	307.1488	25.8021	306.615298	25.635019	318.241154	43.22286	67.06317106	-7.53431612	93.9583	54208.4668634259	2007-04-18 11:12:17	54209.4134143518	2007-04-19 09:55:19	702081010	41.2988	40	41.3068	41.2988	0	41.3068	2	2	0	2	1	0	0	37.7466	37.7466	81.7699	2	PROCESSED	57538.398275463	2016-05-30 09:33:31	54695	2008-08-17 00:00:00	54217.0231712963	2007-04-27 00:33:22	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021374	Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702081010/	Quick Look
208	TYPE2AGN	216.4026	35.2819	215.878545	35.506676	198.09088	46.269263	60.85487771	68.34395808	307.3753	54292.1781712963	2007-07-11 04:16:34	54292.6183333333	2007-07-11 14:50:24	702090010	19.8387	19	19.8467	19.8547	0	19.8387	2	2	0	2	1	0	0	20.87	20.87	38.0159	0	PROCESSED	57539.1533912037	2016-05-31 03:40:53	54706	2008-08-28 00:00:00	54339.0120833333	2007-08-27 00:17:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021376	We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs.	EXTRAGALACTIC COMPACT SOURCES	7	C	CHRISTINE JONES		USA	2	AO2	OBSCURED AGN AND XBONGS IN BOOTES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702090010/	Quick Look
209	NGC3227	155.8768	19.8688	155.194236	20.122176	150.387557	9.143202	216.98485011	55.4460253	111.8565	54790.7083333333	2008-11-20 17:00:00	54792.374525463	2008-11-22 08:59:19	703022040	64.5679	50	64.5759	64.5679	0	64.5759	2	2	0	2	1	0	0	46.622	46.622	143.9478	1	PROCESSED	57544.506412037	2016-06-05 12:09:14	54557	2008-04-01 00:00:00	54812.4380324074	2008-12-12 10:30:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031013	We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	3	AO3	NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022040/	Quick Look
210	NGC3227	155.8768	19.8687	155.194236	20.122076	150.387594	9.143109	216.98501654	55.44599229	109.926	54802.6028125	2008-12-02 14:28:03	54803.7231365741	2008-12-03 17:21:19	703022060	51.4105	50	51.4105	51.4105	0	51.4105	2	2	0	2	1	0	0	39.6836	39.6836	96.7818	1	PROCESSED	57544.6321875	2016-06-05 15:10:21	54557	2008-04-01 00:00:00	54812.4432407407	2008-12-12 10:38:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031013	We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	3	AO3	NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022060/	Quick Look
211	SN 2006JD	120.5331	0.8102	119.888824	0.950282	122.553341	-19.245849	220.45612728	16.05834455	284.354	54578.4377777778	2008-04-22 10:30:24	54579.6807175926	2008-04-23 16:20:14	703026010	54.1968	50	54.2048	54.1968	0	54.2048	2	2	0	2	1	0	0	52.0488	52.0488	107.3398	1	PROCESSED	57542.379837963	2016-06-03 09:06:58	54957	2009-05-06 00:00:00	54588.1523611111	2008-05-02 03:39:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031241	Supernovae (SNe) 2005kd and 2006jd are some of the brightest SNe ever detected in X-rays. The high X-ray luminosities (>E41 erg/s) are the results of the SN shock interacting with dense material in the environment of the SNe. We propose one Suzaku observation of each SN to obtain high-quality spectra that will be used to measure the temperature of the forward and reverse shock and to establish the rate of decline in comparison with existing Swift, Chandra and XMM-Newton data. The data will further be used to measure the circumstellar matter density and mass-loss rate of the progenitors to probe the nature of the SN progenitors. Our science objectives rely on Suzaku's uniqueness, i.e. the large collecting area, good spectral resolution, and the high sensitivity in the hard X-ray band.	EXTRAGALACTIC COMPACT SOURCES	7	B	STEFAN IMMLER		USA	3	AO3	SUZAKU OBSERVATIONS OF X-RAY BRIGHT SUPERNOVAE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703026010/	Quick Look
212	ESO 103- G 035	279.5941	-65.4238	278.351287	-65.467222	275.354112	-42.161198	329.78379096	-23.17817546	291.5832	54761.6331597222	2008-10-22 15:11:45	54764.1717476852	2008-10-25 04:07:19	703031010	91.442	80	91.442	91.45	0	91.45	2	2	0	2	1	0	0	81.0096	81.0096	219.282	2	PROCESSED	57544.3339467593	2016-06-05 08:00:53	55148	2009-11-13 00:00:00	54782.4220023148	2008-11-12 10:07:41	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031322	X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s.	EXTRAGALACTIC COMPACT SOURCES	7	B	VALENTINA BRAITO		USA	3	AO3	THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703031010/	Quick Look
213	Q0551-3637	88.2027	-36.6207	87.768974	-36.630505	87.117827	-60.044705	242.37463259	-26.91966553	321.5977	54600.5596643518	2008-05-14 13:25:55	54601.2044444444	2008-05-15 04:54:24	703036020	21.6143	22	21.6143	21.6143	0	21.6183	2	2	0	2	1	0	0	18.2831	18.2831	55.684	1	PROCESSED	57542.5389236111	2016-06-03 12:56:03	54979	2009-05-28 00:00:00	54613.0157060185	2008-05-27 00:22:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031334	Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	3	AO3	A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703036020/	Quick Look
214	Q0329-385	52.7815	-38.4067	52.316664	-38.576045	34.470474	-54.910107	241.941352	-54.89845774	23.7676	54633.4249421296	2008-06-16 10:11:55	54634.1898611111	2008-06-17 04:33:24	703038010	30.203	29	30.219	30.203	0	30.219	2	2	0	2	1	0	0	25.2925	25.2925	66.082	1	PROCESSED	57542.8370601852	2016-06-03 20:05:22	55010	2009-06-28 00:00:00	54644.1762615741	2008-06-27 04:13:49	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031334	Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	3	AO3	A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703038010/	Quick Look
215	ESO 548-G081	55.4927	-21.1949	54.941134	-21.353755	46.730142	-39.596754	213.74761618	-50.8353425	69.3236	55046.3350462963	2009-08-03 08:02:28	55047.1946064815	2009-08-04 04:40:14	704026010	39.4112	40	39.4192	39.4192	0	39.4112	2	2	0	2	1	0	0	36.1429	36.1429	74.2599	0	PROCESSED	57548.0531481482	2016-06-09 01:16:32	55427	2010-08-19 00:00:00	55060.8071875	2009-08-17 19:22:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041402	The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples.	EXTRAGALACTIC COMPACT SOURCES	7	B	LISA WINTER		USA	4	AO4	SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704026010/	Quick Look
216	MCG +04-22-042	140.9461	22.9693	140.230202	23.184366	136.125191	7.311314	205.9821846	43.11036681	106.3587	55157.3309259259	2009-11-22 07:56:32	55158.2634143518	2009-11-23 06:19:19	704028010	40.962	40	40.994	40.962	0	40.986	1	1	0	1	1	0	0	35.8969	35.8969	80.5599	0	PROCESSED	57549.5187384259	2016-06-10 12:26:59	55542	2010-12-12 00:00:00	55176.1858101852	2009-12-11 04:27:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041402	The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples.	EXTRAGALACTIC COMPACT SOURCES	7	B	LISA WINTER		USA	4	AO4	SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704028010/	Quick Look
217	1H0323+342	51.1507	34.2411	50.363828	34.065013	57.518057	15.07869	155.67406743	-18.71640786	76.7168	55038.1604513889	2009-07-26 03:51:03	55040.2084722222	2009-07-28 05:00:12	704034010	84.0884	80	84.0884	84.2404	0	84.3524	2	2	0	2	1	0	0	74.2979	74.2979	176.9379	0	PROCESSED	57548.0010532407	2016-06-09 00:01:31	55419	2010-08-11 00:00:00	55050.8162847222	2009-08-07 19:35:27	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041408	Recent radio observations reveal blazar-like properties in some radio-loud narrow line Seyfert-1 AGNs. 1H0323+342, classified as this class of AGNs, shows prominent hard X-ray emission with a hard photon index. Since the spectrum in hard X-ray is reminiscent of blazar, its X-ray spectrum seems to have different components originated from disk and jet. Thanks to sensitive X-ray detectors extending to the hard X-ray band, Suzaku observation is expected to resolve a possible multi-component structure in the spectrum. Since beamed radiation from jet is highly variable, spectral temporal behavior is also vital information to distinguish the emission origin. As this source is located relatively nearby (z=0.061), the source is an excellent target to investigate the emission from disk and jet.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASAAKI HAYASHIDA		USA	4	AO4	SUZAKU OBSERVATION OF 1H0323+342: A PECULIAR SEYFERT-1 --PROBING THE DISK AND JET CONNECTION IN AGN--	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704034010/	Quick Look
218	MCG0208	43.0963	-8.5129	42.484335	-8.717227	37.842662	-23.868775	185.55840319	-55.88722126	57.4541	55016.0987037037	2009-07-04 02:22:08	55017.2134722222	2009-07-05 05:07:24	704045010	42.9115	40	42.9435	42.9115	0	42.9195	2	2	0	2	1	0	0	36.7878	36.7878	96.286	5	PROCESSED	57547.7724768518	2016-06-08 18:32:22	55395	2010-07-18 00:00:00	55027.1160532407	2009-07-15 02:47:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041414	We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc.	EXTRAGALACTIC COMPACT SOURCES	7	A	EZEQUIEL TREISTER		USA	4	AO4	THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704045010/	Quick Look
219	SDSS J1352+4239	208.1832	42.6476	207.663098	42.893525	184.337785	49.439251	88.11360974	70.09649039	316.6443	54984.9959375	2009-06-02 23:54:09	54985.7502199074	2009-06-03 18:00:19	704050010	32.0745	30	32.0825	32.0745	0	32.0825	2	2	0	2	1	0	0	29.5021	29.5021	65.1639	0	PROCESSED	57547.4324652778	2016-06-08 10:22:45	55364	2010-06-17 00:00:00	54994.4273032407	2009-06-12 10:15:19	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041422	BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction.	EXTRAGALACTIC COMPACT SOURCES	7	A	XINYU DAI		USA	4	AO4	X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704050010/	Quick Look
220	SDSS J0943+5417	145.8252	54.2751	144.963883	54.504193	127.754031	37.9036	161.23003018	46.41565232	274.2141	54975.5889236111	2009-05-24 14:08:03	54976.3473611111	2009-05-25 08:20:12	704052010	34.2264	30	34.2264	34.2264	0	34.2264	2	2	0	2	1	0	0	32.0591	32.0591	65.5179	2	PROCESSED	57546.6638773148	2016-06-07 15:55:59	55358	2010-06-11 00:00:00	54992.6588888889	2009-06-10 15:48:48	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041422	BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction.	EXTRAGALACTIC COMPACT SOURCES	7	A	XINYU DAI		USA	4	AO4	X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704052010/	Quick Look
221	CEN A S LOBE NO. 2	200.3949	-45.1401	199.658837	-44.878468	217.502785	-33.539168	308.49497877	17.40582221	289.0008	55419.7766087963	2010-08-11 18:38:19	55420.9641087963	2010-08-12 23:08:19	705033010	81.3878	80	81.3958	81.3878	0	81.4038	2	2	0	2	1	0	0	68.1085	68.1085	102.5858	0	PROCESSED	57552.9708564815	2016-06-13 23:18:02	55812	2011-09-08 00:00:00	55445.267662037	2010-09-06 06:25:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051401	We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays).	EXTRAGALACTIC COMPACT SOURCES	7	B	GRZEGORZ MADEJSKI		USA	5	AO5	SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705033010/	Quick Look
222	1RXS J111706.3+20141	169.2749	20.2432	168.614437	20.516401	162.09404	14.35752	225.56577108	67.37465885	120.2309	55510.3081944444	2010-11-10 07:23:48	55511.1543402778	2010-11-11 03:42:15	705036010	34.2125	32	34.2125	34.2125	0	34.2125	2	2	0	2	1	0	0	31.5366	31.5366	73.0979	0	PROCESSED	57554.0402199074	2016-06-15 00:57:55	55903	2011-12-08 00:00:00	55537.0979050926	2010-12-07 02:20:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051402	High frequency peaked BL Lacs are a peculiar subclass of Blazars characterized by non-thermal emission across the whole electromagnetic spectrum. Their spectral energy distributions (SEDs) include two main components: a low-energy component with power peaking in the range from the UV to the X-ray band, and a substantial high-energy component often dominated by gamma-rays. We propose 3 observations (32 ks each) of a selected sample of HBLs to study the behavior of the first component, widely interpreted as synchrotron radiation. First, we will be able to disentangle between different spectral shapes of the synchrotron SED of HBLs. Second, we will use the proposed observations to investigate the properties of the most representative sample of TeV candidate HBLs.	EXTRAGALACTIC COMPACT SOURCES	7	C	FRANCESCO MASSARO		USA	5	AO5	X-RAY CURVED SPECTRA IN HIGH FREQUENCY PEAKED BL LACS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705036010/	Quick Look
223	3C111	64.5838	38.0329	63.747646	37.911608	69.36811	16.396021	161.66828978	-8.81804056	76.1726	55453.9599768518	2010-09-14 23:02:22	55455.7432986111	2010-09-16 17:50:21	705040030	80.3659	80	80.3819	80.3659	0	80.3819	2	2	0	2	1	0	0	70.9533	70.9533	154.0639	2	PROCESSED	57553.468599537	2016-06-14 11:14:47	55835	2011-10-01 00:00:00	55469.3718287037	2010-09-30 08:55:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051412	Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components.	EXTRAGALACTIC COMPACT SOURCES	7	A	RITA SAMBRUNA		USA	5	AO5	PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705040030/	Quick Look
224	MKN 590	33.6477	-0.7713	33.009436	-1.003927	31.140057	-13.460103	163.51612886	-56.94122484	251.1273	55587.0949652778	2011-01-26 02:16:45	55588.2146990741	2011-01-27 05:09:10	705043020	40.9139	150	40.9219	40.9219	0	40.9139	2	2	0	2	1	0	0	37.8699	37.8699	96.7339	1	PROCESSED	57600.7810763889	2016-07-31 18:44:45	55988	2012-03-02 00:00:00	55621.2137731482	2011-03-01 05:07:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051433	We propose a 150 ks Suzaku long-look to study the Compton reflection component, soft excess, ionized emission and possible ionized reflection of the Seyfert 1.2 AGN Mkn 590, which has an unobscured line of sight or "bare nucleus" and as of yet unquantified reflection. We aim to accurately constrain the geometry of the circumnuclear material and determine the ionization states of both the Compton-thin and Compton-thick material surrounding the black hole by studying the origin of the soft excess, determining the likelihood of ionized reflection and accurately measuring the intensity of neutral, H-like and He-like Fe emission lines.	EXTRAGALACTIC COMPACT SOURCES	7	C	ELIZABETH RIVERS		USA	5	AO5	QUANTIFYING THE COMPTON REFLECTION AND IONIZED EMISSION IN MKN 590	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705043020/	Quick Look
225	NGC 4945	196.3636	-49.4659	195.633608	-49.198211	217.017818	-38.639251	305.27160994	13.34216317	120.2557	55590.0873842593	2011-01-29 02:05:50	55591.1182175926	2011-01-30 02:50:14	705047050	46.1076	40	46.1076	46.1076	0	46.1076	2	2	0	2	1	0	0	54.0907	54.0907	89.0518	0	PROCESSED	57600.8100810185	2016-07-31 19:26:31	55969	2012-02-12 00:00:00	55602.2238194445	2011-02-10 05:22:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051442	We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval.	EXTRAGALACTIC COMPACT SOURCES	7	B	GUIDO RISALITI		USA	5	AO5	HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047050/	Quick Look
226	SWIFTJ2344.6-424322	356.1059	-42.7624	355.44614	-43.040118	336.666972	-37.094539	339.65324523	-69.27134863	225.0657	55505.2812731482	2010-11-05 06:45:02	55506.5570601852	2010-11-06 13:22:10	705049010	61.7416	60	61.7416	61.7416	0	61.7416	2	2	0	2	1	0	0	50.3941	50.3941	110.2118	1	PROCESSED	57553.9985532407	2016-06-14 23:57:55	55885	2011-11-20 00:00:00	55518.3162847222	2010-11-18 07:35:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051443	We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec.	EXTRAGALACTIC COMPACT SOURCES	7	C	WAYNE BAUMGARTNER		USA	5	AO5	SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705049010/	Quick Look
227	SMC X-1	19.2724	-73.4484	18.941012	-73.711562	312.330249	-66.473862	300.41553375	-43.55429702	25.8573	55691.0197337963	2011-05-10 00:28:25	55691.4064814815	2011-05-10 09:45:20	706030040	17.9054	18	17.9214	17.9214	0	17.9054	1	1	0	1	1	0	0	16.8143	16.8143	33.4079	0	PROCESSED	57601.9922222222	2016-08-01 23:48:48	56068	2012-05-21 00:00:00	55701.1543981482	2011-05-20 03:42:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030040/	Quick Look
228	SMC X-1	19.2675	-73.4407	18.935881	-73.70387	312.347206	-66.469935	300.41598527	-43.56211574	204.2035	55875.0768055556	2011-11-10 01:50:36	55875.6182291667	2011-11-10 14:50:15	706030080	19.8598	18	19.8881	19.8961	0	19.8598	2	2	0	1	1	0	0	19.2508	19.2508	46.772	0	PROCESSED	57603.7203587963	2016-08-03 17:17:19	56260	2012-11-29 00:00:00	55890.6941203704	2011-11-25 16:39:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030080/	Quick Look
229	SMC X-1	19.2681	-73.4483	18.936643	-73.711469	312.329443	-66.472676	300.41718915	-43.55456404	342.3682	56005.2598611111	2012-03-19 06:14:12	56005.8452546296	2012-03-19 20:17:10	706030100	18.5821	18	18.6263	18.6343	0	18.5821	2	2	0	1	1	0	0	20.3061	20.3061	50.5719	0	PROCESSED	57604.9618055556	2016-08-04 23:05:00	56399	2013-04-17 00:00:00	56022.2021296296	2012-04-05 04:51:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030100/	Quick Look
230	III ZW 2	2.6244	10.9839	1.981573	10.705729	6.801457	9.029508	106.97577765	-50.61513425	67.4163	55726.9877893518	2011-06-14 23:42:25	55728.9792708333	2011-06-16 23:30:09	706031010	81.466	80	81.466	81.466	0	81.466	2	2	0	2	1	0	0	74.3629	74.3629	172.0397	3	PROCESSED	57602.3450925926	2016-08-02 08:16:56	56127	2012-07-19 00:00:00	55757.7040046296	2011-07-15 16:53:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061411	Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects.	EXTRAGALACTIC COMPACT SOURCES	7	A	MASAAKI HAYASHIDA		USA	6	AO6	SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706031010/	Quick Look
231	ESO 323-G077	196.6073	-40.4236	195.900559	-40.156267	212.090645	-30.55227	306.0162391	22.35835315	295.8925	55762.647337963	2011-07-20 15:32:10	55763.4168287037	2011-07-21 10:00:14	706033010	44.1222	40	44.1222	44.1222	0	44.1222	2	2	0	2	1	0	0	40.9258	40.9258	66.4819	0	PROCESSED	57602.6188310185	2016-08-02 14:51:07	56212	2012-10-12 00:00:00	55845.2395949074	2011-10-11 05:45:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061411	Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects.	EXTRAGALACTIC COMPACT SOURCES	7	B	MASAAKI HAYASHIDA		USA	6	AO6	SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706033010/	Quick Look
232	1622-297	246.5282	-29.8629	245.741591	-29.750241	249.573082	-8.070344	348.81494865	13.309894	287.0011	55828.8879166667	2011-09-24 21:18:36	55829.1800810185	2011-09-25 04:19:19	706044010	8.7781	10	8.7781	8.7781	0	8.7781	2	2	0	2	1	0	0	8.7513	8.7513	25.198	0	PROCESSED	57603.2321064815	2016-08-03 05:34:14	56236	2012-11-05 00:00:00	55868.9351851852	2011-11-03 22:26:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061601	We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	6	AO6	EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706044010/	Quick Look
233	4C38.41	248.824	38.1186	248.386993	38.220121	236.373082	59.10929	61.06470824	42.32788618	255.0463	55829.1891666667	2011-09-25 04:32:24	55829.4148032407	2011-09-25 09:57:19	706045010	8.9239	10	8.9319	8.9319	0	8.9239	1	1	0	1	1	0	0	9.5353	9.5353	19.4719	0	PROCESSED	57603.2349305556	2016-08-03 05:38:18	56225	2012-10-25 00:00:00	55875.6235185185	2011-11-10 14:57:52	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061601	We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	6	AO6	EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706045010/	Quick Look
234	HOLMBERG IX X-1	149.4435	69.0486	148.425456	69.287009	119.776016	51.672601	141.95726659	41.07139178	311.5635	56030.7575810185	2012-04-13 18:10:55	56034.6807175926	2012-04-17 16:20:14	707019010	182.5274	500	182.5274	182.5274	0	182.5274	2	2	0	2	1	0	0	208.6236	208.6236	338.9339	3	PROCESSED	57605.2861342593	2016-08-05 06:52:02	56018	2012-04-01 00:00:00	56044.4614699074	2012-04-27 11:04:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071251	Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy.	EXTRAGALACTIC COMPACT SOURCES	7	A	JON MILLER		USA	7	AO7	A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019010/	Quick Look
235	HOLMBERG IX X-1	149.4877	69.0751	148.469613	69.31362	119.77363	51.703415	141.9165022	41.0686989	124.501	56221.770162037	2012-10-21 18:29:02	56224.1252083333	2012-10-24 03:00:18	707019020	107.4958	320	107.4958	107.4958	0	107.4958	2	2	0	2	1	0	0	106.8673	106.8673	203.4479	1	PROCESSED	57607.8555324074	2016-08-07 20:31:58	56018	2012-04-01 00:00:00	56330.5864930556	2013-02-07 14:04:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071251	Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy.	EXTRAGALACTIC COMPACT SOURCES	7	A	JON MILLER		USA	7	AO7	A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019020/	Quick Look
236	HOLMBERG IX X-1	149.4867	69.0744	148.468616	69.312918	119.773774	51.702635	141.91753226	41.06881922	124.4999	56226.4169097222	2012-10-26 10:00:21	56228.7717708333	2012-10-28 18:31:21	707019040	110.0175	500	110.0383	110.0175	0	110.0175	3	2	0	2	1	0	0	105.7961	105.7961	203.426	2	PROCESSED	57607.8756018518	2016-08-07 21:00:52	56018	2012-04-01 00:00:00	56240.5502430556	2012-11-09 13:12:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071251	Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy.	EXTRAGALACTIC COMPACT SOURCES	7	A	JON MILLER		USA	7	AO7	A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707019040/	Quick Look
237	NGC 4151	182.642	39.4132	182.010684	39.69131	164.095796	36.629182	155.04475012	75.06022062	134.3454	56242.8428472222	2012-11-11 20:13:42	56245.9599537037	2012-11-14 23:02:20	707024010	150.2669	150	150.2829	150.2669	0	150.2829	2	2	0	2	1	0	0	150.5465	150.5465	269.2897	4	PROCESSED	57608.0679861111	2016-08-08 01:37:54	56702	2014-02-14 00:00:00	56330.6348032407	2013-02-07 15:14:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071417	We propose simultaneous NuSTAR/Suzaku observations of NGC 4151 and IC 4329A. These pointings will achieve three goals: (1) They will provide the best-ever broad-band X-ray spectra of two of the brightest Seyfert galaxies in the 0.5-80 keV band; (2) They will enable broad-band, time-resolved X-ray spectroscopy of these fascinating and variable sources; (3) They will serve as invaluable calibration targets for the two observatories. The spectral coverage and sensitivity will enable the continuum, absorption and reflection components of each spectrum to be conclusively disentangled, allowing us to determine whether inner disk reflection signatures are present. We will also be able to break the degeneracy between the coronal temperature and optical depth in both AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	LAURA BRENNEMAN		USA	7	AO7	SHEDDING NEW LIGHT ON THE BROAD-BAND X-RAY SPECTRA OF NGC 4151 AND IC 4329A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707024010/	Quick Look
238	NGC 5252	204.5663	4.5481	203.934961	4.801923	201.032031	13.744519	331.30380316	64.80829028	117.6998	56287.8794791667	2012-12-26 21:06:27	56289.0952777778	2012-12-28 02:17:12	707028010	50.2701	45	50.2701	50.2921	0	50.2766	2	2	0	2	1	0	0	43.3367	43.3367	105.0278	0	PROCESSED	57608.3760300926	2016-08-08 09:01:29	56687	2014-01-30 00:00:00	56321.5462268518	2013-01-29 13:06:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071424	A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN.	EXTRAGALACTIC COMPACT SOURCES	7	C	TRACEY TURNER		USA	7	AO7	INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707028010/	Quick Look
239	PDS 456	262.0802	-14.261	261.369515	-14.22093	262.220782	8.966234	10.39487872	11.16781955	96.2511	56344.8907407407	2013-02-21 21:22:40	56349.993912037	2013-02-26 23:51:14	707035010	182.299	450	182.299	182.299	0	182.299	2	2	0	2	1	0	0	160.3071	160.3071	440.8752	4	PROCESSED	57610.7549768518	2016-08-10 18:07:10	56018	2012-04-01 00:00:00	56363.6993981482	2013-03-12 16:47:08	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071431	PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456.	EXTRAGALACTIC COMPACT SOURCES	7	B	JAMES REEVES		USA	7	AO7	VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707035010/	Quick Look
240	PDS 456	262.0805	-14.2617	261.369811	-14.221632	262.221115	8.965551	10.39443055	11.16720212	96.2512	56354.8215972222	2013-03-03 19:43:06	56359.5001388889	2013-03-08 12:00:12	707035020	164.8107	450	164.8267	164.8107	0	164.8291	2	2	0	2	1	0	0	147.4496	147.4496	404.1815	2	PROCESSED	57610.8342824074	2016-08-10 20:01:22	56018	2012-04-01 00:00:00	56373.6804166667	2013-03-22 16:19:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071431	PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456.	EXTRAGALACTIC COMPACT SOURCES	7	B	JAMES REEVES		USA	7	AO7	VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707035020/	Quick Look
241	0836+710	130.3582	70.9091	129.096	71.086996	109.311372	50.162038	143.52368034	34.42368753	111.9979	56213.6030787037	2012-10-13 14:28:26	56213.8223726852	2012-10-13 19:44:13	707042010	10.613	10	10.613	10.613	0	10.613	1	1	0	1	1	0	0	8.866	8.866	18.9279	0	PROCESSED	57607.7537615741	2016-08-07 18:05:25	56598	2013-11-02 00:00:00	56232.4320717593	2012-11-01 10:22:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071601	We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	7	AO7	MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707042010/	Quick Look
242	BL LAC	330.6707	42.2941	330.154473	42.052039	354.261979	49.60384	92.59387966	-10.42383814	77.7587	56431.6193981482	2013-05-19 14:51:56	56431.8724884259	2013-05-19 20:56:23	707044010	12.7426	10	12.7506	12.7426	0	12.7506	1	1	0	1	1	0	0	13.144	13.144	21.8319	0	PROCESSED	57611.320625	2016-08-11 07:41:42	56826	2014-06-18 00:00:00	56455.7300231482	2013-06-12 17:31:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071601	We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	7	AO7	MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707044010/	Quick Look
243	MKN 335	1.5767	20.2085	0.933785	19.930185	9.740922	17.859652	108.75946317	-41.41793251	71.5257	56454.1494907407	2013-06-11 03:35:16	56457.9792824074	2013-06-14 23:30:10	708016010	143.995	300	144.027	143.995	0	144.027	2	2	0	2	1	0	0	129.5529	129.5529	330.8674	3	PROCESSED	57611.6156828704	2016-08-11 14:46:35	56383	2013-04-01 00:00:00	56470.7662037037	2013-06-27 18:23:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081411	The idea of this proposal is trigger a 300ks observation with Suzaku of the Narrow Line Seyfert 1 Galaxy Mkn 335 during one of its low X-ray flux states. The goal here is to measure its underlying broad-band continuum with Suzaku during a low state and compare it with the 2006 high-state observations. Mkn 335 is one of the best examples of an AGN that went into a deep minimum X-ray flux state. Two competing models can explain these extreme low states: reflection models and partial covering absorber models. Both models still require a variable underlying intrinsic continuum. The science driver is to find out what is causing these low X-ray flux states that have been observed in several NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	A	DIRK GRUPE		USA	8	AO8-TOO	INTRINSIC LOW-STATE X-RAY LUMINOSITY OF THE NLS1 MKN 335	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708016010/	Quick Look
244	MCG-5-23-16	146.9232	-30.945	146.373955	-30.712416	162.623211	-41.142672	262.74537578	17.2400137	295.4404	56444.9213194444	2013-06-01 22:06:42	56448.2467361111	2013-06-05 05:55:18	708021010	159.5262	300	159.5582	159.5262	0	159.5582	2	2	0	2	1	0	0	155.1267	155.1267	287.3018	1	PROCESSED	57611.525787037	2016-08-11 12:37:08	56383	2013-04-01 00:00:00	56461.789537037	2013-06-18 18:56:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081416	Significant recent developments in probing environments around AGN black holes has been achieved using X-ray reverberation. They were initially detected in the soft excess of several NLS1s, then recently, the first Fe K reverberation was also seen. In addition to measuring x-rays reverberating a few r_g from the event horizon, short/long delays from different radii have been separated for the first time in NGC4151. Here we propose to observe MCG-5-23-1 for 300 ks in order to study its iron K reverberation. It is optimally one of the brightest and most variable AGN in X-rays. Archival data already show very exciting signatures of Fe K reverberation. With new observations we aim to constrain the emitting region size and study the emission originating at different distances from of the hole.	EXTRAGALACTIC COMPACT SOURCES	7	A	ABDERAHMEN ZOGHBI		USA	8	AO8	IRON K REVERBERATION IN MCG 5-23-16	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708021010/	Quick Look
245	NGC 235A	10.7176	-23.5378	10.098982	-23.81167	359.839777	-25.738096	94.13393297	-85.9211578	213.1719	56636.0921759259	2013-12-10 02:12:44	56636.4792939815	2013-12-10 11:30:11	708026010	19.8251	20	19.8331	19.8251	0	19.8409	2	2	0	2	1	0	0	18.2251	18.2251	33.4439	1	PROCESSED	57613.5511921296	2016-08-13 13:13:43	56383	2013-04-01 00:00:00	56646.6871412037	2013-12-20 16:29:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081419	The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come.	EXTRAGALACTIC COMPACT SOURCES	7	C	TAHIR YAQOOB		USA	8	AO8	ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708026010/	Quick Look
246	CENTAURUS A	201.3699	-43.0194	200.636516	-42.759434	217.141069	-31.326977	309.51956362	19.416494	303.7255	56519.1824305556	2013-08-15 04:22:42	56519.4264930556	2013-08-15 10:14:09	708036010	10.6751	10	10.6751	10.6751	0	10.6911	1	1	0	1	1	0	0	10.0647	10.0647	21.0799	0	PROCESSED	57612.2554050926	2016-08-12 06:07:47	56954	2014-10-24 00:00:00	56587.7389351852	2013-10-22 17:44:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081433	We request observations of the nucleus of the radio galaxy Centaurus A to study time variability of its broadband spectral energy distribution (SED) and constrain jet emission models of radio-loud AGN. Due to its proximity, Cen A can be studied in unique detail. Although frequently observed, no time-dependent, simultaneous SEDs covering the spectrum from radio to gamma-rays have been obtained for Cen A so far. Since AGN are highly variable, only quasi-contemporaneous SEDs allow us to constrain parameters of jet emission models. Combining our TANAMI radio Very Long Baseline Interferometry monitoring campaign and Fermi observations with simultaneous Suzaku spectra will fill the gap in energy and address the time-dependent behavior of jet emission and torus absorption with high accuracy.	EXTRAGALACTIC COMPACT SOURCES	7	B	ROOPESH OJHA		USA	8	AO8	SIMULTANEOUS SUZAKU AND MULTIWAVELENGTH OBSERVATIONS OF THE NUCLEUS OF CENTAURUS A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708036010/	Quick Look
247	CENTAURUS A	201.3033	-43.0014	200.570255	-42.741318	217.080563	-31.331883	309.47108059	19.44109405	111.5377	56663.4710763889	2014-01-06 11:18:21	56663.6613888889	2014-01-06 15:52:24	708036020	7.3652	10	7.3652	7.3732	0	7.3732	1	1	0	1	1	0	0	6.5444	6.5444	16.4399	0	PROCESSED	57613.7500462963	2016-08-13 18:00:04	57086	2015-03-05 00:00:00	56719.7206944444	2014-03-03 17:17:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081433	We request observations of the nucleus of the radio galaxy Centaurus A to study time variability of its broadband spectral energy distribution (SED) and constrain jet emission models of radio-loud AGN. Due to its proximity, Cen A can be studied in unique detail. Although frequently observed, no time-dependent, simultaneous SEDs covering the spectrum from radio to gamma-rays have been obtained for Cen A so far. Since AGN are highly variable, only quasi-contemporaneous SEDs allow us to constrain parameters of jet emission models. Combining our TANAMI radio Very Long Baseline Interferometry monitoring campaign and Fermi observations with simultaneous Suzaku spectra will fill the gap in energy and address the time-dependent behavior of jet emission and torus absorption with high accuracy.	EXTRAGALACTIC COMPACT SOURCES	7	B	ROOPESH OJHA		USA	8	AO8	SIMULTANEOUS SUZAKU AND MULTIWAVELENGTH OBSERVATIONS OF THE NUCLEUS OF CENTAURUS A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708036020/	Quick Look
248	ABELL 998	156.5862	67.9284	155.666008	68.182911	124.296815	52.261797	140.87284378	43.80315875	119.4303	56601.7924768518	2013-11-05 19:01:10	56602.9584722222	2013-11-06 23:00:12	708041010	60.2402	60	60.2402	60.2404	0	60.2562	3	2	0	2	1	0	0	51.856	51.856	100.7319	2	PROCESSED	57613.2563657407	2016-08-13 06:09:10	56980	2014-11-19 00:00:00	56614.6831944444	2013-11-18 16:23:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081533	We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters.	EXTRAGALACTIC COMPACT SOURCES	7	C	LAURENCE DAVID		USA	8	AO8	MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708041010/	Quick Look
249	HOLMBERG IX X-1	149.4663	69.0509	148.44846	69.289367	119.784926	51.679022	141.94846823	41.07666025	284.4995	57158.2357291667	2015-05-16 05:39:27	57159.0827546296	2015-05-17 01:59:10	709015040	34.12	30	34.12	34.128	0	34.128	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.6575347222	2016-08-18 15:46:51	57536	2016-05-28 00:00:00	57168.6253935185	2015-05-26 15:00:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091251	Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs.	EXTRAGALACTIC COMPACT SOURCES	7	A	DOMINIC WALTON		USA	9	AO9	MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015040/	Quick Look
250	HE0512-3329	78.5445	-33.4308	78.084109	-33.487216	72.678048	-56.186874	236.61833373	-33.85137764	251.0519	57071.9701388889	2015-02-18 23:17:00	57072.4937847222	2015-02-19 11:51:03	709020030	25.0955	26	25.0955	25.0955	0	25.0955	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6171296296	2016-08-17 14:48:40	57457	2016-03-10 00:00:00	57087.4623726852	2015-03-06 11:05:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091431	The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission.	EXTRAGALACTIC COMPACT SOURCES	7	B	BIN CHEN		USA	9	AO9	CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709020030/	Quick Look
251	ABELL2801	9.6433	-29.1188	9.027926	-29.393572	356.054774	-30.312746	357.12193154	-86.53506096	232.0377	53701.3547106482	2005-11-27 08:30:47	53702.1668865741	2005-11-28 04:00:19	800008010	34.89	25	34.89	34.89	34.89	34.89	2	2	2	2	1	0	0	30.1636	30.1636	70.1639	1	PROCESSED	57528.0891898148	2016-05-20 02:08:26	54247	2007-05-27 00:00:00	54038.3717361111	2006-10-30 08:55:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001025	We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYUKI TAMURA		JAP	0	SWG	THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800008010/	Quick Look
252	ABELL 1795 Near North	207.2221	26.7993	206.645445	27.047459	193.815884	35.172187	34.737463	77.20142043	130.7334	53714.7756481482	2005-12-10 18:36:56	53715.3203587963	2005-12-11 07:41:19	800012020	24.4106	25	24.4266	24.4106	24.4426	24.4346	1	1	1	1	1	0	0	25.1798	25.1798	47.0559	2	PROCESSED	57532.404375	2016-05-24 09:42:18	54247	2007-05-27 00:00:00	54038.8804166667	2006-10-30 21:07:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012020/	Quick Look
253	ABELL 1795 Near South	207.2228	26.4007	206.645046	26.648859	194.026663	34.812966	32.94964182	77.16185549	129.833	53715.9739467593	2005-12-11 23:22:29	53716.5355787037	2005-12-12 12:51:14	800012040	26.074	25	26.098	26.0919	26.074	26.086	2	2	2	2	1	0	0	25.7986	25.7986	48.522	1	PROCESSED	57532.4329282407	2016-05-24 10:23:25	54247	2007-05-27 00:00:00	54039.0706018518	2006-10-31 01:41:40	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012040/	Quick Look
254	NGC4388	186.4461	12.6674	185.812197	12.944186	180.780806	14.166666	279.11809751	74.34084148	119.622	53728.3779976852	2005-12-24 09:04:19	53731.250162037	2005-12-27 06:00:14	800017010	123.6341	100	123.9249	125.8143	123.6341	124.1523	2	2	2	2	1	0	0	111.8209	111.8209	248.128	3	PROCESSED	57532.5484143518	2016-05-24 13:09:43	54247	2007-05-27 00:00:00	54039.5984375	2006-10-31 14:21:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001077	Large-scale X-ray nebulae up to a few tens of kpc have been often found in starburst galaxies, which is thermally heated up by the superwind from the starburst nucleus. Iwasawa et al. (2003) found a large X-ray nebula up to 16kpc around NGC4388, which is photoiionized by Seyfert nucleus. Thus, this result suggests that the hard X-ray emission from active galactic nucleus could be a prime heat source of nebula. The goals of this observation are (1) to see how far the X-ray nebula is extended, (2) to obtain its precise X-ray spectrum, (3) to determine what is the X-ray emission mechanism, and (4) to exam if the photoionization by AGN could be a prime heat source of the galactic halo. We determine the photon index and the high energy cut-off of the power-law component from the HXD spectrum.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKESHI TSURU		JAP	0	SWG	VERY EXTENDED PHOTOIONIZED X-RAY NEBULA AROUND THE SEYFERT GALAXY NGC4388	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800017010/	Quick Look
255	Z8276	266.0474	32.9693	265.586798	32.989586	263.998981	56.326696	57.88393681	27.65216461	308.1365	53961.1406134259	2006-08-14 03:22:29	53961.4723958333	2006-08-14 11:20:15	801079010	14.9374	14	14.9374	14.9374	14.9374	14.9374	1	1	1	1	1	0	0	15.462	15.462	28.658	0	PROCESSED	57535.267962963	2016-05-27 06:25:52	54391	2007-10-18 00:00:00	54018.6023842593	2006-10-10 14:27:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801079010/	Quick Look
256	BOOTES GROUP 26	219.0541	33.7727	218.530502	33.989642	201.885156	45.915481	55.78379271	66.53529007	323.2958	54265.160787037	2007-06-14 03:51:32	54266.3092476852	2007-06-15 07:25:19	802055010	43.6657	38	43.6737	43.6817	0	43.6657	2	2	0	2	1	0	0	38.8727	38.8727	99.2108	0	PROCESSED	57538.9553703704	2016-05-30 22:55:44	54695	2008-08-17 00:00:00	54271.4809837963	2007-06-20 11:32:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021424	We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MARSHALL BAUTZ		USA	2	AO2	SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802055010/	Quick Look
257	PKS 0745-191	116.8852	-19.2901	116.331446	-19.165404	123.663194	-39.639458	236.4397894	3.03527791	293.9994	54231.0124884259	2007-05-11 00:17:59	54231.8216898148	2007-05-11 19:43:14	802062010	32.0065	30	32.0065	32.0305	0	32.0145	2	2	0	2	1	0	0	27.7016	27.7016	69.9099	0	PROCESSED	57538.6154976852	2016-05-30 14:46:19	54695	2008-08-17 00:00:00	54238.8868518518	2007-05-18 21:17:04	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021440	PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ANDREW YOUNG		USA	2	AO2	PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062010/	Quick Look
258	PKS 0745-191	117.1155	-19.3739	116.561976	-19.248204	123.963107	-39.669924	236.62179243	3.1809503	294.0002	54233.2263773148	2007-05-13 05:25:59	54234.0369675926	2007-05-14 00:53:14	802062040	32.9092	30	32.9092	32.9092	0	32.9092	1	1	0	1	1	0	0	31.0085	31.0085	69.9999	0	PROCESSED	57538.6488541667	2016-05-30 15:34:21	54695	2008-08-17 00:00:00	54245.5354861111	2007-05-25 12:51:06	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021440	PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ANDREW YOUNG		USA	2	AO2	PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062040/	Quick Look
259	NGC1961BACKGROUND	85.5048	67.8763	84.182746	67.851301	87.633372	44.47331	145.2497599	18.81010884	72.0206	54748.602962963	2008-10-09 14:28:16	54749.1197222222	2008-10-10 02:52:24	803041010	24.1435	20	24.1435	24.1435	0	24.1435	2	2	0	2	1	0	0	20.099	20.099	44.6399	1	PROCESSED	57544.0915393518	2016-06-05 02:11:49	55148	2009-11-13 00:00:00	54780.6911342593	2008-11-10 16:35:14	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031401	Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio. The Milky Way is missing at least 70% of its baryons while lower mass galaxies retain less than 10% of their baryons. Theory suggests that these baryons were expelled by intense galactic winds during the primary star formation period. These galactic winds carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding the very massive spiral galaxy, NGC 1961, which has 10 times the stellar content of M31 and with v_rot = 450 km/sec. If successful, we will detect a significant fraction of the 5E11 Msun of its missing baryons.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	3	AO3	THE BARYONS CONTENT OF THE MOST MASSIVE SPIRAL GALAXY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803041010/	Quick Look
260	ABELL S753 RELIC	211.0241	-34.0331	210.287956	-33.79356	220.862622	-20.093047	319.70505054	26.46102153	102.5257	54838.0480555556	2009-01-07 01:09:12	54841.6668287037	2009-01-10 16:00:14	803053010	137.5275	120	137.5355	137.5275	0	137.5355	3	3	0	3	1	0	0	99.5992	99.5992	312.6056	3	PROCESSED	57545.2410069444	2016-06-06 05:47:03	55328	2010-05-12 00:00:00	54851.4730787037	2009-01-20 11:21:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031432	The cluster radio relic PKS B1400-33 in the poor cluster Abell S753 will be observed with the HXD/PIN to detect and characterize the nonthermal Inverse Compton emission. This is one of the brightest cluster radio relics known. Remarkably, it is associated with a relatively poor, cool cluster. Although it has many properties similar to other cluster radio relics, it is possible that it is an old radio lobe, displaced by motions or buoyancy. The HXD/PIN data will be a strong test of merger shock acceleration processes. The XIS observations will constrain the low energy nonthermal spectrum and determine the thermal gas properties near the relic, and allow a merger shock to be detected. The long exposure with the XIS will also provide accurate abundances for the gas in this cool cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CRAIG SARAZIN		USA	3	AO3	PKS B1400-33 AND ABELL S753: A VERY BRIGHT RADIO RELIC IN A POOR CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803053010/	Quick Look
261	A3112	49.4785	-44.2477	49.044044	-44.429449	25.501128	-58.962889	252.95565297	-56.08416767	11.0983	54609.240162037	2008-05-23 05:45:50	54611.0557638889	2008-05-25 01:20:18	803054010	67.4982	60	67.4982	67.4982	0	67.4982	2	2	0	2	1	0	0	59.0658	59.0658	156.8578	0	PROCESSED	57542.6456365741	2016-06-03 15:29:43	54988	2009-06-06 00:00:00	54620.3684490741	2008-06-03 08:50:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031434	We propose to perform spatially resolved spectroscopy on the X-ray bright relaxed galaxy cluster Abell 3112, in order to characterize its soft/hard X-ray excess component. Abell 3112 is one of two clusters with very strong soft excess emission (the other being Abell S1101, observed in AO1). The indications provided by this observation will be crucial in order to assess, beyond doubt, the reality of the soft excess emission, previously observed by all soft X-ray missions since EUVE. The proposed observation will constrain the nature of the excess emitter, and address outstanding questions in observational cosmology: the {it missing baryon} problem, the density of matter in the universe and the non-thermal energy in galaxy clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MASSIMILIANO BONAMENTE		USA	3	AO3	SOFT EXCESS, HARD EXCESS AND THERMAL EMISSION IN ABELL 3112	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803054010/	Quick Look
262	SHAPLEY OFF-FILAMENT	201.0894	-30.5701	200.390777	-30.309695	211.196223	-20.080758	311.26734846	31.76827748	298.8248	54666.4273958333	2008-07-19 10:15:27	54670.1905439815	2008-07-23 04:34:23	803068010	143.4669	140	143.4749	143.4749	0	143.4669	2	2	0	2	1	0	0	110.8111	110.8111	325.0858	2	PROCESSED	57543.1803240741	2016-06-04 04:19:40	55073	2009-08-30 00:00:00	54707.3575694444	2008-08-29 08:34:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031451	It is, in principle, possible to search for the signature of the Warm-Hot Intergalactic Medium (WHIM) in regions between clusters, where WHIM filaments are expected. However, the complexity of the filament network and the distance between clusters makes this approach very difficult (if not impossible), except in few cases where several clusters are sufficiently close together, such as within a supercluster. We propose an investigation using Suzaku of a region within the Shapley Supercluster where, following the cluster network, a filament is expected and a ROSAT PSPC investigation has found excess emission. Suzaku s characteristics will allow a clear detection and characterization of the filament. A second observation in an empty region nearby will be used as control field.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MASSIMILIANO GALEAZZI		USA	3	AO3	FILAMENTARY X-RAY STRUCTURE IN THE SHAPLEY SUPERCLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803068010/	Quick Look
263	SMC X-1	19.2661	-73.446	18.934565	-73.709172	312.334379	-66.471359	300.41753301	-43.55692043	64.0051	55740.5953819444	2011-06-28 14:17:21	55741.0960069444	2011-06-29 02:18:15	706030060	18.6682	18	18.7129	18.7049	0	18.6682	2	2	0	1	1	0	0	20.6764	20.6764	43.2479	0	PROCESSED	57602.4222800926	2016-08-02 10:08:05	56163	2012-08-24 00:00:00	55775.167974537	2011-08-02 04:01:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030060/	Quick Look
264	NGC 669	26.8113	35.5683	26.082401	35.319076	38.038857	22.814409	135.52840833	-25.9346715	67.5273	55017.2207523148	2009-07-05 05:17:53	55018.4377777778	2009-07-06 10:30:24	804049010	50.2528	50	50.2608	50.2528	0	50.2608	1	1	0	1	1	0	0	45.4023	45.4023	105.1199	11	PROCESSED	57547.7727430556	2016-06-08 18:32:45	55395	2010-07-18 00:00:00	55029.2656944444	2009-07-17 06:22:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041504	Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio: the Milky Way retained only 30% of its baryons while lower mass galaxies retain less than 10%. Probably, these baryons were expelled by intense galactic winds during the early star formation period at z = 1-3. These galactic winds can carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding two extremely massive spiral galaxies, with 6-8 times the stellar content of M31 and with v_rot = 370, 420 km/s. If successful, we will detect a significant fraction of the 3-4E11 Msun of the missing baryons as hot gas.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	JOEL BREGMAN		USA	4	AO4	THE BARYON CONTENT OF MASSIVE SPIRAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804049010/	Quick Look
265	RXJ1159+5531	179.953	55.611	179.309735	55.889319	149.803846	49.191232	137.55848692	60.02702904	317.8793	54953.4172222222	2009-05-02 10:00:48	54955.52875	2009-05-04 12:41:24	804051010	85.4892	75	85.4972	85.4892	0	85.4972	2	2	0	2	1	0	0	82.4128	82.4128	182.4218	2	PROCESSED	57546.517974537	2016-06-07 12:25:53	55343	2010-05-27 00:00:00	54976.1055439815	2009-05-25 02:31:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041514	We propose a 75ks observation of the galaxy group RXJ1159+5531 to place definitive constraints on its gas out to the virial radius (Rvir). These unprecedented measurements will enable us to study the entropy profile at scales near the region in which accretion shocks become important, and will reveal whether its flattening outside the core of the group extends as far as Rvir. Furthermore, we will obtain the mass profile and test the validity of the NFW model in the outer parts of the halo. Due to its high surface brightness and favourable distance, RXJ1159+5531 is the ideal target with which to carry out this study. It will constitute a textbook case for constraining the feedback and other nongravitational processes which shape the distribution of hot gas in galaxy groups.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	PHILIP HUMPHREY		USA	4	AO4	GAS IN A GALAXY GROUP AT THE VIRIAL RADIUS: RXJ1159+5531, A TEXTBOOK EXAMPLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804051010/	Quick Look
266	NGC741MOSAICE_P1	29.7199	5.461	29.066489	5.218433	29.574235	-6.258595	152.014798	-53.55912322	71.7248	55053.8433796296	2009-08-10 20:14:28	55054.0834837963	2009-08-11 02:00:13	804052010	10.8302	10	10.8342	10.8302	0	10.8381	2	2	0	2	1	0	0	7.8627	7.8627	20.74	0	PROCESSED	57548.1137847222	2016-06-09 02:43:51	55448	2010-09-09 00:00:00	55081.2096875	2009-09-07 05:01:57	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052010/	Quick Look
267	NGC741MOSAICS_P4	29.2193	5.0492	28.567063	4.805449	28.959637	-6.470888	151.55342081	-54.14565062	71.7599	55053.1534259259	2009-08-10 03:40:56	55053.3759143518	2009-08-10 09:01:19	804054040	10.589	10	10.597	10.589	0	10.589	1	1	0	1	1	0	0	9.9689	9.9689	19.1919	0	PROCESSED	57548.09625	2016-06-09 02:18:36	55451	2010-09-12 00:00:00	55084.9935763889	2009-09-10 23:50:45	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054040/	Quick Look
268	ABELL 426 E1	50.3027	41.5257	49.474155	41.346372	58.885391	22.278944	150.79331238	-13.10366228	89.0025	55041.5144560185	2009-07-29 12:20:49	55041.7141666667	2009-07-29 17:08:24	804056010	9.696	10	9.696	9.696	0	9.696	1	1	0	1	1	0	0	7.856	7.856	17.2479	0	PROCESSED	57547.9587268518	2016-06-08 23:00:34	55419	2010-08-11 00:00:00	55050.256400463	2009-08-07 06:09:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804056010/	Quick Look
269	ABELL 426 E5	51.7975	41.5108	50.964978	41.337079	60.044403	21.962427	151.74947693	-12.48443224	87.0002	55042.7485069444	2009-07-30 17:57:51	55043.2932175926	2009-07-31 07:02:14	804060010	21.649	20	21.649	21.9423	0	21.929	3	2	0	2	1	0	0	22.1391	22.1391	47.0481	0	PROCESSED	57548.0130208333	2016-06-09 00:18:45	55427	2010-08-19 00:00:00	55060.702349537	2009-08-17 16:51:23	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804060010/	Quick Look
270	ABELL 426 N3	49.4023	42.2033	48.571812	42.020646	58.391407	23.116315	149.83616068	-12.90614214	59.9986	55062.4722106482	2009-08-19 11:19:59	55062.7542708333	2009-08-19 18:06:09	804065010	12.2498	10	12.2498	12.2498	0	12.2498	1	1	0	1	1	0	0	11.8582	11.8582	24.3619	0	PROCESSED	57548.2751157407	2016-06-09 06:36:10	55441	2010-09-02 00:00:00	55074.9931597222	2009-08-31 23:50:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804065010/	Quick Look
271	ABELL 426 N7	48.6285	43.1676	47.793828	42.98212	58.096043	24.202758	148.81295674	-12.39950143	59.9993	55064.6340509259	2009-08-21 15:13:02	55065.4329166667	2009-08-22 10:23:24	804069010	36.4901	30	36.4901	36.5101	0	36.5021	2	2	0	2	1	0	0	30.3696	30.3696	69.018	0	PROCESSED	57548.3120486111	2016-06-09 07:29:21	55441	2010-09-02 00:00:00	55075.0667708333	2009-09-01 01:36:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804069010/	Quick Look
272	RCS0928+3646	142.0898	36.7798	141.319732	36.998258	132.498761	20.704213	186.98438508	46.37223207	116.6063	55148.3222800926	2009-11-13 07:44:05	55149.1064699074	2009-11-14 02:33:19	804080010	36.5167	30	36.5327	36.5167	0	36.5327	2	2	0	2	1	0	0	27.0584	27.0584	67.7439	1	PROCESSED	57549.3099652778	2016-06-10 07:26:21	55546	2010-12-16 00:00:00	55180.0365972222	2009-12-15 00:52:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041525	Understanding relationships between baryons in galaxy clusters and the underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a cluster sample chosen independently of X-ray properties. We propose to study 14 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Chandra observations of 8 high-dispersion, low-z targets. Suzaku s superior throughput is required to probe the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 6 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AMALIA HICKS		USA	4	AO4	DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804080010/	Quick Look
273	A1795_FAR_NORTHEAST	207.4803	26.8793	206.904436	27.126887	194.02783	35.343989	35.17669327	76.97815393	300.5693	55010.6105439815	2009-06-28 14:39:11	55011.5556712963	2009-06-29 13:20:10	804082010	40.0263	35	40.0263	40.0263	0	40.0263	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57547.6967476852	2016-06-08 16:43:19	55395	2010-07-18 00:00:00	55026.4466087963	2009-07-14 10:43:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041528	The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	4	AO4	ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804082010/	Quick Look
274	A1795_FAR_WEST	206.824	26.695	206.246184	26.94403	193.479611	34.924294	34.12189199	77.54661564	300.5663	55008.5840625	2009-06-26 14:01:03	55009.4634143518	2009-06-27 11:07:19	804084010	35.4763	35	35.4843	35.4763	0	35.4843	2	2	0	2	1	0	0	30.3466	30.3466	75.9378	1	PROCESSED	57547.7077662037	2016-06-08 16:59:11	55395	2010-07-18 00:00:00	55022.2936458333	2009-07-10 07:02:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041528	The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	4	AO4	ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804084010/	Quick Look
275	A2204_FIELD_2	248.1003	5.3993	247.484152	5.504515	245.364183	26.985557	20.85022945	33.23419381	260.9996	55435.6212615741	2010-08-27 14:54:37	55436.6744675926	2010-08-28 16:11:14	805057010	39.7312	40	39.7392	39.7312	0	39.7421	2	2	0	2	1	0	0	35.3157	35.3157	90.9818	1	PROCESSED	57553.2244444445	2016-06-14 05:23:12	55287	2010-04-01 00:00:00	55449.2310416667	2010-09-10 05:32:42	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805057010/	Quick Look
276	A1413_FIELD_1	178.851	23.2234	178.207267	23.50167	169.288709	20.757468	226.97411288	76.74388731	303.0003	55345.0808333333	2010-05-29 01:56:24	55346.139849537	2010-05-30 03:21:23	805059010	40.2041	40	40.2041	40.2041	0	40.2041	2	2	0	2	1	0	0	34.564	34.564	91.4919	1	PROCESSED	57551.6776041667	2016-06-12 16:15:45	55287	2010-04-01 00:00:00	55365.2529513889	2010-06-18 06:04:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805059010/	Quick Look
277	NGC5129 OFF-CENTER2	201.1253	13.7341	200.509035	13.994301	194.045924	20.91983	334.52733324	74.54035563	127.8098	55548.7900810185	2010-12-18 18:57:43	55549.42875	2010-12-19 10:17:24	805073010	30.7651	30	30.7811	30.7651	0	30.7811	2	2	0	2	1	0	0	25.2475	25.2475	55.168	0	PROCESSED	57554.4510416667	2016-06-15 10:49:30	55960	2012-02-03 00:00:00	55593.1036805556	2011-02-01 02:29:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051512	Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	XINYU DAI		USA	5	AO5	BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805073010/	Quick Look
278	NGC5129 BACKGROUND	201.7433	13.5725	201.127421	13.831619	194.704871	21.009611	336.16988197	74.1046924	116.4041	55547.7947106482	2010-12-17 19:04:23	55548.0397106482	2010-12-18 00:57:11	805074010	12.2767	10	12.2767	12.2847	0	12.2927	2	2	0	2	1	0	0	10.7811	10.7811	21.16	0	PROCESSED	57554.4321180556	2016-06-15 10:22:15	55960	2012-02-03 00:00:00	55592.9616435185	2011-01-31 23:04:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051512	Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	XINYU DAI		USA	5	AO5	BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805074010/	Quick Look
279	ESO3060170 OFFSET	85.0343	-41.2366	84.63691	-41.261684	81.30371	-64.529199	246.8664627	-30.36071331	321.0164	55326.497025463	2010-05-10 11:55:43	55327.7204166667	2010-05-11 17:17:24	805076010	78.6782	80	78.6782	78.6862	0	78.6862	2	2	0	2	1	0	0	69.7827	69.7827	105.6858	1	PROCESSED	57551.4828240741	2016-06-12 11:35:16	55707	2011-05-26 00:00:00	55341.5427893518	2010-05-25 13:01:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051513	We propose 30 and 80 ksec observations of the X-ray brightest fossil group, ESO 3060170. The target pointings will reach to 75% of the virial radius from the center of the galaxy, in order to determine the temperature and metal abundances of group gas at large radii. This will allow us to determine the radial profiles of the gaseous iron mass to stellar light ratio, the relative distributions of ejecta from SN Ia and SN II, the entropy, the total mass to light ratio, and the dark matter concentration for this fossil group. The energy resolution and low background of the XIS instrument are crucial for this study, which will help constrain the evolutional history of this fossil group and tell us how fossil groups relate to normal groups and clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	YUANYUAN SU		USA	5	AO5	HOW DO FOSSIL GROUPS OF GALAXIES DIFFER FROM NORMAL GROUPS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805076010/	Quick Look
280	PKS 0745-191	116.7033	-18.9048	116.14781	-18.780899	123.330634	-39.304661	236.01965558	3.07990407	294.0011	55315.865462963	2010-04-29 20:46:16	55316.6418518518	2010-04-30 15:24:16	805084010	34.8356	35	34.8356	34.8356	0	34.8356	2	2	0	2	1	0	0	29.5067	29.5067	67.0759	1	PROCESSED	57551.3211458333	2016-06-12 07:42:27	55696	2011-05-15 00:00:00	55330.1469675926	2010-05-14 03:31:38	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051526	Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MATTHEW GEORGE		USA	5	AO5	BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805084010/	Quick Look
281	T CRB	239.8773	25.9106	239.353591	26.051383	230.095833	45.264151	42.36027985	48.16117824	268.9321	53984.9474652778	2006-09-06 22:44:21	53986.0911921296	2006-09-08 02:11:19	401043010	46.3033	50	46.3113	46.3113	46.3193	46.3033	2	2	2	2	1	0	0	45.4314	45.4314	98.8159	1	PROCESSED	57535.5107175926	2016-05-27 12:15:26	54526	2008-03-01 00:00:00	54053.4340856482	2006-11-14 10:25:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011106	Hard X-ray emission up to ~100 keV has recently been detected with INTEGRAL and Swift from 3 exceptional symbiotic stars. These 3 objects are members of a subclass of symbiotics characterized by rapid optical flickering, and in some cases jets, recurrent nova eruptions, and high-mass white dwarfs possibly headed toward supernova Type Ia explosion. The origin of the hard X-ray emission from these accreting white dwarfs is a mystery. Broad-band X-ray observations, which only Suzaku can provide, are needed to bridge the gap between existing soft and hard X-ray spectra. We propose to perform such Suzaku observations of RT Cru, T CrB, and RS Oph to distinguish among thermal emission from a magnetic accretion column, non-thermal emission from a jet, or some unforeseen emission mechanism.	GALACTIC POINT SOURCES	4	A	JENNIFER SOKOLOSKI		USA	1	AO1	THE NATURE OF HARD X-RAY SYMBIOTIC BINARIES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401043010/	Quick Look
282	RCS2343-3517	355.9933	-35.2927	355.337628	-35.570369	340.879701	-30.492367	359.21699124	-73.45928386	237.6557	55523.8239930556	2010-11-23 19:46:33	55525.0418171296	2010-11-25 01:00:13	805088010	48.3167	61	48.3167	48.3167	0	48.3167	2	2	0	2	1	0	0	40.1454	40.1454	105.1859	1	PROCESSED	57554.2088078704	2016-06-15 05:00:41	55903	2011-12-08 00:00:00	55537.0179861111	2010-12-07 00:25:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051527	Understanding relationships between baryons in galaxy clusters and underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a sample chosen independently of X-ray properties. We propose to study 13 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Suzaku/Chandra observations of 11 high-dispersion, low-z targets. Suzaku's superior throughput is required to complete the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 2 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	5	AO5	DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805088010/	Quick Look
283	IGRJ16465-4507	251.6303	-45.1738	250.724808	-45.083948	256.064043	-22.616175	340.00343338	0.10772124	284.9562	53987.3839814815	2006-09-09 09:12:56	53987.9203009259	2006-09-09 22:05:14	401052010	22.5279	20	22.5359	22.5279	22.5359	22.5359	2	2	2	2	1	0	0	24.6454	24.6454	46.332	0	PROCESSED	57535.4975925926	2016-05-27 11:56:32	54526	2008-03-01 00:00:00	54021.113287037	2006-10-13 02:43:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011132	INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	1	AO1	HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401052010/	Quick Look
284	ABELL 773	139.2619	51.6127	138.389122	51.822209	124.54102	33.911668	166.27594696	43.26641657	277.0001	55684.0736342593	2011-05-03 01:46:02	55684.909212963	2011-05-03 21:49:16	806027030	47.578	50	47.578	47.578	0	47.578	2	2	0	2	1	0	0	44.1095	44.1095	72.1819	0	PROCESSED	57601.9127083333	2016-08-01 21:54:18	55652	2011-04-01 00:00:00	55697.2793518518	2011-05-16 06:42:16	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806027030/	Quick Look
285	ABELL 1068	160.1718	40.1411	159.449793	40.402342	145.494968	29.227943	178.75085582	60.06234552	130.0011	55860.7020601852	2011-10-26 16:50:58	55861.8821527778	2011-10-27 21:10:18	806028010	51.9826	50	51.9906	51.9826	0	51.9826	2	2	0	2	1	0	0	44.5347	44.5347	101.9378	1	PROCESSED	57603.6168981482	2016-08-03 14:48:20	55652	2011-04-01 00:00:00	55874.1455324074	2011-11-09 03:29:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806028010/	Quick Look
286	ABELL 2667	358.0843	-26.1324	357.438238	-26.410641	347.261091	-23.090967	33.89369276	-76.76238411	64.8814	55725.7013773148	2011-06-13 16:49:59	55726.9814351852	2011-06-14 23:33:16	806029040	51.7936	50	51.7936	51.8161	0	51.8016	2	2	0	2	1	0	0	43.6427	43.6427	110.5818	1	PROCESSED	57602.3116319444	2016-08-02 07:28:45	55652	2011-04-01 00:00:00	55757.7024652778	2011-07-15 16:51:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806029040/	Quick Look
287	COMA E4	196.1292	27.8947	195.52895	28.162497	182.637315	31.793754	48.48781449	87.00057059	279.9984	55729.6868287037	2011-06-17 16:29:02	55730.3355671296	2011-06-18 08:03:13	806033010	20.2023	20	20.2023	20.2103	0	20.2183	2	2	0	2	1	0	0	20.516	20.516	56.0419	1	PROCESSED	57602.3427199074	2016-08-02 08:13:31	55652	2011-04-01 00:00:00	55770.1680092593	2011-07-28 04:01:56	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806033010/	Quick Look
288	BEYOND VIRGO 1	187.7129	16.0953	187.082675	16.371354	180.479874	17.795652	278.48728746	77.9786094	118.4704	55905.1491666667	2011-12-10 03:34:48	55905.8431828704	2011-12-10 20:14:11	806060010	22.2598	20	22.2678	22.2678	0	22.2598	2	2	0	2	1	0	0	20.63	20.63	59.9539	1	PROCESSED	57604.1022569444	2016-08-04 02:27:15	56284	2012-12-23 00:00:00	55917.0698958333	2011-12-22 01:40:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061523	To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORBERT WERNER		USA	6	AO6	LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806060010/	Quick Look
289	BEYOND VIRGO 2	187.7135	16.3643	187.083459	16.640353	180.363309	18.040696	277.98453264	78.22684296	118.4711	55905.8436574074	2011-12-10 20:14:52	55906.3980439815	2011-12-11 09:33:11	806061010	21.4115	20	21.4275	21.4115	0	21.4335	1	1	0	1	1	0	0	19.1816	19.1816	47.872	1	PROCESSED	57604.0951041667	2016-08-04 02:16:57	56284	2012-12-23 00:00:00	55917.0723842593	2011-12-22 01:44:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061523	To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORBERT WERNER		USA	6	AO6	LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806061010/	Quick Look
290	BEYOND VIRGO 6	187.7152	17.4312	187.085892	17.70725	179.897096	19.011602	275.76419982	79.20143703	118.777	55919.8968287037	2011-12-24 21:31:26	55920.9286574074	2011-12-25 22:17:16	806065010	39.5769	40	39.6169	39.5769	0	39.6169	1	1	0	1	1	0	0	33.7703	33.7703	89.136	2	PROCESSED	57604.2337962963	2016-08-04 05:36:40	56339	2013-02-16 00:00:00	55972.6645833333	2012-02-15 15:57:00	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061523	To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORBERT WERNER		USA	6	AO6	LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806065010/	Quick Look
291	LOCK-365	161.9095	57.7105	161.128548	57.974475	136.113511	45.200495	149.74973686	52.48617693	106.5217	55897.0768981482	2011-12-02 01:50:44	55900.1780439815	2011-12-05 04:16:23	806077010	149.9102	150	149.9422	149.9102	0	149.9422	2	2	0	2	1	0	0	131.1259	131.1259	267.9076	0	PROCESSED	57604.1079050926	2016-08-04 02:35:23	56065	2012-05-18 00:00:00	55914.3640393518	2011-12-19 08:44:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061532	We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	6	AO6	OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806077010/	Quick Look
292	AE AQUARII	310.0457	-0.9355	309.401118	-1.113434	312.219972	16.829528	45.22275468	-24.45710482	264.8759	53673.9022685185	2005-10-30 21:39:16	53676.043275463	2005-11-02 01:02:19	400001010	70.5289	100	70.5289	70.6169	70.5689	70.5449	3	3	3	3	1	0	0	59.4538	59.4538	184.9569	2	PROCESSED	57527.7308217593	2016-05-19 17:32:23	54247	2007-05-27 00:00:00	54036.9851388889	2006-10-28 23:38:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001004	We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku.	GALACTIC POINT SOURCES	4	A	YUKIKATSU TERADA		JAP	0	SWG	SEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKU		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400001010/	Quick Look
293	RCS051838-4324.9	79.6593	-43.4168	79.277976	-43.467716	71.171582	-66.18535	248.71475233	-34.61566895	286.4929	56016.4337268518	2012-03-30 10:24:34	56018.0001388889	2012-04-01 00:00:12	806083010	67.6666	75	67.6906	67.6666	0	67.6906	2	2	0	2	1	0	0	57.511	57.511	135.2938	1	PROCESSED	57605.0718402778	2016-08-05 01:43:27	56399	2013-04-17 00:00:00	56027.1518287037	2012-04-10 03:38:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061533	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	6	AO6	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806083010/	Quick Look
294	FG04	121.8798	33.9978	121.078663	34.143156	116.761327	13.47104	187.39667673	29.69857824	274.999	56053.6835648148	2012-05-06 16:24:20	56053.9411921296	2012-05-06 22:35:19	807053010	10.821	10	10.821	10.821	0	10.821	1	1	0	1	1	0	0	11.0766	11.0766	22.2559	0	PROCESSED	57605.3537268518	2016-08-05 08:29:22	56435	2013-05-23 00:00:00	56068.6337152778	2012-05-21 15:12:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071511	Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ELENA D'ONGHIA		USA	7	AO7	SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807053010/	Quick Look
295	RXJ1416.4+2315	214.0475	23.1701	213.473378	23.401516	202.507315	34.451007	25.95045598	70.44211392	293.1172	56123.5919675926	2012-07-15 14:12:26	56124.3335300926	2012-07-16 08:00:17	807065010	23.7192	120	23.7272	23.7192	0	23.7272	1	1	0	1	1	0	0	22.6028	22.6028	64.0639	1	PROCESSED	57606.624537037	2016-08-06 14:59:20	56598	2013-11-02 00:00:00	56144.9996180556	2012-08-05 23:59:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071514	Our study of the fossil group RXJ 1159+5531 does not find the gas clumping invoked to explain unexpectedly flat entropy profiles and large gas fractions near r_vir in some clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation, which may reflect that hydrostatic equilibrium is very accurate in this highly evolved fossil group. To examine whether these results extend to other fossils and to more massive systems, we propose to observe the fossil cluster RXJ 1416.4+2315 (M_vir ~3 x 10^14 M_sun) to constrain its entropy and gas fraction out to r_vir (r_112). Since it is located at a redshift of 0.137, this target provides an efficient means to explore the outer ICM, where a large azimuthal portion (~80%) of r_vir can be observed in a single Suzaku field.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DAVID BUOTE		USA	7	AO7	RXJ1416.4+2315: A MASSIVE FOSSIL CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807065010/	Quick Look
296	ANTLIA E4	158.9815	-35.3293	158.412243	-35.069878	177.109135	-40.308725	274.02289995	19.82417732	279.0004	56094.1885532407	2012-06-16 04:31:31	56095.3688888889	2012-06-17 08:51:12	807069010	46.5031	45	46.5031	46.5195	0	46.5111	2	2	0	2	1	0	0	38.6185	38.6185	101.9699	0	PROCESSED	57605.7108564815	2016-08-05 17:03:38	56477	2013-07-04 00:00:00	56111.0445023148	2012-07-03 01:04:05	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071521	We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	7	AO7	MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807069010/	Quick Look
297	ABELL 2597	351.5123	-12.2071	350.862263	-12.482246	347.371921	-7.852378	65.46064183	-65.03980804	250.0004	56263.5374884259	2012-12-02 12:53:59	56264.7744907407	2012-12-03 18:35:16	807073030	50.2983	50	50.3063	50.2983	0	50.2983	2	2	0	2	1	0	0	42.3364	42.3364	106.8558	0	PROCESSED	57608.190625	2016-08-08 04:34:30	56018	2012-04-01 00:00:00	56279.6896180556	2012-12-18 16:33:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073030/	Quick Look
298	RCS022456-0348.8	36.2382	-3.8143	35.608784	-4.039767	32.599151	-17.199331	170.77871975	-57.71972182	253.341	56324.4414814815	2013-02-01 10:35:44	56325.9579282407	2013-02-02 22:59:25	807078010	50.8118	49	50.8227	50.8147	0	50.8118	2	2	0	2	1	0	0	46.195	46.195	131.0078	0	PROCESSED	57610.5290509259	2016-08-10 12:41:50	56711	2014-02-23 00:00:00	56345.5401967593	2013-02-22 12:57:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071525	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	7	AO7	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807078010/	Quick Look
299	COMA NW3	194.5571	28.6697	193.954123	28.93948	180.77176	31.860187	79.10101688	87.84902047	319.997	55732.646099537	2011-06-20 15:30:23	55732.9793865741	2011-06-20 23:30:19	806040010	10.469	10	10.469	10.469	0	10.469	2	2	0	2	1	0	0	10.1768	10.1768	28.7899	0	PROCESSED	57602.3615856482	2016-08-02 08:40:41	55652	2011-04-01 00:00:00	55768.2657523148	2011-07-26 06:22:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806040010/	Quick Look
300	ESO318-021	163.2697	-40.3328	162.69794	-40.066534	184.394245	-42.926152	279.73310675	17.14745123	111.1499	56639.0964467593	2013-12-13 02:18:53	56643.3605902778	2013-12-17 08:39:15	808063010	152.2198	150	152.2198	152.2198	0	152.2198	2	2	0	2	1	0	0	132.9733	132.9733	368.3777	4	PROCESSED	57613.6558101852	2016-08-13 15:44:22	57050	2015-01-28 00:00:00	56680.7667476852	2014-01-23 18:24:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081503	The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	DAVID BUOTE		USA	8	AO8	THE DARK MATTER AND BARYON PROFILES OF ISOLATED ELLIPTICAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808063010/	Quick Look
301	RXJ1416.4+2315	214.0623	23.3458	213.488767	23.577175	202.437112	34.617457	26.46691952	70.47697816	292.671	56496.6431712963	2013-07-23 15:26:10	56499.3349074074	2013-07-26 08:02:16	808064010	122.9317	120	122.9317	122.9317	0	122.9317	2	2	0	2	1	0	0	116.8226	116.8226	232.5474	2	PROCESSED	57612.032650463	2016-08-12 00:47:01	56953	2014-10-23 00:00:00	56587.4880671296	2013-10-22 11:42:49	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081511	Our preliminary analysis of AO7 XIS data of the fossil cluster RXJ 1416.4+2315 does not find evidence for the gas clumping invoked to explain the flat entropy profiles and large gas fractions found near r_vir in several nearby clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation as we found previously for the fossil group/cluster RXJ 1159+5531, which may reflect that hydrostatic equilibrium is very accurate in these highly evolved fossil systems. Therefore, we propose a Suzaku observation in a different azimuthal direction to double the azimuthal coverage at r_vir (from ~30% to ~60%) in order to test for the presence of azimuthal ICM variations expected for clusters that grow by accretion along large-scale filaments.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	DAVID BUOTE		USA	8	AO8	VERIFYING RELAXED ICM AT THE VIRIAL RADIUS IN A FOSSIL GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808064010/	Quick Look
302	MKW-N2	181.1507	2.5267	180.510236	2.805064	180.047061	2.775514	276.44275792	62.96433079	120.2659	56663.6701967593	2014-01-06 16:05:05	56666.0195023148	2014-01-09 00:28:05	808067010	99.7883	100	99.7883	99.7883	0	99.7883	2	2	0	2	1	0	0	99.9362	99.9362	202.9537	4	PROCESSED	57613.8221643518	2016-08-13 19:43:55	57096	2015-03-15 00:00:00	56730.5704166667	2014-03-14 13:41:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081512	We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	YUANYUAN SU		USA	8	AO8	PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808067010/	Quick Look
303	A133_FIELD_2	15.4723	-21.5865	14.860654	-21.855252	5.175152	-25.865615	146.72727626	-83.96930246	231.9996	56646.6689583333	2013-12-20 16:03:18	56647.8294212963	2013-12-21 19:54:22	808082010	50.6406	50	50.6646	50.6566	0	50.6406	2	2	0	2	1	0	0	46.4338	46.4338	100.2559	1	PROCESSED	57613.6561921296	2016-08-13 15:44:55	57061	2015-02-08 00:00:00	56695.6286689815	2014-02-07 15:05:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081525	We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ERIC MILLER		USA	8	AO8	A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808082010/	Quick Look
304	ABELL 1689 (OFFSET)	198.1816	-1.2688	197.539227	-1.003818	197.250037	5.95631	314.01012466	61.14421574	293.5484	56470.3775578704	2013-06-27 09:03:41	56473.3751273148	2013-06-30 09:00:11	808089010	105.7518	396	105.7598	105.7518	0	105.7518	2	2	0	2	1	0	0	95.0477	95.0477	258.9556	4	PROCESSED	57611.7314930556	2016-08-11 17:33:21	56383	2013-04-01 00:00:00	56523.7467708333	2013-08-19 17:55:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081528	Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	8	AO8	SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089010/	Quick Look
305	ABELL 1689 (OFFSET)	198.1818	-1.2687	197.539427	-1.003718	197.250185	5.956479	314.01056832	61.14428006	293.5484	56473.3751388889	2013-06-30 09:00:12	56475.3022916667	2013-07-02 07:15:18	808089020	67.8003	396	67.8083	67.8003	0	67.8083	2	2	0	2	1	0	0	60.9649	60.9649	166.4698	5	PROCESSED	57611.6944907407	2016-08-11 16:40:04	56383	2013-04-01 00:00:00	56491.6594675926	2013-07-18 15:49:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081528	Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	8	AO8	SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089020/	Quick Look
306	A1413	178.8303	23.6485	178.18646	23.926767	169.076487	21.133974	225.18767075	76.86550896	123.0348	53689.8362847222	2005-11-15 20:04:15	53692.5939699074	2005-11-18 14:15:19	800001010	107.8672	100	107.8672	108.0032	107.9472	107.9103	2	2	2	2	1	0	0	102.4315	102.4315	238.2397	7	PROCESSED	57528.0427546296	2016-05-20 01:01:34	54247	2007-05-27 00:00:00	54038.1136689815	2006-10-30 02:43:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001010	No cluster has had its X-ray temperature measured out to the virial radius. Hence no cluster has had it total mass measured using X-ray methods. Typically these measurements extend only to 60% of the virial radius. We propose to perform these measurements for the first time and with high accuracy for the relaxed cluster A1413. The low Suzaku background permits us to make this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	J. HENRY		JAP	0	SWG	CLUSTER TEMPERATURE AND MASS MEASUREMENT TO THE VIRIAL RADIUS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800001010/	Quick Look
307	NGC 953	37.7955	29.584	37.059252	29.362946	44.923297	13.943505	147.58231113	-28.46974369	250.5565	57059.5397222222	2015-02-06 12:57:12	57063.4376157407	2015-02-10 10:30:10	809055010	150.8191	150	150.8191	150.8671	0	150.8671	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6137037037	2016-08-17 14:43:44	56748	2014-04-01 00:00:00	57107.4400578704	2015-03-26 10:33:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091503	The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^13 m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have complementary Chandra observations.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	DAVID BUOTE		USA	9	AO9	THE DARK MATTER AND BARYON PROFILES OF ISOLATED ELLIPTICAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809055010/	Quick Look
308	FG10	163.7228	55.3656	162.966111	55.632252	139.04941	43.748241	151.60913312	54.78459511	121.1085	56973.8939467593	2014-11-12 21:27:17	56975.0737615741	2014-11-14 01:46:13	809061010	61.1085	60	61.1085	61.2978	0	61.2978	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7792361111	2016-08-16 18:42:06	57444	2016-02-26 00:00:00	57076.4143865741	2015-02-23 09:56:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091512	Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	ELENA D'ONGHIA		USA	9	AO9	SCALING RELATIONS OF FOSSIL GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809061010/	Quick Look
309	ABELL 2259	259.9722	27.8097	259.476075	27.85934	255.895749	50.75928	50.52312942	31.25775464	109.9997	57081.1636458333	2015-02-28 03:55:39	57082.4113194445	2015-03-01 09:52:18	809081010	42.2203	42.5	42.2203	43.0443	0	43.1003	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.6840509259	2016-08-17 16:25:02	57465	2016-03-18 00:00:00	57091.4611226852	2015-03-10 11:04:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091526	Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	9	AO9	REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809081010/	Quick Look
310	ABELL 2259	260.1067	27.5543	259.609076	27.603301	256.126173	50.518333	50.27658806	31.07091189	109.9997	57083.6006018518	2015-03-02 14:24:52	57084.7258564815	2015-03-03 17:25:14	809081030	44.2468	42.5	44.2468	44.2548	0	44.2548	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.7027314815	2016-08-17 16:51:56	57475	2016-03-28 00:00:00	57107.4892476852	2015-03-26 11:44:31	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091526	Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	KA-WAH WONG		USA	9	AO9	REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809081030/	Quick Look
311	M82 N1	148.6748	70.0409	147.627175	70.277324	118.519213	52.349642	141.10131259	40.27429686	283.7057	57159.0836921296	2015-05-17 02:00:31	57160.4702546296	2015-05-18 11:17:10	809122010	59.5055	60	59.5055	59.5055	0	59.5135	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57618.6721759259	2016-08-18 16:07:56	57538	2016-05-30 00:00:00	57171.5244212963	2015-05-29 12:35:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091701	We propose to carry out joint Chandra and Suzaku observations of the starburst galaxy M82. We will search for extended clumps similar to the Northern Cap out to 45 kpc. We will also constrain the density and temperature profiles of the tenuous wind emission out to large radii. These data can place important constraints on theoretical models of starburst galaxies and their environments. We will test models such as the Chevalier & Clegg adiabatic wind model, hydrostatic halo model, shocked clouds in a wind, etc. The excellent Chandra spatial resolution combining with the low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	S	KA-WAH WONG		USA	9	AO9	SEARCH FOR THE OUTER BOUNDARY OF THE STARBURST GALAXY: M82	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809122010/	Quick Look
312	ZETA OPH	249.2878	-10.5628	248.598836	-10.46277	249.217592	11.396196	6.28378927	23.59180747	94.9452	54540.8758912037	2008-03-15 21:01:17	54543.8543287037	2008-03-18 20:30:14	402038010	105.5837	100	105.5917	105.5917	0	105.5837	2	2	0	2	1	0	0	79.9813	79.9813	257.3178	2	PROCESSED	57541.9592708333	2016-06-02 23:01:21	54922	2009-04-01 00:00:00	54553.3785300926	2008-03-28 09:05:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021022	Zeta Oph is a well known optical and UV variable star and is now known to displays both short (hours) and long (years) term X-ray variability. The short term variability has different periods for the soft and hard X-ray bands. The soft period being identical with the UV DAC reoccurrence period. The hard period is 40 percent smaller than the soft period and the source of it's variability is thus far unclear. Zeta Oph has been observed by several X-ray telescopes over a 22 year time span and the observations show significant variations in the total observed X-ray flux. We are requesting an XIS observation of this star to develop: 1) a greater understanding of the hard X-ray emission; 2) confirm the hard and soft periodicities, and; 3) provide further monitoring of the long term variability.	GALACTIC POINT SOURCES	4	C	WAYNE WALDRON		USA	2	AO2	MULTIPLE X-RAY EMISSION PERIODICITY IN THE RAPIDLY ROTATING O-STAR, ZETA OPH	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402038010/	Quick Look
313	4U1705-44	257.2319	-44.0961	256.328793	-44.032411	260.195881	-21.087692	343.32770356	-2.34122442	265.637	54348.6112847222	2007-09-05 14:40:15	54349.0140509259	2007-09-06 00:20:14	402051010	13.3436	15	13.3436	13.3436	0	13.3436	1	1	0	1	1	0	0	9.3706	9.3706	34.7919	1	PROCESSED	57539.9453472222	2016-05-31 22:41:18	54773	2008-11-03 00:00:00	54356.2627430556	2007-09-13 06:18:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021113	We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability.	GALACTIC POINT SOURCES	4	A	RONALD REMILLARD		USA	2	AO2	X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402051010/	Quick Look
314	AQL X-1	287.8182	0.5791	287.179926	0.495378	289.379323	22.828874	35.71383379	-4.14703266	264.9589	54382.2112384259	2007-10-09 05:04:11	54382.6877893518	2007-10-09 16:30:25	402053030	19.7117	15	19.7197	19.7277	0	19.7117	2	2	0	2	1	0	0	17.5522	17.5522	41.162	0	PROCESSED	57540.2157291667	2016-06-01 05:10:39	54770	2008-10-31 00:00:00	54402.5719328704	2007-10-29 13:43:35	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021114	We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data.	GALACTIC POINT SOURCES	4	A	RONALD REMILLARD		USA	2	AO2-TOO	X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402053030/	Quick Look
315	AQL X-1	287.8172	0.5775	287.178919	0.493782	289.378018	22.82742	35.71194856	-4.14687642	265.833	54397.9824074074	2007-10-24 23:34:40	54398.5072222222	2007-10-25 12:10:24	402053060	21.3648	15	21.4608	21.4608	0	21.3648	2	2	0	2	1	0	0	21.4022	21.4022	45.3439	0	PROCESSED	57540.3340509259	2016-06-01 08:01:02	54776	2008-11-06 00:00:00	54407.3747222222	2007-11-03 08:59:36	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021114	We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data.	GALACTIC POINT SOURCES	4	A	RONALD REMILLARD		USA	2	AO2-TOO	X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402053060/	Quick Look
316	AQL X-1	287.8217	0.5796	287.183429	0.495861	289.383158	22.828908	35.71588636	-4.14991498	243.6715	54403.2743171296	2007-10-30 06:35:01	54403.66	2007-10-30 15:50:24	402053070	17.5362	15	17.5842	17.604	0	17.5362	1	1	0	1	1	0	0	14.3322	14.3322	33.3199	0	PROCESSED	57540.3767824074	2016-06-01 09:02:34	54776	2008-11-06 00:00:00	54409.1320138889	2007-11-05 03:10:06	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021114	We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data.	GALACTIC POINT SOURCES	4	A	RONALD REMILLARD		USA	2	AO2-TOO	X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402053070/	Quick Look
317	X1630-472	248.5414	-47.3441	247.620794	-47.24014	254.106628	-25.078548	336.96314137	0.26612574	120.5775	53802.0758796296	2006-03-08 01:49:16	53802.7300231482	2006-03-08 17:31:14	400010040	21.2481	200	21.2481	21.2499	21.2499	21.2499	3	3	3	3	1	0	0	20.4778	20.4778	56.512	0	PROCESSED	57533.1620486111	2016-05-25 03:53:21	54247	2007-05-27 00:00:00	54041.7698726852	2006-11-02 18:28:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001058	We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		JAP	0	SWG-TOO	FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400010040/	Quick Look
318	4U2206+54	331.9811	54.5897	331.524827	54.344502	8.281106	58.879755	100.6432606	-1.04691755	90.2357	54236.1620949074	2007-05-16 03:53:25	54237.812662037	2007-05-17 19:30:14	402069010	103.9768	100	103.9848	103.9906	0	103.9768	3	3	0	3	1	0	0	99.7842	99.7842	142.5819	1	PROCESSED	57538.7118402778	2016-05-30 17:05:03	54695	2008-08-17 00:00:00	54242.76625	2007-05-22 18:23:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021125	4U 2206+54 is a high mass X-ray binary which is suspected to contain a neutron star accreting from the wind of its companion BD +53 2790. However, there has been no confirmed detection of X-ray pulsations, and while several authors have reported hints of a cyclotron line in the energy spectra near 30 keV, none have reported significant detections. We propose Suzaku observations to search for long-period pulsations with the XIS, and possible confirmation of the cyclotron line using HXD/PIN.	GALACTIC POINT SOURCES	4	A	MARK FINGER		USA	2	AO2	SUZAKU OBSERVATIONS OF THE PECULIAR HMXB 4U 2206+54	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402069010/	Quick Look
319	GRS 1915+105	288.7933	10.9535	288.203422	10.865162	292.134883	32.961388	45.37037141	-0.21130356	67.354	54227.6113657407	2007-05-07 14:40:22	54229.0717476852	2007-05-09 01:43:19	402071010	65.6568	37	65.6568	65.8039	0	65.6728	1	2	0	1	1	0	0	56.8973	56.8973	126.168	1	PROCESSED	57538.6640972222	2016-05-30 15:56:18	54702	2008-08-24 00:00:00	54235.5321759259	2007-05-15 12:46:20	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021132	We have discovered a connection between Fe line strength and QPO phase in RXTE observations of GRS 1915+105. This connection independently ties Fe lines to radii less than 100 R_Schw. QPO-phase-resolved Suzaku spectra will enable us to detect changes in the relativistic line profile (inner radius, equivalent width), to extend the connection to the broadband disk reflection spectrum, and to test models for the Fe line - QPO connection. Moreover, at CCD resolution, the connection can be used to over-constrain disk radii - a first step toward mapping the inner disk. We therefore request a 37 ksec TOO observation of GRS 1915+105. Understanding black hole accretion is fundamental to NASA's "SEU" theme.	GALACTIC POINT SOURCES	4	A	JON MILLER		USA	2	AO2-TOO	THE RELATIVISTIC IRON LINE - QPO CONNECTION IN GRS 1915+105	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402071010/	Quick Look
320	VELA PWN NE2	130.6211	-44.2844	130.186671	-44.103918	154.655956	-58.950029	263.6136326	-1.23809583	141.8635	55917.0080439815	2011-12-22 00:11:35	55917.6126273148	2011-12-22 14:42:11	506042010	18.514	15	18.538	18.514	0	18.514	2	2	0	2	1	0	0	16.8755	16.8755	52.2259	0	PROCESSED	57604.2062962963	2016-08-04 04:57:04	56305	2013-01-13 00:00:00	55937.7869212963	2012-01-11 18:53:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	C	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506042010/	Quick Look
321	SGR C BGD	265.7856	-29.8854	264.98542	-29.862996	266.313646	-6.498142	358.90876565	-0.03691694	81.9998	53789.4522106482	2006-02-23 10:51:11	53789.8349421296	2006-02-23 20:02:19	500019010	13.3073	10	13.3153	13.3153	13.3153	13.3073	2	2	2	2	1	0	0	12.2404	12.2404	33.0639	0	PROCESSED	57533.050462963	2016-05-25 01:12:40	54247	2007-05-27 00:00:00	54041.3629166667	2006-11-02 08:42:36	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001079	We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI MURAKAMI		JAP	0	SWG	FOSSILS OF THE GALACTIC CENTER ACTIVITY	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500019010/	Quick Look
322	1H 0707-495	107.1586	-49.5558	106.829982	-49.474426	125.752559	-70.871973	260.16951247	-17.68246857	144.7199	53707.1759143518	2005-12-03 04:13:19	53710.0974537037	2005-12-06 02:20:20	700008010	97.2291	100	97.8529	100.3891	97.2291	97.8149	4	2	4	4	1	0	0	91.8008	91.8008	252.3688	4	PROCESSED	57532.4288194444	2016-05-24 10:17:30	54247	2007-05-27 00:00:00	54059.7078472222	2006-11-20 16:59:18	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001040	We propose a 100 ks observation of the NLS1 1H 0707--495 in order to understand its remarkable and puzzling spectral and variability properties. The Suzaku data will help us to disentangle between the two interpretations adopted so far, namely partial covering and relativistically blurred reflection.	EXTRAGALACTIC COMPACT SOURCES	7	A	GIOVANNI MINIUTTI		JAP	0	SWG	THE EXTREME PROPERTIES OF THE NLS1 GALAXY 1H 0707-495	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700008010/	Quick Look
323	MRK 501	253.4335	39.8281	253.015349	39.90842	242.48193	61.693142	63.68387876	38.89139128	70.9919	54913.7775347222	2009-03-23 18:39:39	54915.3328587963	2009-03-25 07:59:19	703046010	72.3342	65	72.3342	72.3342	0	72.3342	2	2	0	2	1	0	0	64.8365	64.8365	134.3581	1	PROCESSED	57545.930462963	2016-06-06 22:19:52	55329	2010-05-13 00:00:00	54924.366724537	2009-04-03 08:48:05	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031343	We propose to observe two bright TeV blazars with Suzaku, in coordination with VERITAS and MAGIC at TeV energies. The primary objective is to make use of the recently available observational capabilities in collecting the much needed simultaneous X-ray and TeV data on these intriguing sources. The data will be essential for addressing a number of unresolved issues in the study of TeV blazars, such as spectral variability, X-ray/TeV correlation and associated time lags, spectral hysteresis, etc. The results will likely provide insights into the properties of the emitting particles, as well as those of the emitting regions, emission mechanism, composition of the jets, and acceleration energetics.	EXTRAGALACTIC COMPACT SOURCES	7	A	WEI CUI		USA	3	AO3	COORDINATED X-RAY/TEV OBSERVATIONS OF TEV BLAZARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703046010/	Quick Look
324	TAU SCO	248.9722	-28.2177	248.192662	-28.11602	251.449604	-6.120068	351.53437371	12.80599439	271.5181	54696.3145833333	2008-08-18 07:33:00	54696.6675810185	2008-08-18 16:01:19	403034050	16.3136	10	16.3504	16.3136	0	16.3584	1	1	0	1	1	0	0	13.967	13.967	30.472	0	PROCESSED	57543.3225694444	2016-06-04 07:44:30	55084	2009-09-10 00:00:00	54713.1924189815	2008-09-04 04:37:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031121	We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars.	GALACTIC POINT SOURCES	4	A	RICHARD IGNACE		USA	3	AO3	X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403034050/	Quick Look
325	CENTAURUS X-3	170.3244	-60.5721	169.768632	-60.297812	209.195093	-56.294338	292.07802241	0.38603209	97.3521	54808.2886111111	2008-12-08 06:55:36	54810.2085532407	2008-12-10 05:00:19	403046010	97.5871	90	97.5871	97.5871	0	97.5871	2	2	0	2	1	0	0	79.6562	79.6562	165.8537	0	PROCESSED	57544.7036805556	2016-06-05 16:53:18	55188	2009-12-23 00:00:00	54822.6243634259	2008-12-22 14:59:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031154	We ask for a 90 ks observation (which will be performed within typically 180 ks taking Suzaku's duty cycle into account) of the accreting HMXB Centaurus X-3 to conduct the most sensitive study to date of the wide range of changes of its broad band spectrum over one 2.1 binary orbit and with pulse phase. Especially we will determine the evolution of the hydrogen absorption column over the orbit and test whether signatures of the tidal wake observed with RXTE can be confirmed. The variable Fe line complex will be studied. The cyclotron resonance scattering feature of Cen X-3 at ~30 keV is especially well suited to test new physical models describing phase-resolved line profiles, since it is very variable over the pulse, with the line centroid spanning an energy range from 28 to 39 keV.	GALACTIC POINT SOURCES	4	A	KATJA POTTSCHMIDT		USA	3	AO3	THE BROAD BAND SPECTRUM OF CEN X-3 OVER ORBIT AND PULSE PHASE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403046010/	Quick Look
326	SS CYG	325.6842	43.5739	325.1931	43.344666	350.456739	52.648094	90.55430501	-7.12254626	256.8767	53692.6066203704	2005-11-18 14:33:32	53693.8646759259	2005-11-19 20:45:08	400007010	56.043	60	56.059	56.179	56.043	56.059	2	2	2	2	1	0	0	54.3572	54.3572	108.6658	2	PROCESSED	57528.0435763889	2016-05-20 01:02:45	54247	2007-05-27 00:00:00	54037.9128472222	2006-10-29 21:54:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001044	Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst.	GALACTIC POINT SOURCES	4	A	MANABU ISHIDA		JAP	0	SWG-TOO	SS CYG OBSERVATION IN OUTBURST	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400007010/	Quick Look
327	73P/SW3	17.9545	-9.1915	17.327695	-9.456837	12.929266	-15.523337	138.90931762	-71.42827213	59.4015	53893.8691666667	2006-06-07 20:51:36	53893.9356365741	2006-06-07 22:27:19	500014040	3.236	35	3.236	3.236	3.236	3.236	1	1	1	1	1	0	0	2.4909	2.4909	5.7359	0	PROCESSED	57534.5832407407	2016-05-26 13:59:52	54267	2007-06-16 00:00:00	54052.5308912037	2006-11-13 12:44:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014040/	Quick Look
328	CYG X-2	326.1609	38.3293	325.643028	38.098792	346.688554	47.972011	87.3271497	-11.30495752	51.1203	54648.0669097222	2008-07-01 01:36:21	54650.6154398148	2008-07-03 14:46:14	403063010	72.4308	100	102.6922	72.4308	0	89.8144	1	1	0	2	1	0	0	88.1331	88.1331	220.1678	0	PROCESSED	57527.0641319444	2016-05-19 01:32:21	55031	2009-07-19 00:00:00	54665.3170601852	2008-07-18 07:36:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031165	The nature of ultra-dense matter in neutron stars remains enigmatic. To probe this requires accurate neutron star radii and masses. We recently showed that broad iron lines in neutron star low-mass X-ray binaries (LMXBs) constrain the neutron star radius. LMXBs also provide us with another tool, kHz quasi-periodic oscillations (QPOs). Combining the inner disk velocity (from modeling the iron line) and the frequency of the kHz QPOs gives a method to measure the neutron star mass. We propose a 100 ks observation of Cyg X-2 with Suzaku to provide a detailed iron line profile. Combined with simultaneous observations with RXTE to determine the kHz QPO frequency, we will measure the neutron star mass. Cyg X-2 is the perfect test case as it already has a known mass from optical observations.	GALACTIC POINT SOURCES	4	B	EDWARD CACKETT		USA	3	AO3	MEASURING NEUTRON STAR MASSES USING BROAD IRON LINES AND KHZ QPOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403063010/	Quick Look
329	JUPITER	226.6157	-16.1957	225.916913	-16.003222	228.709072	1.245307	344.00356707	35.68981432	118.4907	53792.7940856482	2006-02-26 19:03:29	53793.8599421296	2006-02-27 20:38:19	401001030	40.7912	36	40.7992	40.7912	40.7992	40.7992	2	2	2	2	1	0	0	35.5363	35.5363	92.0739	0	PROCESSED	57533.1063078704	2016-05-25 02:33:05	54401	2007-10-28 00:00:00	53905.5868055556	2006-06-19 14:05:00	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011003	We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure.	GALACTIC POINT SOURCES	4	C	RONALD ELSNER		USA	1	AO1	JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001030/	Quick Look
330	4U 1608-52	243.1805	-52.3646	242.219607	-52.236867	251.312675	-30.647361	330.96698106	-0.80844416	94.0316	55270.6937615741	2010-03-15 16:39:01	55271.6668287037	2010-03-16 16:00:14	404044020	32.7181	30	32.7181	32.7261	0	32.7181	2	1	0	2	1	0	0	26.988	26.988	84.0558	1	PROCESSED	57550.9065277778	2016-06-11 21:45:24	55651	2011-03-31 00:00:00	55285.1175462963	2010-03-30 02:49:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041223	The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona.	GALACTIC POINT SOURCES	4	A	EDWARD CACKETT		USA	4	AO4-TOO	ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404044020/	Quick Look
331	BETA LYR	282.5094	33.3738	282.047614	33.314587	288.857821	55.998718	63.19462876	14.79594569	59.4704	53862.545474537	2006-05-07 13:05:29	53862.9952083333	2006-05-07 23:53:06	401036010	20.2515	20	20.2675	20.2515	20.2675	20.2675	2	2	2	2	1	0	0	9.8947	9.8947	38.8519	1	PROCESSED	57533.7394212963	2016-05-25 17:44:46	54401	2007-10-28 00:00:00	53913.8191550926	2006-06-27 19:39:35	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011031	The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse.	GALACTIC POINT SOURCES	4	A	RICHARD IGNACE		USA	1	AO1	AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036010/	Quick Look
332	BETA LYR	282.5093	33.3719	282.047501	33.312687	288.85715	55.996853	63.19278609	14.79528012	53.4973	53871.4311226852	2006-05-16 10:20:49	53871.8571875	2006-05-16 20:34:21	401036030	18.1954	20	18.1954	18.1954	18.1954	18.1954	2	2	2	2	1	0	0	19.8421	19.8421	36.8079	0	PROCESSED	57534.3160532407	2016-05-26 07:35:07	54401	2007-10-28 00:00:00	53920.4164351852	2006-07-04 09:59:40	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011031	The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse.	GALACTIC POINT SOURCES	4	A	RICHARD IGNACE		USA	1	AO1	AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036030/	Quick Look
333	SKY_50.0_-62.4	50.0507	-62.4328	49.819854	-62.612067	354.772614	-72.643934	278.67600391	-47.08169247	281.591	53795.7055671296	2006-03-01 16:56:01	53796.9369675926	2006-03-02 22:29:14	501001010	80.145	80	80.153	80.145	80.153	80.145	2	2	2	2	1	0	0	74.0122	74.0122	106.376	0	PROCESSED	57533.1282638889	2016-05-25 03:04:42	54401	2007-10-28 00:00:00	53905.6164930556	2006-06-19 14:47:45	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011252	We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble.	GALACTIC DIFFUSE EMISSION	5	A	ROBIN SHELTON		USA	1	AO1	SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501001010/	Quick Look
334	PSR B1259-63	195.6931	-63.8349	194.903784	-63.566278	227.685916	-50.892951	304.18120501	-0.9906484	99.8696	55566.8369212963	2011-01-05 20:05:10	55569.3959722222	2011-01-08 09:30:12	405037010	90.0407	80	90.0407	90.0407	0	90.0407	2	2	0	2	1	0	0	74.4506	74.4506	221.0618	1	PROCESSED	57600.639375	2016-07-31 15:20:42	55961	2012-02-04 00:00:00	55595.2642939815	2011-02-03 06:20:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051221	We propose to observe a gamma-ray binary PSR B1259-63 during the pulsar's second disk crossing after periastron passage. PSR B1259-63 is a young radio pulsar orbiting around a B2e star with a highly eccentric 3.4 yr orbit. Suzaku XIS+HXD measurements of the hard continuum emission from the binary system allow us to investigate particle acceleration in a highly variable environment as a result of interactions between the relativistic wind of the pulsar and the circumstellar disk of the Be star. With the advent of the Fermi Gamma-ray Space Telescope, we will be able to simultaneously observe X-rays and GeV gamma-rays during the disk transit for the first time. The observations of PSR B1259-63 will give us a unique opportunity to study the physics of pulsar winds on AU-scale.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		USA	5	AO5	SUZAKU BROADBAND OBSERVATIONS OF A GAMMA-RAY BINARY PSRB1259-63 DURING THE POST-PERIASTRON FLARE IN 2011	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405037010/	Quick Look
335	4U 1728-34	262.9799	-33.9051	262.153704	-33.869072	264.067005	-10.60817	354.23908298	-0.18221646	278.0266	55473.517349537	2010-10-04 12:24:59	55475.6876967593	2010-10-06 16:30:17	405048010	50.5472	100	50.6522	50.5472	0	50.6522	2	2	0	2	1	0	0	95.3606	95.3606	187.4678	3	PROCESSED	57553.6884490741	2016-06-14 16:31:22	55867	2011-11-02 00:00:00	55487.4662615741	2010-10-18 11:11:25	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051244	Fe K-alpha lines have been detected in ten NS-LMXBs. Under the commonly accepted interpretation, they can be used to set tight constrains on the accretion disk geometry. 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 kHz QPOs. We have recently shown that simultaneous measurements of Fe lines and kHz QPOs in a NS-LMXB appear to contradict this picture. We propose to observe 4U 1728-34 with Suzaku five times for 20 ks, simultaneously with RXTE and ATCA. This program will allow us to study and compare the dynamics of the inner edge of the disk as inferred from the Fe line and the kHz QPOs, as well as the relation of both observables with the jet radio emission.	GALACTIC POINT SOURCES	4	A	MANUEL LINARES		USA	5	AO5	ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405048010/	Quick Look
336	4U 1636-536	250.2272	-53.754	249.230789	-53.657507	256.461332	-31.236669	332.91133194	-4.81789372	91.2454	54160.0424421296	2007-03-01 01:01:07	54160.8931597222	2007-03-01 21:26:09	401050030	38.7193	38	38.7274	38.7193	0	38.7194	2	1	0	2	1	0	0	48.1459	48.1459	73.498	1	PROCESSED	57537.5161111111	2016-05-29 12:23:12	54695	2008-08-17 00:00:00	54167.6400462963	2007-03-08 15:21:40	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011117	Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.	GALACTIC POINT SOURCES	4	A	JEROEN HOMAN		USA	1	AO1	THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050030/	Quick Look
337	SWIFTJ2000.6+3210	300.1137	32.1218	299.624092	31.983158	312.678705	51.196511	68.93835501	1.08211502	255.6072	54039.0205671296	2006-10-31 00:29:37	54039.3029976852	2006-10-31 07:16:19	401053020	12.7484	10	12.7564	12.7484	12.7564	12.7564	2	2	2	2	1	0	0	11.727	11.727	24.3939	0	PROCESSED	57535.9859490741	2016-05-27 23:39:46	54775	2008-11-05 00:00:00	54056.1959953704	2006-11-17 04:42:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011132	INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	1	AO1	HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401053020/	Quick Look
338	HD162020	267.6661	-40.3245	266.789333	-40.311026	268.130752	-16.898333	350.73610578	-6.73339029	259.9986	55833.0255208333	2011-09-29 00:36:45	55833.4279513889	2011-09-29 10:16:15	406037040	16.7297	15	16.7377	16.7377	0	16.7297	1	1	0	1	1	0	0	15.7286	15.7286	34.7499	0	PROCESSED	57603.2728356482	2016-08-03 06:32:53	56225	2012-10-25 00:00:00	55858.1397453704	2011-10-24 03:21:14	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061202	Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction.	GALACTIC POINT SOURCES	4	A	IGNAZIO PILLITTERI		USA	6	AO6	STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS.	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406037040/	Quick Look
339	CH CYG	291.1621	50.2424	290.833167	50.142645	313.7082	70.490137	81.86550652	15.56609243	185.7481	53739.5736458333	2006-01-04 13:46:03	53740.2919560185	2006-01-05 07:00:25	400016020	33.3058	25	33.3075	33.3378	33.3155	33.3058	2	2	2	2	1	0	0	28.4615	28.4615	62.056	1	PROCESSED	57532.6355902778	2016-05-24 15:15:15	54247	2007-05-27 00:00:00	54039.6712268518	2006-10-31 16:06:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001082	CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS.	GALACTIC POINT SOURCES	4	A	KOJI MUKAI		JAP	0	SWG	SUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNI	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400016020/	Quick Look
340	ETA CARINAE	161.2181	-59.7282	160.732192	-59.464935	202.181916	-58.969104	287.59637986	-0.67920855	289.0006	54274.2459259259	2007-06-23 05:54:08	54275.9015509259	2007-06-24 21:38:14	402039010	58.3961	50	58.4041	58.3961	0	58.4041	2	2	0	2	1	0	0	51.552	51.552	143.0099	1	PROCESSED	57539.0368981482	2016-05-31 00:53:08	54695	2008-08-17 00:00:00	54322.5140856482	2007-08-10 12:20:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021026	XMM-Newton observations in 2003 suggest that X-ray emission from Eta Carinae has a hard X-ray component above 10 keV in addition to the thermal emission with kT ~3-5 keV. The excess is apparently strongest near the 2-10 keV X-ray maximum, and possibly produced by very hot plasma or 1st-order Fermi acceleration of particles which then inverse Compton-upscatter UV seed photons from the stellar photospheres. We propose a 50 ksec observation of Eta Carinae with the Suzaku telescope during AO2, compare the X-ray spectrum with earlier observations and determine the level of emission at E >9 keV.	GALACTIC POINT SOURCES	4	B	KENJI HAMAGUCHI		USA	2	AO2	HARD X-RAY EMISSION FROM ETA CARINAE	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402039010/	Quick Look
341	SNR G93.3+6.9 S2	312.6887	55.4958	312.345372	55.307685	351.959804	67.182569	93.24230604	7.18061007	40.0056	53905.9701736111	2006-06-19 23:17:03	53906.4293865741	2006-06-20 10:18:19	501081010	16.0092	15	16.0352	16.0272	16.0092	16.0352	2	2	2	2	1	0	0	18.3757	18.3757	39.6679	1	PROCESSED	57534.7256134259	2016-05-26 17:24:53	54401	2007-10-28 00:00:00	53927.314537037	2006-07-11 07:32:56	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501081010/	Quick Look
342	GX17+2	274.0087	-14.1006	273.298097	-14.118345	273.929719	9.285377	16.37694194	1.24456043	269.7113	54362.2773032407	2007-09-19 06:39:19	54362.8543402778	2007-09-19 20:30:15	402050010	19.0959	20	19.0959	19.1044	0	19.0959	2	1	0	2	1	0	0	16.0445	16.0445	49.8499	0	PROCESSED	57540.0136458333	2016-06-01 00:19:39	54751	2008-10-12 00:00:00	54384.4487037037	2007-10-11 10:46:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021111	Z sources are bright low-mass X-ray binaries with variable spectra that describe a characteristic "Z" shape in an X-ray color-color plot. The forces driving the spectral shape and variability of the Z sources are not well understood, as there are few detectors with the necessary capabilities. GX17+2 is a Sco-type Z sources with an unusual time-varying hard X-ray tail whose origin is uncertain. Bright X-ray sources also illuminate the interstellar medium. Highly absorbed X-ray sources show halos due to dust scattering as well as absorption features. These will allow us to place constraints on interstellar dust and gas models. Suzaku can address all of these issues with simultaneous observations of the hard X-ray continuum and the dust-scattered X-ray halo.	GALACTIC POINT SOURCES	4	A	RANDALL SMITH		USA	2	AO2	OBSERVING THE SPECTRUM AND HALO OF GX17+2	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402050010/	Quick Look
343	A 0535+26	84.7195	26.3786	83.941618	26.351102	85.26575	3.024576	181.38803208	-2.61609461	86.1856	55067.9626273148	2009-08-24 23:06:11	55069.1599421296	2009-08-26 03:50:19	404054010	51.8668	45	51.8706	51.8706	0	51.8668	2	2	0	2	1	0	0	42.078	42.078	103.4298	1	PROCESSED	57548.3667708333	2016-06-09 08:48:09	55448	2010-09-09 00:00:00	55078.219837963	2009-09-04 05:16:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041232	We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku's AO-4. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line(s) in this system and to constrain its broad band spectrum.	GALACTIC POINT SOURCES	4	A	KATJA POTTSCHMIDT		USA	4	AO4-TOO	CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404054010/	Quick Look
344	PUP A : SE	126.0128	-43.1802	125.58355	-43.01733	147.904142	-59.590498	260.74447692	-3.25911558	277.1832	53843.3098842593	2006-04-18 07:26:14	53843.8328009259	2006-04-18 19:59:14	501089010	29.7493	30	29.7493	29.8172	29.7652	29.7612	4	2	4	4	1	0	0	22.8867	22.8867	45.174	0	PROCESSED	57533.5119675926	2016-05-25 12:17:14	54401	2007-10-28 00:00:00	53907.001412037	2006-06-21 00:02:02	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501089010/	Quick Look
345	AQL X-1	287.816	0.5784	287.177723	0.494688	289.376856	22.828471	35.71219982	-4.14539755	284.0925	54371.6493402778	2007-09-28 15:35:03	54372.062662037	2007-09-29 01:30:14	402053010	13.8252	15	13.8252	13.8252	0	13.8252	2	1	0	2	1	0	0	13.745	13.745	35.704	0	PROCESSED	57540.1327199074	2016-06-01 03:11:07	54769	2008-10-30 00:00:00	54402.3541550926	2007-10-29 08:29:59	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021114	We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data.	GALACTIC POINT SOURCES	4	A	RONALD REMILLARD		USA	2	AO2-TOO	X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402053010/	Quick Look
346	4U 0115+63	19.6139	63.7554	18.78861	63.492562	49.805717	49.807631	125.91367385	1.04017806	82.1235	55750.053587963	2011-07-08 01:17:10	55751.0210763889	2011-07-09 00:30:21	406049010	42.2748	45	42.2748	42.3548	0	42.3548	2	2	0	2	1	0	0	42.1432	42.1432	83.5779	1	PROCESSED	57602.5577662037	2016-08-02 13:23:11	56163	2012-08-24 00:00:00	55778.4311226852	2011-08-05 10:20:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061234	We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma.	GALACTIC POINT SOURCES	4	A	KATJA POTTSCHMIDT		USA	6	AO6-TOO	CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406049010/	Quick Look
347	2S 0921-630	140.6632	-63.3	140.373022	-63.085068	195.142403	-68.892754	281.84517925	-9.33739383	20.5636	54340.7614351852	2007-08-28 18:16:28	54341.8335532407	2007-08-29 20:00:19	402057010	43.2131	40	43.2131	43.2211	0	43.2211	2	2	0	2	1	0	0	15.8568	15.8568	92.6158	0	PROCESSED	57539.9304976852	2016-05-31 22:19:55	54721	2008-09-12 00:00:00	54353.4365625	2007-09-10 10:28:39	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021118	2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum.	GALACTIC POINT SOURCES	4	A	JEAN COTTAM		USA	2	AO2	PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402057010/	Quick Look
348	HEN 3-1591	271.8863	-25.8981	271.110376	-25.90538	271.688765	-2.468309	5.07192211	-2.68044312	269.6421	56203.7249537037	2012-10-03 17:23:56	56204.7793981482	2012-10-04 18:42:20	407042010	51.3876	50	51.3877	51.3876	0	51.4036	4	3	0	3	1	0	0	52.3681	52.3681	91.0959	1	PROCESSED	57607.2899884259	2016-08-07 06:57:35	56592	2013-10-27 00:00:00	56226.5545601852	2012-10-26 13:18:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071211	The number of symbiotic stars known to be medium energy (2-10 keV) X-ray emitters has increased markedly in the last several years. These are white dwarfs accreting from a giant mass donor, unlike the less common class of symbiotic X-ray binaries in which the accretor is a neutron star. The X-ray spectra of the white dwarf symbiotics can be used to constrain the white dwarf mass and accretion rate. Here we focus on one object, Hen 3-1591, which belongs to a rare subclass of d'-type yellow symbiotic, commonly thought to harbor a young white dwarf. Hen 3-1591 is the first of this subclass to show medium energy X-ray emission, and hence we propose a moderately deep Suzaku observation to characterize its white dwarf and the circum-binary environment.	GALACTIC POINT SOURCES	4	B	KOJI MUKAI		USA	7	AO7	THE X-RAY EMISSION OF THE YELLOW SYMBIOTIC STAR, HEN 3-1591	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407042010/	Quick Look
349	NGC 5506	213.3121	-3.2119	212.6632	-2.97838	212.190756	9.596557	339.14659218	53.80640928	287.3747	53958.1015972222	2006-08-11 02:26:18	53959.4488425926	2006-08-12 10:46:20	701030020	53.2962	63	53.3042	53.2962	53.3042	53.3042	2	2	2	2	1	0	0	47.9832	47.9832	116.386	1	PROCESSED	57535.2817476852	2016-05-27 06:45:43	54695	2008-08-17 00:00:00	54116.3307291667	2007-01-16 07:56:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011312	NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	A	TRACEY TURNER		USA	1	AO1	SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030020/	Quick Look
350	MBM12 OFF-CLOUD	41.3205	18.3346	40.61976	18.124407	44.482795	2.251416	157.33933963	-36.81758445	247.4802	53772.648599537	2006-02-06 15:33:59	53774.618275463	2006-02-08 14:50:19	501104010	75.3292	70	75.3372	75.3292	75.3372	75.3372	2	2	2	2	1	0	0	67.769	67.769	170.1159	1	PROCESSED	57532.9691550926	2016-05-24 23:15:35	54401	2007-10-28 00:00:00	53905.9757523148	2006-06-19 23:25:05	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011262	Suzaku will observe MBM 12, a nearby molecular cloud which shadows all but the most local soft X-ray emission. The goal of that observation is to measure the O VII and O VIII emission from the Local Hot Bubble, taking advantage of Suzaku's low energy sensitivity and low background. In light of this, we propose to observe the diffuse background near the MBM 12 position. This will: (1) Measure the O VII and O VIII emission from the Galactic disk and halo, after subtracting the local emission, and (2) confirm that this background emission does not contaminate the initial observation. The absolute measure of the strength of the O VII line, as well as the O VIII/O VII ratio, is essential to understanding the origin of the Galactic component to the 3/4 keV diffuse emission.	GALACTIC DIFFUSE EMISSION	5	B	RANDALL SMITH		USA	1	AO1	THE ORIGIN OF THE GALACTIC DIFFUSE 3/4 KEV X-RAY BACKGROUND	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501104010/	Quick Look
351	CYGNUS X-1	299.5969	35.1891	299.126785	35.052601	313.664382	54.235906	71.32710759	3.05572664	254.8701	56231.3416782407	2012-10-31 08:12:01	56232.109212963	2012-11-01 02:37:16	407072010	0.3726	30	1.9394	1.9908	0	0.3726	1	1	0	1	1	0	0	30.0857	30.0857	66.3059	0	PROCESSED	57607.9427430556	2016-08-07 22:37:33	56611	2013-11-15 00:00:00	56245.5107407407	2012-11-14 12:15:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071241	We propose for a single 30 ks observation of the accreting black hole Cygnus X-1. NuSTAR is an upcoming (to be launched in Spring 2012) hard X-ray (5-80 keV) mission that will plan its schedule to obtain simultaneous coverage of Cyg X-1 with Suzaku. The observations will be used for both science and cross-calibration. The combination of Suzaku and NuSTAR will provide the best measurement of the reflection component, including a relativistically broadened iron line and a hard X-ray excess, and the information will be used to test emission models and constrain the Cyg X-1 accretion geometry. The XIS capabilities to measure the iron line are essential for the science, and the HXD coverage is essential for the cross-calibration.	GALACTIC POINT SOURCES	4	A	JOHN TOMSICK		USA	7	AO7	CYGNUS X-1 WITH SUZAKU AND NUSTAR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407072010/	Quick Look
352	MRK 766	184.6147	29.8197	183.986078	30.097268	171.204802	28.944359	190.62410896	82.27145087	134.9989	54421.893287037	2007-11-17 21:26:20	54423.2363310185	2007-11-19 05:40:19	701035020	59.3635	50	59.3635	59.3635	0	59.3635	1	1	0	1	1	0	0	51.1517	51.1517	116.0238	1	PROCESSED	57540.5762384259	2016-06-01 13:49:47	54800	2008-11-30 00:00:00	54433.2716666667	2007-11-29 06:31:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011328	X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components	EXTRAGALACTIC COMPACT SOURCES	7	B	TRACEY TURNER		USA	1	AO1	DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701035020/	Quick Look
353	TAU SCO	248.9729	-28.218	248.19336	-28.116323	251.450261	-6.120276	351.53455344	12.80533126	274.2608	54703.1981597222	2008-08-25 04:45:21	54703.5447222222	2008-08-25 13:04:24	403034060	15.0183	10	15.0263	15.0343	0	15.0183	1	1	0	1	1	0	0	12.9049	12.9049	29.9119	0	PROCESSED	57543.3841898148	2016-06-04 09:13:14	55084	2009-09-10 00:00:00	54713.2754976852	2008-09-04 06:36:43	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031121	We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars.	GALACTIC POINT SOURCES	4	A	RICHARD IGNACE		USA	3	AO3	X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403034060/	Quick Look
354	COMET_8P_TUTTLE-P2_01	39.6412	-35.6843	39.127956	-35.899537	21.259605	-47.847912	240.18300744	-65.68930545	257.5577	54490.0082291667	2008-01-25 00:11:51	54490.1627083333	2008-01-25 03:54:18	502063010	4.3468	5	4.3468	4.3468	0	4.3468	2	2	0	2	1	0	0	4.4029	4.4029	13.3279	1	PROCESSED	57541.3739236111	2016-06-02 08:58:27	54912	2009-03-22 00:00:00	54546.0974189815	2008-03-21 02:20:17	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063010/	Quick Look
355	GX 301-2	186.5611	-62.8021	185.862176	-62.525248	221.491572	-52.675278	300.05773343	-0.07103063	326.712	54703.5522800926	2008-08-25 13:15:17	54704.0036689815	2008-08-26 00:05:17	403044010	11.4275	60	11.4292	11.4306	0	11.4275	2	2	0	2	1	0	0	10.7148	10.7148	38.9939	0	PROCESSED	57543.3977546296	2016-06-04 09:32:46	55218	2010-01-22 00:00:00	54720.435462963	2008-09-11 10:27:04	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031152	We propose the first observation of the bright neutron star GX 301-2 with Suzaku. The aim of the proposed 60 ks observation is a study of the broadband spectrum of the source in unprecedented detail and quality. This will allow us to analyze the structure (including density and clumpiness) of the intense wind of the optical companion and the gas stream flowing from Wray 977 to the neutron star. Spectral data will be used to study the evolution of nH and the iron line with very high time resolution. Furthermore, we will perform phase resolved spectroscopy to study the spectral variation of the cyclotron line with pulse phase.	GALACTIC POINT SOURCES	4	A	RICHARD ROTHSCHILD		USA	3	AO3	BROAD-BAND STUDY OF GX 301-2	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403044010/	Quick Look
356	COMET_8P_TUTTLE-P2_06	39.9457	-36.3936	39.436659	-36.607889	21.099638	-48.591179	241.70384829	-65.28238509	258.0349	54490.6963773148	2008-01-25 16:42:47	54490.8293287037	2008-01-25 19:54:14	502063060	6.6904	6.7	6.6906	6.6906	0	6.6904	1	1	0	1	1	0	0	4.338	4.338	11.4799	0	PROCESSED	57541.3927893518	2016-06-02 09:25:37	54912	2009-03-22 00:00:00	54546.1201736111	2008-03-21 02:53:03	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063060/	Quick Look
357	ETA CARINAE	161.2819	-59.6866	160.795238	-59.423234	202.165647	-58.917186	287.60543966	-0.62739972	356.4874	56894.0150810185	2014-08-25 00:21:43	56894.6884375	2014-08-25 16:31:21	409027010	34.5098	30	34.5098	34.5256	0	34.5258	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.5156712963	2016-08-16 12:22:34	57285	2015-09-20 00:00:00	56910.6449884259	2014-09-10 15:28:47	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091202	Eta Carinae is an extremely massive binary system whose strong winds produce a variety of high-energy X-ray and possibly gamma-ray emission. Earlier XMM-Newton, Suzaku and INTEGRAL observations found interesting features in the extremely hard X-ray band: i) a flat spectral component above 9 keV toward the flux maximum; ii) strong 15-20 keV emission during an occultation of the wind-wind colliding plasma; iii) stable power-law emission above 25 keV. These features are signs of the highest energy processes yet detected in any colliding wind binary. Broad band X-ray observations around periastron are essential to understanding those features. We therefore propose Suzaku observations at 5 key phases around the next periastron passage of eta Carinae in 2014.6.	GALACTIC POINT SOURCES	4	A	KENJI HAMAGUCHI		USA	9	AO9	PROBING THE HIGHEST ENERGY PHENOMENA OF ETA CARINAE AROUND PERIASTRON IN 2014	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409027010/	Quick Look
358	G332.5-5.6 NE	251.0925	-54.3783	250.085838	-54.28574	257.162856	-31.775018	332.77088512	-5.61037777	77.916	54504.4521296296	2008-02-08 10:51:04	54505.6669444444	2008-02-09 16:00:24	502067010	71.1926	80	71.2006	71.2086	0	71.1926	2	2	0	2	1	0	0	65.2508	65.2508	104.9418	0	PROCESSED	57541.5340277778	2016-06-02 12:49:00	54883	2009-02-21 00:00:00	54515.6965509259	2008-02-19 16:43:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021216	We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova.	GALACTIC DIFFUSE EMISSION	5	B	STEPHEN REYNOLDS		USA	2	AO2	G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502067010/	Quick Look
359	HD6903	17.4507	19.662	16.780979	19.395948	23.622213	11.325445	128.84764567	-42.9987034	70.0004	55031.3824305556	2009-07-19 09:10:42	55032.3578703704	2009-07-20 08:35:20	404034010	36.8135	35	36.8295	36.8135	0	36.8215	2	2	0	2	1	0	0	29.6727	29.6727	84.2639	0	PROCESSED	57547.8823958333	2016-06-08 21:10:39	55419	2010-08-11 00:00:00	55048.3029976852	2009-08-05 07:16:19	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041201	Suzaku XIS spectra of two G0 III Hertzsprung gap giants will complete a multi-observatory survey of the anomalous coronal behavior of this "X-ray deficient" class. The abrupt rise in coronal luminosities from the warmer giants to their cooler cousins, only slightly further advanced in evolution, might signal disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. Key discriminators are the coronal energy distribution, composition (FIP bias), and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution, and both have supporting HST UV spectra. Expanding the high energy sample of this key class of objects is essential for probing their contrary, but perhaps deeply significant, behavior.	GALACTIC POINT SOURCES	4	B	THOMAS AYRES		USA	4	AO4	ANOMALOUS CORONAE IN THE MIDST OF THE HERTZSPRUNG GAP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404034010/	Quick Look
360	GS 2023+338	306.0444	33.8015	305.554336	33.638661	321.046576	51.052001	73.0785131	-2.14854563	252.4521	55142.9636805556	2009-11-07 23:07:42	55144.0550810185	2009-11-09 01:19:19	404059010	42.3246	40	42.3486	42.3246	0	42.3566	2	2	0	2	1	0	0	29.1404	29.1404	94.2839	1	PROCESSED	57549.1887384259	2016-06-10 04:31:47	55531	2010-12-01 00:00:00	55155.1065625	2009-11-20 02:33:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041243	The quiescent state is the dominant accretion mode for black holes on all mass scales. Our knowledge of the X-ray spectrum is limited due to the characteristic low luminosity in this state. Here, we propose a 40 ks observation of the most luminous quiescent stellar mass black hole GS 2023+338 (V404 Cyg). These observations will allow us to detect hard X-ray emission from a quiescent stellar mass black hole for the first time, providing unique contraints on the nature of the accretion flow in this low luminosity state.	GALACTIC POINT SOURCES	4	B	MARK REYNOLDS		USA	4	AO4	CONSTRAINING THE QUIESCENT ACCRETION FLOW AROUND A BLACK HOLE WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404059010/	Quick Look
361	ETA CARINAE	161.2814	-59.6826	160.794718	-59.419235	202.159659	-58.914636	287.60335194	-0.62397837	335.8837	56875.8359259259	2014-08-06 20:03:44	56876.6961111111	2014-08-07 16:42:24	409028010	21.5455	30	21.5455	21.5455	0	21.5455	2	2	0	2	1	0	0	9.9582	9.9582	22.028	0	PROCESSED	57616.4668518518	2016-08-16 11:12:16	57264	2015-08-30 00:00:00	56898.441875	2014-08-29 10:36:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091202	Eta Carinae is an extremely massive binary system whose strong winds produce a variety of high-energy X-ray and possibly gamma-ray emission. Earlier XMM-Newton, Suzaku and INTEGRAL observations found interesting features in the extremely hard X-ray band: i) a flat spectral component above 9 keV toward the flux maximum; ii) strong 15-20 keV emission during an occultation of the wind-wind colliding plasma; iii) stable power-law emission above 25 keV. These features are signs of the highest energy processes yet detected in any colliding wind binary. Broad band X-ray observations around periastron are essential to understanding those features. We therefore propose Suzaku observations at 5 key phases around the next periastron passage of eta Carinae in 2014.6.	GALACTIC POINT SOURCES	4	A	KENJI HAMAGUCHI		USA	9	AO9	PROBING THE HIGHEST ENERGY PHENOMENA OF ETA CARINAE AROUND PERIASTRON IN 2014	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409028010/	Quick Look
362	IGR J14536-5522	223.4257	-55.3573	222.511349	-55.15352	238.942519	-36.822348	319.76650903	3.46705373	279.1547	56870.9840277778	2014-08-01 23:37:00	56872.0398263889	2014-08-03 00:57:21	409031010	38.8825	40	38.8825	38.8905	0	38.8905	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.4455902778	2016-08-16 10:41:39	57270	2015-09-05 00:00:00	56902.7225231482	2014-09-02 17:20:26	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091211	Cataclysmic variables (CVs) detected in the INTEGRAL and Swift BAT hard X-ray surveys are predominantly magnetic systems of the intermediate polar subtype. However, as the survey sensitivity improves, an increasing number of polars are also detected as hard X-ray sources, even though the majority of polars are soft X-ray bright and hard X-ray faint. Over the long term, we hope to understand why most polars are soft X-ray dominated, and why a subset is hard X-ray bright. Here we propose Suzaku observations of four poorly studied BAT-detected polars, 1RXS J032540.0-081442, Swift J2319.4+2619, IW Eri, and IGR J14536-5522, supported by ground-based observations including optical polarimetry, to determine their system parameters.	GALACTIC POINT SOURCES	4	A	KOJI MUKAI		USA	9	AO9	HARD X-RAY BRIGHT POLARS: WHY ARE THEY DIFFERENT?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409031010/	Quick Look
363	CEP X-4	324.858	56.9961	324.464066	56.769041	5.88583	63.403956	99.01064753	3.3270936	51.1039	56826.8679282407	2014-06-18 20:49:49	56828.0363541667	2014-06-20 00:52:21	409037010	29.7647	50	29.7647	50.4597	0	30.9332	2	3	0	2	1	0	0	53.3133	53.3133	100.9358	1	PROCESSED	57615.3130671296	2016-08-15 07:30:49	57206	2015-07-03 00:00:00	56839.8053240741	2014-07-01 19:19:40	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091232	We propose to perform Target of Opportunity observations of two accreting neutron stars that are known cyclotron line sources, out of a sample of five, in outburst. The aim is to observe the sources for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma.	GALACTIC POINT SOURCES	4	A	FELIX FUERST		USA	9	AO9-TOO	CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409037010/	Quick Look
364	4U 1608-52	243.1735	-52.4241	242.21194	-52.296335	251.322253	-30.70644	330.92310685	-0.84886634	127.9983	55277.989849537	2010-03-22 23:45:23	55278.9140393518	2010-03-23 21:56:13	404044040	16.0728	30	16.0728	16.0728	0	16.0728	3	3	0	3	1	0	0	15.6557	15.6557	79.8439	2	PROCESSED	57550.9805439815	2016-06-11 23:31:59	55665	2011-04-14 00:00:00	55299.4128819444	2010-04-13 09:54:33	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041223	The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona.	GALACTIC POINT SOURCES	4	A	EDWARD CACKETT		USA	4	AO4-TOO	ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404044040/	Quick Look
365	HESS J1804-216	271.1693	-21.6722	270.417896	-21.676057	271.077547	1.764239	8.44223916	-0.04647489	89.0483	53831.6120138889	2006-04-06 14:41:18	53832.4919328704	2006-04-07 11:48:23	500007010	37.5222	50	37.5222	37.5222	37.5222	37.5222	2	2	2	2	1	0	0	28.9336	28.9336	75.9901	0	PROCESSED	57533.4045138889	2016-05-25 09:42:30	54247	2007-05-27 00:00:00	54042.288900463	2006-11-03 06:56:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001029	HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	0	SWG	SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS''	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500007010/	Quick Look
366	HESS J1804-216 BGD	270.9564	-22.0176	270.203045	-22.020418	270.877317	1.420312	8.04431311	-0.04388906	89.2004	53832.4925462963	2006-04-07 11:49:16	53833.454375	2006-04-08 10:54:18	500008010	40.7171	50	40.7171	40.7171	40.7171	40.7171	2	2	2	2	1	0	0	30.6429	30.6429	83.0879	1	PROCESSED	57533.4349537037	2016-05-25 10:26:20	54247	2007-05-27 00:00:00	54056.4266666667	2006-11-17 10:14:24	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001029	HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators.	GALACTIC DIFFUSE EMISSION	5	A	AYA BAMBA		JAP	0	SWG	SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS''	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500008010/	Quick Look
367	RXJ_0852-4622_NW	132.2926	-45.6157	131.862494	-45.429101	157.976747	-59.482382	265.39238743	-1.14402175	137.763	53723.4478240741	2005-12-19 10:44:52	53727.3016666667	2005-12-23 07:14:24	500010010	175.453	150	175.453	175.525	175.4608	175.461	2	2	2	2	1	0	0	230.0025	230.0025	332.9437	7	PROCESSED	57532.5654513889	2016-05-24 13:34:15	54247	2007-05-27 00:00:00	54059.902662037	2006-11-20 21:39:50	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001048	We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		JAP	0	SWG	HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500010010/	Quick Look
368	SMC DIFFUSE 1	13.0188	-72.8206	12.579325	-73.092182	312.037754	-64.558836	302.86615918	-44.30756989	221.6864	53687.4452893518	2005-11-13 10:41:13	53688.2231944445	2005-11-14 05:21:24	500011010	46.7789	50	46.7789	46.7869	46.7869	46.7869	1	1	1	1	1	0	0	47.8684	47.8684	67.1999	0	PROCESSED	57527.967337963	2016-05-19 23:12:58	54247	2007-05-27 00:00:00	54038.3531712963	2006-10-30 08:28:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001049	We propose to use Suzaku XIS to observe regions of diffuse emission in the Magellanic Clouds. The diffuse component was identified by ROSAT PSPC observations, but has never been studied with a true spectroscopic instrument. Suzaku is well-matched to the angular size and expected temperature of the regions of diffuse emission in the LMC. Not only will such observations give a clear view of the temperature structure of this gas, they will provide a direct measurement of ambient abundances in the Clouds.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		JAP	0	SWG	DIFFUSE EMISSION IN THE MAGELLANIC CLOUDS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500011010/	Quick Look
369	73P/SW3	18.4857	-9.3839	17.859598	-9.648443	13.351737	-15.906108	140.65827116	-71.47693301	59.4008	53893.6903703704	2006-06-07 16:34:08	53893.7356365741	2006-06-07 17:39:19	500014010	3.228	35	3.228	3.228	3.228	3.228	1	1	1	1	1	0	0	3.312	3.312	3.9039	0	PROCESSED	57534.5195486111	2016-05-26 12:28:09	54267	2007-06-16 00:00:00	54052.5070949074	2006-11-13 12:10:13	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014010/	Quick Look
370	73P/SW3	18.2949	-9.3163	17.668546	-9.581131	13.199293	-15.770045	140.03044964	-71.46265703	59.3979	53894.3358101852	2006-06-08 08:03:34	53894.4022800926	2006-06-08 09:39:17	500014110	1.4249	35	1.4249	1.4249	1.4249	1.4249	1	1	1	1	1	0	0	1.433	1.433	5.742	0	PROCESSED	57534.5994444445	2016-05-26 14:23:12	54267	2007-06-16 00:00:00	54052.5225694444	2006-11-13 12:32:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014110/	Quick Look
371	73P/SW3	18.4874	-9.3902	17.861309	-9.65474	13.350771	-15.912562	140.66879726	-71.4825298	59.4036	53894.6018055556	2006-06-08 14:26:36	53894.680775463	2006-06-08 16:20:19	500014150	3.232	35	3.232	3.232	3.232	3.232	1	1	1	1	1	0	0	3.293	3.293	6.8159	0	PROCESSED	57534.6057638889	2016-05-26 14:32:18	54267	2007-06-16 00:00:00	54052.5265509259	2006-11-13 12:38:14	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014150/	Quick Look
372	CYGNUS LOOP NE3	313.7583	32.1826	313.244151	31.990973	329.188805	47.043725	75.71932756	-8.27611719	222.9011	53703.7415162037	2005-11-29 17:47:47	53704.2355208333	2005-11-30 05:39:09	500022010	21.1338	20	21.1916	21.7199	21.1338	21.3599	2	2	2	2	1	0	0	20.2445	20.2445	42.6799	1	PROCESSED	57528.1127893518	2016-05-20 02:42:25	54247	2007-05-27 00:00:00	54038.7522106482	2006-10-30 18:03:11	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001093	We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI TSUNEMI		JAP	0	SWG	CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500022010/	Quick Look
373	PSR B1259-63	195.6913	-63.8356	194.901997	-63.566976	227.68559	-50.893989	304.18038114	-0.9913128	117.5773	55594.1927662037	2011-02-02 04:37:35	55594.4487731482	2011-02-02 10:46:14	405038010	21.4781	20	21.4941	21.4781	0	21.4941	1	1	0	1	1	0	0	15.6774	15.6774	22.1119	0	PROCESSED	57600.7966435185	2016-07-31 19:07:10	55974	2012-02-17 00:00:00	55607.1295601852	2011-02-15 03:06:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051221	We propose to observe a gamma-ray binary PSR B1259-63 during the pulsar's second disk crossing after periastron passage. PSR B1259-63 is a young radio pulsar orbiting around a B2e star with a highly eccentric 3.4 yr orbit. Suzaku XIS+HXD measurements of the hard continuum emission from the binary system allow us to investigate particle acceleration in a highly variable environment as a result of interactions between the relativistic wind of the pulsar and the circumstellar disk of the Be star. With the advent of the Fermi Gamma-ray Space Telescope, we will be able to simultaneously observe X-rays and GeV gamma-rays during the disk transit for the first time. The observations of PSR B1259-63 will give us a unique opportunity to study the physics of pulsar winds on AU-scale.	GALACTIC POINT SOURCES	4	A	YASUNOBU UCHIYAMA		USA	5	AO5	SUZAKU BROADBAND OBSERVATIONS OF A GAMMA-RAY BINARY PSRB1259-63 DURING THE POST-PERIASTRON FLARE IN 2011	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405038010/	Quick Look
374	3C 111	64.5741	38.0889	63.737568	37.967565	69.370671	16.452489	161.62276278	-8.7838332	81.5451	54700.4141898148	2008-08-22 09:56:26	54703.1836111111	2008-08-25 04:24:24	703034010	122.378	120	122.386	122.378	0	122.378	2	2	0	2	1	0	0	109.7067	109.7067	239.2517	1	PROCESSED	57543.4018287037	2016-06-04 09:38:38	55084	2009-09-10 00:00:00	54713.6361226852	2008-09-04 15:16:01	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031332	The origin of the high-energy emission from Broad-Line Radio Galaxies is still an open issue. A plausible scenario is reprocessed emission from a cold medium (disk) diluted by variable, non-thermal jet flux. To test this scenario we propose Suzaku observations of the BLRG 3C 111, which exhibits flux variability above 10 keV from available data, suggesting a jet contribution. Moreover, 3C 111 was previously detected with EGRET at GeV energies, and synergy with GLAST will thus be exploited in the proposed program. The coupled timing and spectral information provided by Suzaku are key to disentangle the disk and jet contributions, and determine their respective role for the source energy budget.	EXTRAGALACTIC COMPACT SOURCES	7	A	RITA SAMBRUNA		USA	3	AO3	SUZAKU OBSERVATIONS OF 3C 111: UNCOVERING THE JET WITHIN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703034010/	Quick Look
375	SKY_53.3_-63.4	53.24	-63.4549	53.047022	-63.62196	354.144887	-74.40934	278.62179386	-45.30780651	286.1724	53797.8694444444	2006-03-03 20:52:00	53800.3342476852	2006-03-06 08:01:19	501002010	101.4752	100	101.4752	101.4752	101.4752	101.4752	2	2	2	2	1	0	0	145.4318	145.4318	212.8539	4	PROCESSED	57533.1863425926	2016-05-25 04:28:20	54401	2007-10-28 00:00:00	53906.7729282407	2006-06-20 18:33:01	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011252	We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble.	GALACTIC DIFFUSE EMISSION	5	A	ROBIN SHELTON		USA	1	AO1	SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501002010/	Quick Look
376	4U 1630-47	248.5034	-47.402	247.582302	-47.297867	254.088861	-25.13983	336.90313759	0.24577164	279.8256	55432.911724537	2010-08-24 21:52:53	55435.6134259259	2010-08-27 14:43:20	405051010	99.9373	100	99.9373	99.9373	0	99.9373	2	2	0	2	1	0	0	90.4512	90.4512	233.3976	2	PROCESSED	57553.2849652778	2016-06-14 06:50:21	55815	2011-09-11 00:00:00	55449.4369560185	2010-09-10 10:29:13	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051252	Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions.	GALACTIC POINT SOURCES	4	A	JOHN TOMSICK		USA	5	AO5-TOO	CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405051010/	Quick Look
377	ABELL 2667	357.9715	-25.9262	357.325218	-26.204419	347.258509	-22.861194	34.71945037	-76.63317585	64.8859	55721.5923611111	2011-06-09 14:13:00	55722.9050925926	2011-06-10 21:43:20	806029010	51.2214	50	51.2294	51.2294	0	51.2214	2	2	0	2	1	0	0	40.4843	40.4843	113.4098	1	PROCESSED	57602.2712962963	2016-08-02 06:30:40	55652	2011-04-01 00:00:00	55757.6995486111	2011-07-15 16:47:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806029010/	Quick Look
378	V1082 SGR	286.8363	-20.7721	286.094048	-20.85102	285.710494	1.754645	15.88147607	-12.67535412	81.3818	56009.1848148148	2012-03-23 04:26:08	56010.4459375	2012-03-24 10:42:09	406042010	39.4605	40	39.4605	39.4605	0	39.4605	2	2	0	2	1	0	0	36.0171	36.0171	108.924	2	PROCESSED	57605.0088541667	2016-08-05 00:12:45	56399	2013-04-17 00:00:00	56023.1564236111	2012-04-06 03:45:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061217	V1082 Sgr is a BAT-detected cataclysmic variable with a 20 hr orbital period that exhibits high and low states. The high X-ray luminosity and the presence of the HeII 4686 lines in its optical spectrum have led to the suggestion that this is an intermediate polar (IP). We propose an exploratory 40 ks Suzaku observation with the aim of establishing if it is indeed an IP. If it is, then this system may provide a unique opportunity to study an IP in a low state, which has not been possible with other IPs.	GALACTIC POINT SOURCES	4	C	KOJI MUKAI		USA	6	AO6	AN UNUSUAL BAT-DETECTED CATACLYSMIC VARIABLE, V1082 SGR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406042010/	Quick Look
379	G156.2+5.7E	75.8128	51.6405	74.832405	51.569986	80.017374	28.69124	156.70319129	6.10796494	274.6638	54149.9177893518	2007-02-18 22:01:37	54151.1750231482	2007-02-20 04:12:02	501074010	53.3331	50	53.3494	53.3491	0	53.3331	2	2	0	2	1	0	0	50.8218	50.8218	108.6199	2	PROCESSED	57537.4302893518	2016-05-29 10:19:37	54773	2008-11-03 00:00:00	54158.2839583333	2007-02-27 06:48:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011235	G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target.	GALACTIC DIFFUSE EMISSION	5	C	ROBERT PETRE		USA	1	AO1	A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501074010/	Quick Look
380	SNR G93.3+6.9 S3	313.171	55.2801	312.823004	55.090273	352.082126	66.837166	93.24775568	6.83197363	40.0152	53906.4300462963	2006-06-20 10:19:16	53906.7266087963	2006-06-20 17:26:19	501082010	16.3347	15	16.3347	16.3587	16.3507	16.3427	1	1	1	1	1	0	0	13.9186	13.9186	25.6159	0	PROCESSED	57534.7339814815	2016-05-26 17:36:56	54401	2007-10-28 00:00:00	53926.2481365741	2006-07-10 05:57:19	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011242	The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment.	GALACTIC DIFFUSE EMISSION	5	B	Q. DANIEL WANG		USA	1	AO1	G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501082010/	Quick Look
381	PUP A : NE	125.7583	-42.7117	125.326284	-42.549841	147.156331	-59.259606	260.25284038	-3.14403225	277.1213	53842.913287037	2006-04-17 21:55:08	53843.3091319445	2006-04-18 07:25:09	501087010	20.7109	20	20.7336	20.7349	20.7189	20.7109	1	1	1	1	1	0	0	19.7443	19.7443	34.1899	1	PROCESSED	57533.5127083333	2016-05-25 12:18:18	54401	2007-10-28 00:00:00	53906.9450231482	2006-06-20 22:40:50	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501087010/	Quick Look
382	TYCHO SNR	6.3139	64.1469	5.613879	63.870082	42.846574	53.765969	120.08177164	1.42013769	53.7834	54682.0646759259	2008-08-04 01:33:08	54686.9529398148	2008-08-08 22:52:14	503085010	312.892	400	312.916	312.892	0	312.908	2	2	0	2	1	0	0	289.9494	289.9494	307.8699	3	PROCESSED	57543.3766782407	2016-06-04 09:02:25	54557	2008-04-01 00:00:00	54707.038287037	2008-08-29 00:55:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031003	Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		USA	3	AO3	SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503085010/	Quick Look
383	N11 SB	74.1823	-66.412	74.156384	-66.487992	354.048784	-83.709745	277.1886014	-36.07081942	146.432	54046.4407291667	2006-11-07 10:34:39	54047.232037037	2006-11-08 05:34:08	501091010	30.452	30	30.452	30.452	30.452	30.452	2	2	2	2	1	0	0	26.405	26.405	68.3659	0	PROCESSED	57536.0384953704	2016-05-28 00:55:26	54455	2007-12-21 00:00:00	54088.5643287037	2006-12-19 13:32:38	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011251	Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 2 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 4 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission.	GALACTIC DIFFUSE EMISSION	5	C	ROSA WILLIAMS		USA	1	AO1	A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501091010/	Quick Look
384	GAMMA CASSIOPEIAE	14.1598	60.7356	13.401441	60.465287	43.939726	48.837698	123.56796459	-2.12972511	72.5084	55755.0038888889	2011-07-13 00:05:36	55756.333587963	2011-07-14 08:00:22	406040010	55.394	50	55.394	55.394	0	55.394	2	2	0	2	1	0	0	56.2164	56.2164	114.8778	0	PROCESSED	57602.6019791667	2016-08-02 14:26:51	56183	2012-09-13 00:00:00	55816.6655208333	2011-09-12 15:58:21	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061207	We propose a 50 ks Suzaku observation to obtain for the first time the hard X-ray spectrum of the classical Be star Gamma Cas. This star is a prototype of the "Gamma Cas stars" class, whose nature is not yet understood. Earlier XMM-Newton and Swift BAT observations gave a hint of the presence of the hard X-ray emission above 10 keV. The broadband Suzaku spectrum will allow to establish its X-ray emission mechanism - non-thermal emission or reflection of thermal emission from a neutral surface. On this basis, we will be able to discriminate the mechanisms between the magnetic disk dynamo and the accretion on a compact star. These new data will be pivotal in solving the enigma of Gamma Cas and revealing the true nature of this astrophysically important object.	GALACTIC POINT SOURCES	4	C	KENJI HAMAGUCHI		USA	6	AO6	SUZAKU'S HARD LOOK AT GAMMA CASSIOPEIAE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406040010/	Quick Look
385	SDSS J1723+5553	260.8912	55.8942	260.65651	55.938805	243.54174	78.493359	83.89291292	34.34970174	8.0654	54986.3677777778	2009-06-04 08:49:36	54986.8148032407	2009-06-04 19:33:19	704051010	35.9368	30	35.9448	35.9368	0	35.9528	1	1	0	1	1	0	0	29.0393	29.0393	38.6159	0	PROCESSED	57547.4618865741	2016-06-08 11:05:07	55364	2010-06-17 00:00:00	54998.1759722222	2009-06-16 04:13:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041422	BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction.	EXTRAGALACTIC COMPACT SOURCES	7	A	XINYU DAI		USA	4	AO4	X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704051010/	Quick Look
386	E0102-72	16.0206	-72.0231	15.615717	-72.291056	314.640431	-65.037838	301.55102123	-45.07123322	281.396	53752.9742708333	2006-01-17 23:22:57	53755.3752199074	2006-01-20 09:00:19	100044020	41.2605	20	41.268	41.8524	41.2605	41.361	3	4	3	4	1	0	0	99.7935	99.7935	207.4298	3	PROCESSED	57532.7555555556	2016-05-24 18:08:00	54247	2007-05-27 00:00:00	54040.6979513889	2006-11-01 16:45:03	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001097	We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip	CALIBRATION	1	A	HIRONORI MATSUMOTO		JAP	0	SWG	XIS FLIGHT CAIBRATION PLAN	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100044020/	Quick Look
387	B1920+10(2)	292.8971	10.8605	292.305399	10.753499	296.831046	32.19317	47.18977478	-3.80874006	248.6642	54783.7420833333	2008-11-13 17:48:36	54785.8981365741	2008-11-15 21:33:19	503091010	100.4577	100	100.4577	100.4577	0	100.4577	2	2	0	2	1	0	0	93.8731	93.8731	186.248	0	PROCESSED	57544.4390972222	2016-06-05 10:32:18	55167	2009-12-02 00:00:00	54797.1537731482	2008-11-27 03:41:26	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031204	A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps.	GALACTIC DIFFUSE EMISSION	5	C	ZDENKA MISANOVIC		USA	3	AO3	STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503091010/	Quick Look
388	GCL4	265.3437	-29.192	264.548064	-29.167468	265.905576	-5.816983	359.29532739	0.65531706	106.9407	54907.3257986111	2009-03-17 07:49:09	54908.0711111111	2009-03-18 01:42:24	503102010	33.6554	25	33.6794	33.6558	0	33.6554	2	2	0	2	1	0	0	30.0521	30.0521	64.3899	0	PROCESSED	57545.8492939815	2016-06-06 20:22:59	55329	2010-05-13 00:00:00	54920.054837963	2009-03-30 01:18:58	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031234	We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity.	GALACTIC DIFFUSE EMISSION	5	B	FARHAD YUSEF-ZADEH		USA	3	AO3	A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503102010/	Quick Look
389	COMET_8P_TUTTLE-P1-6	28.2017	6.7525	27.54593	6.506397	28.607042	-4.520684	148.82276905	-53.00641332	248.5018	54470.8491666667	2008-01-05 20:22:48	54470.9154050926	2008-01-05 21:58:11	502062060	2.0266	2	2.0266	2.0266	0	2.0266	1	1	0	1	1	0	0	2.044	2.044	5.664	0	PROCESSED	57541.0007986111	2016-06-02 00:01:09	54908	2009-03-18 00:00:00	54542.2318634259	2008-03-17 05:33:53	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062060/	Quick Look
390	COMET_8P_TUTTLE-P2_02	39.704	-35.8295	39.191609	-36.044542	21.228259	-48.000366	240.49763907	-65.60654763	257.6692	54490.1630902778	2008-01-25 03:54:51	54490.2960069444	2008-01-25 07:06:15	502063020	5.2049	5	5.2049	5.2049	0	5.2049	1	1	0	1	1	0	0	5.5919	5.5919	11.4499	0	PROCESSED	57541.3791898148	2016-06-02 09:06:02	54912	2009-03-22 00:00:00	54546.1091666667	2008-03-21 02:37:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063020/	Quick Look
391	COMET_8P_TUTTLE-P2_07	40.0041	-36.5319	39.495887	-36.746007	21.066088	-48.735556	241.99586619	-65.20252382	258.1285	54490.8297106482	2008-01-25 19:54:47	54490.962662037	2008-01-25 23:06:14	502063070	5.2676	5	5.2916	5.2676	0	5.2994	1	1	0	1	1	0	0	2.753	2.753	11.4799	0	PROCESSED	57541.3952777778	2016-06-02 09:29:12	54912	2009-03-22 00:00:00	54546.130462963	2008-03-21 03:07:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063070/	Quick Look
392	COMET_8P_TUTTLE-P2_BGD-2	40.4817	-37.5941	39.980067	-37.806706	20.824934	-49.853115	244.17118034	-64.55380496	254.4101	54492.5631365741	2008-01-27 13:30:55	54492.7293287037	2008-01-27 17:30:14	502064020	6.9797	5	6.9797	7.0037	0	6.9877	1	1	0	1	1	0	0	5.5471	5.5471	14.3519	0	PROCESSED	57554.5355671296	2016-06-15 12:51:13	54912	2009-03-22 00:00:00	54546.2537847222	2008-03-21 06:05:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502064020/	Quick Look
393	G21.5-0.9	278.4035	-10.5067	277.711514	-10.545731	278.460081	12.687392	21.56184596	-0.8687642	103.5554	54188.7945023148	2007-03-29 19:04:05	54189.6252199074	2007-03-30 15:00:19	502065010	25.1416	100	25.156	25.1416	0	25.156	1	2	0	1	1	0	0	22.889	22.889	71.7699	1	PROCESSED	57538.0286921296	2016-05-30 00:41:19	54695	2008-08-17 00:00:00	54209.5181018518	2007-04-19 12:26:04	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021211	We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray.	GALACTIC DIFFUSE EMISSION	5	B	ILANA HARRUS		USA	2	AO2	SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502065010/	Quick Look
394	G296.1-0.5N	177.8287	-62.3875	177.210977	-62.109277	215.982021	-55.076396	296.02814016	-0.3243747	322.3815	54321.2538541667	2007-08-09 06:05:33	54323.4522453704	2007-08-11 10:51:14	502068010	77.1759	67	77.1759	77.1759	0	77.1759	2	2	0	2	1	0	0	68.4846	68.4846	189.9237	1	PROCESSED	57539.4859953704	2016-05-31 11:39:50	54716	2008-09-07 00:00:00	54347.5137268518	2007-09-04 12:19:46	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021218	Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles.	GALACTIC DIFFUSE EMISSION	5	B	KAZIMIERZ BORKOWSKI		USA	2	AO2	G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502068010/	Quick Look
395	GC CENTER #2	266.7693	-28.6295	265.976908	-28.611884	267.143281	-5.22043	0.42794484	-0.11339991	74.7707	53821.958587963	2006-03-27 23:00:22	53823.7585069444	2006-03-29 18:12:15	500005010	88.4247	100	88.4327	88.4247	88.4327	88.4327	2	2	2	2	1	0	0	64.5911	64.5911	155.5019	2	PROCESSED	57533.3630324074	2016-05-25 08:42:46	54247	2007-05-27 00:00:00	54133.0079861111	2007-02-02 00:11:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001020	We propose to obtain high quality spectrum near the GC. The objective is to resolve 6.4, 6.7, and 6.9 keV line and determine the high energy tail and sub-structures, which may be X-ray reflection from Sgr A* (6.4 keV line + 7.1 keV edge + high energy tail), thermal plasma (6.7 + 6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.	GALACTIC DIFFUSE EMISSION	5	A	KATSUJI KOYAMA		JAP	0	SWG	SUZAKU GALACTIC CENTER OBSERVATION PROJECT: #2 SGR B1		N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500005010/	Quick Look
396	4U1626-67	248.0601	-67.4675	246.801189	-67.3606	258.324109	-44.911512	321.78071552	-13.09322804	103.0359	53803.0543518518	2006-03-09 01:18:16	53805.818275463	2006-03-11 19:38:19	400015010	102.6392	100	102.654	102.6392	102.6472	102.654	2	2	2	2	1	0	0	93.3932	93.3932	238.7819	3	PROCESSED	57533.2349652778	2016-05-25 05:38:21	54247	2007-05-27 00:00:00	54042.4663657407	2006-11-03 11:11:34	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001081	The X-ray spectrum of the 7 second LMXRB pulsar 4U1626-67 is dominated by low energy line emission with little evedence of iron K line in the pulse phase resolved spectra. It showd also cyclotron line at 37 keV that departs from the correlation of energy cutoff cyclotron energy observed in many other X-ray pulsars. This Suzaku observation allow to characterize the overall continuum, the low energy, the iron K alpha and cyclotron lines as function of the pulse phase,	GALACTIC POINT SOURCES	4	A	LORELLA ANGELINI		JAP	0	SWG	4U1626-67: PHASE RESOLVED SPECTRA AND CYCLOTRON LINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/400015010/	Quick Look
397	1FGL J1018.6-5856	154.7369	-58.9465	154.294298	-58.695121	196.565847	-60.86994	284.35429996	-1.68890631	297.8367	56093.0246875	2012-06-15 00:35:33	56093.5348032407	2012-06-15 12:50:07	407071010	20.8203	20	20.8203	20.8203	0	20.8203	2	2	0	2	1	0	0	16.813	16.813	44.0639	0	PROCESSED	57605.6779282407	2016-08-05 16:16:13	56542	2013-09-07 00:00:00	56176.237025463	2012-09-06 05:41:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071234	We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation.	GALACTIC POINT SOURCES	4	B	TAKAAKI TANAKA		USA	7	AO7	SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407071010/	Quick Look
398	SNR 0049-73.6	12.7817	-73.3677	12.345533	-73.639533	310.812589	-64.728588	302.96274339	-43.76053264	62.7682	54629.4818518518	2008-06-12 11:33:52	54632.7605787037	2008-06-15 18:15:14	503094010	120.478	120	120.486	120.478	0	120.486	2	2	0	2	1	0	0	107.7079	107.7079	283.2419	3	PROCESSED	57542.894525463	2016-06-03 21:28:07	55008	2009-06-26 00:00:00	54642.6050694444	2008-06-25 14:31:18	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031211	We propose to observe the O-rich supernova remnant (SNR) 0049-73.6 in the Small Magellanic Cloud (SMC). SNR 0049-73.6 shares some similarities and differences with another O-rich SNR 0103-72.6 in the SMC. High resolution X-ray spectroscopy of these SNRs with Suzaku/XIS observations should provide a useful insight for the details of thermal evolution of a core-collapse SNR. We began this program with an AO1 Suzaku/XIS observation of SNR 0103-72.6. We here propose to continue this program with our AO3 Suzaku observation of 0049-73.6. We request for a 120 ks Suzaku/XIS observation of 0049-73.6.	GALACTIC DIFFUSE EMISSION	5	B	SANGWOOK PARK		USA	3	AO3	OXYGEN-RICH SUPERNOVA REMNANT 0049-73.6 IN THE SMC	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503094010/	Quick Look
399	CD -28 3719	105.2866	-29.1168	104.795571	-29.044554	111.677742	-51.412828	240.20191687	-10.89157366	97.0723	56577.3593634259	2013-10-12 08:37:29	56579.416099537	2013-10-14 09:59:11	408032010	14.3679	90	14.3679	90.0777	0	90.0777	3	2	0	2	1	0	0	78.3569	78.3569	177.6659	1	PROCESSED	57645.4999652778	2016-09-14 11:59:57	57009	2014-12-18 00:00:00	56642.7667476852	2013-12-16 18:24:07	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081214	Since they were discovered, it has been almost impossible to directly observe the accretion region in most symbiotic stars, in which a white dwarf (WD) accretes from the wind of a red giant. With the discovery that hard X-ray emission (E > 2 keV) is a common feature of WD symbiotics, that situation has finally changed. We propose to use Suzaku observations of 3 typical symbiotics with hard X-ray emission to test the hypothesis that such emission emanates from an accretion-disk boundary layer. With the proposed observations, we will determine whether the WD's magnetic field is high enough to disrupt the accretion flow, and estimate the WD mass and accretion rate. This work has implications for the study of accretion in wide binaries and symbiotics stars as progenitors of SNIa.	GALACTIC POINT SOURCES	4	B	JENNIFER SOKOLOSKI		USA	8	AO8	X-RAYS FROM THE ACCRETION FLOWS IN SYMBIOTIC STARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408032010/	Quick Look
400	TYCHO SNR	6.3115	64.1447	5.611508	63.867881	42.842768	53.765034	120.08050675	1.41805528	43.1557	54689.3425578704	2008-08-11 08:13:17	54690.918275463	2008-08-12 22:02:19	503085020	102.8556	100	102.8556	102.8556	0	102.8556	2	2	0	2	1	0	0	91.9078	91.9078	136.1039	1	PROCESSED	57543.2895717593	2016-06-04 06:56:59	54557	2008-04-01 00:00:00	54706.7896412037	2008-08-28 18:57:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031003	Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		USA	3	AO3	SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503085020/	Quick Look
401	GCL1	265.1726	-28.5274	264.381201	-28.50205	265.733071	-5.157711	359.7799359	1.13423351	69.7267	54900.8188425926	2009-03-10 19:39:08	54901.4557175926	2009-03-11 10:56:14	503099010	29.706	25	29.7241	29.722	0	29.706	2	2	0	2	1	0	0	30.5649	30.5649	55.02	1	PROCESSED	57545.7841782407	2016-06-06 18:49:13	55329	2010-05-13 00:00:00	54916.3706828704	2009-03-26 08:53:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031234	We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity.	GALACTIC DIFFUSE EMISSION	5	B	FARHAD YUSEF-ZADEH		USA	3	AO3	A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503099010/	Quick Look
402	SLX 1737-282	265.2352	-28.3094	264.445148	-28.284356	265.781005	-4.938001	359.99405573	1.20298654	69.9745	54901.4562384259	2009-03-11 10:56:59	54901.8035648148	2009-03-11 19:17:08	503103010	18.316	10	18.3324	18.332	0	18.316	2	2	0	2	1	0	0	16.3659	16.3659	30.0019	0	PROCESSED	57545.7980208333	2016-06-06 19:09:09	55329	2010-05-13 00:00:00	54916.9907638889	2009-03-26 23:46:42	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031234	We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity.	GALACTIC DIFFUSE EMISSION	5	C	FARHAD YUSEF-ZADEH		USA	3	AO3	A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503103010/	Quick Look
403	TYCHO SNR	6.3244	64.1507	5.624265	63.873888	42.856632	53.765731	120.08671326	1.42345384	81.1044	53913.439224537	2006-06-27 10:32:29	53915.6530555556	2006-06-29 15:40:24	500024010	101.1274	100	101.1434	101.1274	101.1434	101.1434	2	2	2	2	1	0	0	94.5123	94.5123	191.2068	3	PROCESSED	57534.8252199074	2016-05-26 19:48:19	54289	2007-07-08 00:00:00	54052.7199884259	2006-11-13 17:16:47	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001099	We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		JAP	0	SWG	SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500024010/	Quick Look
404	NEP #3	270.0483	66.5696	270.04982	66.569341	34.92017	89.983512	96.39421541	29.79223028	188.0738	55180.9320949074	2009-12-15 22:22:13	55182.0557638889	2009-12-17 01:20:18	504074010	50.1769	50	50.1769	50.1769	0	50.1769	2	2	0	2	1	0	0	33.3374	33.3374	97.0499	1	PROCESSED	57549.895162037	2016-06-10 21:29:02	54922	2009-04-01 00:00:00	55200.4707291667	2010-01-04 11:17:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041101	We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe.	GALACTIC DIFFUSE EMISSION	5	A	STEVEN SNOWDEN		USA	4	AO4	OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504074010/	Quick Look
405	HESS J1809-193E	272.0013	-19.5033	271.261943	-19.51123	271.881238	3.92439	10.71539243	0.332309	270.1011	55085.7498148148	2009-09-11 17:59:44	55087.1564351852	2009-09-13 03:45:16	504079010	51.0289	50	51.0289	51.0289	0	51.0289	2	2	0	2	1	0	0	41.8753	41.8753	121.5198	2	PROCESSED	57548.5914699074	2016-06-09 14:11:43	55465	2010-09-26 00:00:00	55098.3372337963	2009-09-24 08:05:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041303	We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background.	GALACTIC DIFFUSE EMISSION	5	A	OLEG KARGALTSEV		USA	4	AO4	CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504079010/	Quick Look
406	G156.2+5.7 (NW2)	74.4322	52.0607	73.448956	51.983713	79.105505	29.208158	155.84514532	5.68920631	266.0115	55258.7553587963	2010-03-03 18:07:43	55259.9821643518	2010-03-04 23:34:19	504081010	52.8646	50	52.8678	52.8678	0	52.8646	2	2	0	2	1	0	0	49.3866	49.3866	105.991	1	PROCESSED	57550.7899189815	2016-06-11 18:57:29	55689	2011-05-08 00:00:00	55322.3173842593	2010-05-06 07:37:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041311	The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks.	GALACTIC DIFFUSE EMISSION	5	C	SATORU KATSUDA		USA	4	AO4	REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504081010/	Quick Look
407	XB1916-053	289.7015	-5.2503	289.036388	-5.342643	290.518339	16.797779	31.34764946	-8.47089453	261.8034	56948.5140856482	2014-10-18 12:20:17	56952.1112152778	2014-10-22 02:40:09	409032020	140.4495	300	140.4575	140.4655	0	140.4495	2	2	0	2	1	0	0	6.8873	6.8873	14.636	0	PROCESSED	57616.6738773148	2016-08-16 16:10:23	56748	2014-04-01 00:00:00	57000.2058680556	2014-12-09 04:56:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091221	XB1916-053 is a prototypical dipping low mass X-ray binary (LMXB) with a dip recurrence period of 3000.6+-0.2s. However, extensive optical observations also show a longer stable period of 3027s. The former is most likely the orbital period, and the latter the superhump period caused by the precession of an elliptical accretion disk at a period of 3.9 days, representing the beat period between optical and X-ray periods. The morphology of the X-ray dips does indeed change dramatically over several days, but existing data suggest a somewhat longer period for the dip morphology cycle of 4.7 days. Here we propose a 300ks Suzaku observation of XB1916-053 with as few interruptions as possible, to conduct a definitive timing and spectroscopic study of its disk emission and dipping activity.	GALACTIC POINT SOURCES	4	B	ALAN SMALE		USA	9	AO9	THE PRECESSING DISK IN THE DIPPING X-RAY BINARY XB1916-053	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409032020/	Quick Look
408	330.2+1.0	240.2338	-51.588	239.290439	-51.447752	249.06097	-30.286548	330.14009051	0.98414205	285.0002	55078.1480671296	2009-09-04 03:33:13	55080.8126736111	2009-09-06 19:30:15	504083010	127.7746	150	127.7826	127.7746	0	127.7746	2	2	0	2	1	0	0	112.8484	112.8484	230.1578	1	PROCESSED	57548.4938657407	2016-06-09 11:51:10	55455	2010-09-16 00:00:00	55089.3295949074	2009-09-15 07:54:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041312	Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity.	GALACTIC DIFFUSE EMISSION	5	B	GLENN ALLEN		USA	4	AO4	MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504083010/	Quick Look
409	LMC X-4	83.1804	-66.3624	83.172059	-66.39551	0.975905	-87.276392	276.32693529	-32.54034863	209.1491	54480.3607175926	2008-01-15 08:39:26	54480.7919560185	2008-01-15 19:00:25	702038010	21.6579	20	21.6726	21.6579	0	21.6726	2	2	0	2	1	0	0	22.8837	22.8837	37.252	0	PROCESSED	57541.3108796296	2016-06-02 07:27:40	54860	2009-01-29 00:00:00	54490.3089236111	2008-01-25 07:24:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021127	We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects.	EXTRAGALACTIC COMPACT SOURCES	7	A	RYAN HICKOX		USA	2	AO2	SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702038010/	Quick Look
410	73P/SW3	18.0599	-9.2267	17.433228	-9.491881	13.014248	-15.596574	139.25333623	-71.43625621	59.4006	53894.0025	2006-06-08 00:03:36	53894.0689699074	2006-06-08 01:39:19	500014060	3.235	35	3.235	3.235	3.235	3.235	1	1	1	1	1	0	0	2.49	2.49	5.7359	0	PROCESSED	57534.5883796296	2016-05-26 14:07:16	54267	2007-06-16 00:00:00	54052.5346759259	2006-11-13 12:49:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014060/	Quick Look
411	NGC5548	214.4969	25.1266	213.929993	25.356783	201.998856	36.406453	31.93001973	70.4949274	285.8791	54310.1810648148	2007-07-29 04:20:44	54311.0209953704	2007-07-30 00:30:14	702042070	31.8099	30	31.8099	31.8099	0	31.8099	1	1	0	1	1	0	0	29.503	29.503	72.5279	1	PROCESSED	57539.3547569444	2016-05-31 08:30:51	54706	2008-08-28 00:00:00	54339.4245486111	2007-08-27 10:11:21	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021307	We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	2	AO2	NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042070/	Quick Look
412	73P/SW3	18.338	-9.3332	17.711705	-9.597966	13.233056	-15.802283	140.17356876	-71.46762322	59.3974	53894.4024768518	2006-06-08 09:39:34	53894.4682986111	2006-06-08 11:14:21	500014120	1.5551	35	1.5551	1.5551	1.5551	1.5551	1	1	1	1	1	0	0	1.566	1.566	5.682	0	PROCESSED	57534.5988773148	2016-05-26 14:22:23	54267	2007-06-16 00:00:00	54052.5441782407	2006-11-13 13:03:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001050	Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.	GALACTIC DIFFUSE EMISSION	5	A	FREDERICK PORTER		JAP	0	SWG	AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014120/	Quick Look
413	NGC 1365	53.3968	-36.1347	52.919388	-36.301683	36.801187	-53.032832	237.94662462	-54.6022242	221.6565	54486.2300578704	2008-01-21 05:31:17	54490.0002083333	2008-01-25 00:00:18	702047010	160.5057	150	160.5057	160.5137	0	160.5137	2	2	0	2	1	0	0	146.8139	146.8139	325.6768	4	PROCESSED	57541.4786342593	2016-06-02 11:29:14	54883	2009-02-21 00:00:00	54515.5847800926	2008-02-19 14:02:05	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021314	We propose a 150 ksec observation of the Seyfert Galaxy NGC 1365. This galaxy have a unique set of properties: FeXXV and FeXXVI Kalpha and Kbeta absorption lines (the highest S/N detection so far among AGNs), rapidly varying cold absorber (nH variations of ~10^23/cm^2 in a few hours, changes from Compton-thick to Compton-thin in two days), a relativistic iron emission line. This new long observation will use at best the unique capabilities of Suzaku to constrain the dimensions of the absorbers, and, for the first time, will investigate the dynamics and physical conditions of the hot absorber responsible of the iron absorption lines. It is likely that an occultation will occur during the observation. This occultation would directly set the dimension of the X-ray source.	EXTRAGALACTIC COMPACT SOURCES	7	C	GUIDO RISALITI		USA	2	AO2	BLACK HOLE OCCULTATION AND OUTFLOW VARIABILITY IN NGC 1365	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702047010/	Quick Look
414	SN1006 SE	225.8656	-42.0517	225.046486	-41.856364	235.600187	-23.734349	327.61589547	14.40537	115.0022	53765.3759259259	2006-01-30 09:01:20	53766.487662037	2006-01-31 11:42:14	500016010	51.6076	50	51.6132	51.6212	51.6212	51.6076	2	2	2	2	1	0	0	55.6704	55.6704	96.0399	2	PROCESSED	57532.8333564815	2016-05-24 20:00:02	54247	2007-05-27 00:00:00	54040.6484259259	2006-11-01 15:33:44	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001062	We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta.	GALACTIC DIFFUSE EMISSION	5	A	JOHN HUGHES		JAP	0	SWG	THE EJECTA IN SN1006	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500016010/	Quick Look
415	SGR C	266.1523	-29.4673	265.354719	-29.446679	266.622211	-6.071258	359.43182832	-0.08906822	82.0001	53786.5315393518	2006-02-20 12:45:25	53789.4515509259	2006-02-23 10:50:14	500018010	106.9219	100	106.9219	106.9219	106.9219	106.9219	2	2	2	2	1	0	0	46.6069	46.6069	252.2778	2	PROCESSED	57533.0732175926	2016-05-25 01:45:26	54247	2007-05-27 00:00:00	54041.6109375	2006-11-02 14:39:45	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001079	We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD.	GALACTIC DIFFUSE EMISSION	5	A	HIROSHI MURAKAMI		JAP	0	SWG	FOSSILS OF THE GALACTIC CENTER ACTIVITY	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500018010/	Quick Look
416	NGC 6300	259.2549	-62.8185	258.083078	-62.76377	263.641528	-39.613132	328.49505458	-14.05378352	296.7285	54390.5141087963	2007-10-17 12:20:19	54392.375162037	2007-10-19 09:00:14	702049010	82.577	80	82.577	82.577	0	82.577	2	2	0	2	1	0	0	105.5127	105.5127	160.7798	1	PROCESSED	57540.3276041667	2016-06-01 07:51:45	54770	2008-10-31 00:00:00	54403.3802083333	2007-10-30 09:07:30	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021331	Recent X-ray observations of Seyfert 2 galaxies have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by AGN Unified Schemes. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (60 ksec each) of four local bright Compton-thin Seyfert2s, selected from the Swift/BAT survey with a hard X-ray flux exceeding 1e-10 cgs to form a flux-limited sample. The unprecedented broad bandpass of Suzaku offers a unique tool to investigate the X-ray emission, placing strong constraints on the geometry and location of the reprocessing matter.	EXTRAGALACTIC COMPACT SOURCES	7	B	JAMES REEVES		USA	2	AO2	REVEALING THE REPROCESSING MATTER IN SEYFERT 2 GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702049010/	Quick Look
417	SEP #3	89.9578	-66.5683	89.959755	-66.568521	317.285609	-89.984917	276.39273536	-29.82821774	172.4885	55179.5059259259	2009-12-14 12:08:32	55180.9169444444	2009-12-15 22:00:24	504073010	44.408	50	44.408	44.416	0	44.416	2	2	0	2	1	0	0	23.8784	23.8784	121.9018	1	PROCESSED	57549.8504282407	2016-06-10 20:24:37	54922	2009-04-01 00:00:00	55200.462337963	2010-01-04 11:05:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041101	We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe.	GALACTIC DIFFUSE EMISSION	5	A	STEVEN SNOWDEN		USA	4	AO4	OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504073010/	Quick Look
418	G156.2+5.7 (E2)	75.2673	51.6789	74.287315	51.605827	79.638917	28.767744	156.46612231	5.86221802	271.6298	55248.7736574074	2010-02-21 18:34:04	55250.0369675926	2010-02-23 00:53:14	504082010	50.3308	50	50.3468	50.3308	0	50.3468	3	2	0	2	1	0	0	46.1424	46.1424	109.1379	0	PROCESSED	57550.6943865741	2016-06-11 16:39:55	55632	2011-03-12 00:00:00	55266.2981597222	2010-03-11 07:09:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041311	The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks.	GALACTIC DIFFUSE EMISSION	5	C	SATORU KATSUDA		USA	4	AO4	REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504082010/	Quick Look
419	PUP A : S	125.6829	-43.1445	125.254263	-42.982932	147.449231	-59.669734	260.57740663	-3.43620983	277.8865	53843.8334606482	2006-04-18 20:00:11	53844.4397569444	2006-04-19 10:33:15	501090010	31.1445	30	31.1605	31.1525	31.1445	31.1685	2	2	2	2	1	0	0	26.5856	26.5856	52.3719	1	PROCESSED	57533.5191550926	2016-05-25 12:27:35	54401	2007-10-28 00:00:00	53907.0902199074	2006-06-21 02:09:55	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011246	We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present.	GALACTIC DIFFUSE EMISSION	5	A	UNA HWANG		USA	1	AO1	MAPPING OXYGEN IN PUPPIS A	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501090010/	Quick Look
420	ESO 506-G027	189.6943	-27.3584	189.030338	-27.083667	200.074921	-21.229266	299.48164005	35.42851647	302.0467	54314.0460300926	2007-08-02 01:06:17	54315.2572222222	2007-08-03 06:10:24	702080010	41.7453	40	41.7533	41.7613	0	41.7453	1	1	0	1	1	0	0	38.2828	38.2828	104.6399	2	PROCESSED	57539.3906134259	2016-05-31 09:22:29	54710	2008-09-01 00:00:00	54340.5553125	2007-08-28 13:19:39	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021374	Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702080010/	Quick Look
421	DEM L238	83.8177	-70.5927	83.963728	-70.62236	296.31824	-85.384034	281.24911245	-31.77318091	307.401	55308.023125	2010-04-22 00:33:18	55312.9730902778	2010-04-26 23:21:15	505063010	199.7795	200	199.7795	199.7795	0	199.7795	2	2	0	2	1	0	0	167.8355	167.8355	427.6297	5	PROCESSED	57551.4910069444	2016-06-12 11:47:03	55287	2010-04-01 00:00:00	55326.6889699074	2010-05-10 16:32:07	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051102	Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors.	GALACTIC DIFFUSE EMISSION	5	A	KAZIMIERZ BORKOWSKI		USA	5	AO5	TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505063010/	Quick Look
422	VELA FRAGMENT B	135.5139	-43.4767	135.058427	-43.278826	159.573758	-56.461444	265.2464603	1.98991007	89.0012	54044.6051388889	2006-11-05 14:31:24	54046.4341898148	2006-11-07 10:25:14	501085010	57.8804	60	57.8964	57.8804	57.8964	57.8964	2	2	2	2	1	0	0	56.9652	56.9652	158.0219	2	PROCESSED	57536.0751157407	2016-05-28 01:48:10	54695	2008-08-17 00:00:00	54091.4107175926	2006-12-22 09:51:26	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011245	Ejecta fragments from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM-Newton, show strongly enhanced but very different abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe another fragment, "B". The abundances and distribution will provide further evidence about the origin and evolution of these ejecta clumps, In combination with the existing observations of fragments A and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interaction with the remnant shell and the surrounding ISM.	GALACTIC DIFFUSE EMISSION	5	C	TERRANCE GAETZ		USA	1	AO1	SEARCHING FOR EJECTA IN VELA SNR FRAGMENT B	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501085010/	Quick Look
423	VELA PWN E3	129.9962	-45.3672	129.571682	-45.189023	154.98711	-60.107857	264.19786494	-2.25193357	304.5033	55712.1335069444	2011-05-31 03:12:15	55712.4099305556	2011-05-31 09:50:18	506046010	14.1787	15	14.2027	14.1947	0	14.1787	2	2	0	2	1	0	0	12.6599	12.6599	23.8759	0	PROCESSED	57602.1638078704	2016-08-02 03:55:53	56093	2012-06-15 00:00:00	55725.9978240741	2011-06-13 23:56:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506046010/	Quick Look
424	SNR HB3 SE-B	35.7593	62.192	34.815236	61.964819	57.837975	44.676486	133.39304715	1.19520932	247.4986	56323.4084259259	2013-01-31 09:48:08	56323.7710532407	2013-01-31 18:30:19	507057010	25.8366	20	25.8446	25.8366	0	25.8526	1	1	0	1	1	0	0	19.3092	19.3092	31.3279	1	PROCESSED	57608.6657638889	2016-08-08 15:58:42	56711	2014-02-23 00:00:00	56345.4750462963	2013-02-22 11:24:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071316	We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective.	GALACTIC DIFFUSE EMISSION	5	C	JUNICHIRO KATSUTA		USA	7	AO7	SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507057010/	Quick Look
425	SNR HB3 SE-C	36.0358	62.4578	35.086232	62.23139	58.169094	44.855041	133.42083063	1.4890972	247.4994	56323.7716666667	2013-01-31 18:31:12	56324.1585532407	2013-02-01 03:48:19	507058010	24.142	20	24.1616	24.142	0	24.1696	2	2	0	2	1	0	0	23.4547	23.4547	33.4239	0	PROCESSED	57608.6786342593	2016-08-08 16:17:14	56711	2014-02-23 00:00:00	56345.4779976852	2013-02-22 11:28:19	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071316	We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective.	GALACTIC DIFFUSE EMISSION	5	C	JUNICHIRO KATSUTA		USA	7	AO7	SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507058010/	Quick Look
426	COMET_8P_TUTTLE-P1-10	28.408	5.7525	27.75444	5.506869	28.446793	-5.529035	149.8061723	-53.84230192	248.5015	54471.1158333333	2008-01-06 02:46:48	54471.1820717593	2008-01-06 04:22:11	502062100	3.2196	3.2	3.2196	3.2196	0	3.2196	1	1	0	1	1	0	0	2.166	2.166	5.6799	0	PROCESSED	57541.2676967593	2016-06-02 06:25:29	54908	2009-03-18 00:00:00	54542.2429513889	2008-03-17 05:49:51	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062100/	Quick Look
427	COMET_8P_TUTTLE-P2_09	40.126	-36.804	39.619449	-37.017725	21.006365	-49.022029	242.56232387	-65.03879756	253.3121	54491.0963773148	2008-01-26 02:18:47	54491.2292824074	2008-01-26 05:30:10	502063090	4.3979	4	4.3979	4.3979	0	4.3979	1	1	0	1	1	0	0	4.752	4.752	11.4439	0	PROCESSED	57541.402662037	2016-06-02 09:39:50	54912	2009-03-22 00:00:00	54546.2142592593	2008-03-21 05:08:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021001	We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite.	GALACTIC DIFFUSE EMISSION	5	A	GREGORY BROWN		USA	2	AO2	SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063090/	Quick Look
428	COMA SW1	194.4352	27.7266	193.830461	27.996528	181.158138	30.970186	56.45564066	88.47880121	314.5924	55735.5408796296	2011-06-23 12:58:52	55735.8654166667	2011-06-23 20:46:12	806047010	8.9948	10	9.0028	8.9948	0	9.0108	2	2	0	2	1	0	0	8.5423	8.5423	28.0339	1	PROCESSED	57602.3938773148	2016-08-02 09:27:11	55652	2011-04-01 00:00:00	55794.9989583333	2011-08-21 23:58:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806047010/	Quick Look
429	COMA SW6	193.5264	26.9952	192.918358	27.266175	180.700954	29.954854	20.45636346	89.39137704	314.5991	55736.3040393518	2011-06-24 07:17:49	55736.5884259259	2011-06-24 14:07:20	806049010	15.6938	15	15.6938	15.7258	0	15.7098	1	1	0	1	1	0	0	13.0934	13.0934	24.5599	0	PROCESSED	57602.3988657407	2016-08-02 09:34:22	55652	2011-04-01 00:00:00	55795.0033333333	2011-08-22 00:04:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806049010/	Quick Look
430	COMA SW6.5	193.4098	26.8733	192.801305	27.144404	180.65639	29.799393	5.58469416	89.44734556	314.5984	55736.5887615741	2011-06-24 14:07:49	55737.1238773148	2011-06-25 02:58:23	806050010	16.5376	15	16.5616	16.5536	0	16.5376	2	2	0	2	1	0	0	16.6623	16.6623	46.208	2	PROCESSED	57602.4126157407	2016-08-02 09:54:10	55652	2011-04-01 00:00:00	55795.0480324074	2011-08-22 01:09:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806050010/	Quick Look
431	G21.5-0.9	278.4038	-10.5066	277.711815	-10.545632	278.460388	12.687474	21.56207071	-0.86897985	103.5553	54190.0674074074	2007-03-31 01:37:04	54191.7405671296	2007-04-01 17:46:25	502065020	53.5261	100	53.5261	53.551	0	53.5661	1	2	0	1	1	0	0	48.618	48.618	144.5418	0	PROCESSED	57538.0817013889	2016-05-30 01:57:39	54695	2008-08-17 00:00:00	54200.5054861111	2007-04-10 12:07:54	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021211	We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray.	GALACTIC DIFFUSE EMISSION	5	B	ILANA HARRUS		USA	2	AO2	SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502065020/	Quick Look
432	NGC 788	30.262	-6.7593	29.638132	-7.000547	25.672425	-17.884233	165.15039638	-63.76864601	77.358	54660.0353819444	2008-07-13 00:50:57	54661.0516666667	2008-07-14 01:14:24	703032010	45.9073	40	45.9153	45.9073	0	45.9153	1	1	0	1	1	0	0	39.594	39.594	87.7999	0	PROCESSED	57543.0405902778	2016-06-04 00:58:27	55048	2009-08-05 00:00:00	54682.1458564815	2008-08-04 03:30:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031323	The classical unified model predicts only one type of Seyfert II (Sy2). Recent observations of SWIFT BAT-detected AGN found at least 4 classes of Sy2s: (1) objects with high column density and scattered soft x-rays, (2) Compton thick objects, (3) `hidden' AGN (Ueda et al. 2007), and (4) the `changing look' objects (Risaliti et al. 2006). The nature of these sources can only be revealed with high quality broad-band X-ray spectra from Suzaku. Thus, we are proposing 40ks observations for 2 of the brightest BAT AGN without high quality data, NGC 788, a type (3) object showing polarized optical broad lines, and NGC 3281, a classified (2) object. Such observations are necessary to build a reasonably large sample of high-quality, broad-band Sy2 spectra covering the range of X-ray/optical types.	EXTRAGALACTIC COMPACT SOURCES	7	A	RICHARD MUSHOTZKY		USA	3	AO3	SUZAKU OBSERVATIONS OF X-RAY BRIGHT TYPE II AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703032010/	Quick Look
433	Q0122-380	21.0759	-37.7461	20.512127	-38.006435	1.342949	-42.439189	271.91657466	-77.33125236	48.7944	54615.4511921296	2008-05-29 10:49:43	54616.2009722222	2008-05-30 04:49:24	703035010	28.481	25	28.481	28.489	0	28.497	2	2	0	2	1	0	0	26.8107	26.8107	64.7699	1	PROCESSED	57542.6524421296	2016-06-03 15:39:31	54999	2009-06-17 00:00:00	54633.6971759259	2008-06-16 16:43:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031334	Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates.	EXTRAGALACTIC COMPACT SOURCES	7	B	GEORGE CHARTAS		USA	3	AO3	A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703035010/	Quick Look
434	Q0551-3637	88.2026	-36.6158	87.768837	-36.625605	87.11791	-60.039805	242.36930247	-26.91846995	296.4731	54575.4385763889	2008-04-19 10:31:33	54575.6251041667	2008-04-19 15:00:09	703036010	3.8954	22	3.8954	3.8954	0	3.8954	1	1	0	1	1	0	0	3.773	3.773	16.0959	0	PROCESSED	57542.3345601852	2016-06-03 08:01:46	54979	2009-05-28 00:00:00	54588.1227314815	2008-05-02 02:56:44	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031334	Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	3	AO3	A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703036010/	Quick Look
435	0509-67.5	77.4191	-67.5347	77.43679	-67.59534	342.967322	-85.012032	278.15520093	-34.57404921	36.9172	56491.0670601852	2013-07-18 01:36:34	56495.4689583333	2013-07-22 11:15:18	508072020	152.6517	150	152.6997	152.6517	0	152.6997	2	2	0	2	1	0	0	139.7536	139.7536	380.2994	7	PROCESSED	57612.009537037	2016-08-12 00:13:44	56383	2013-04-01 00:00:00	56509.8769097222	2013-08-05 21:02:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081315	We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		USA	8	AO8	LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508072020/	Quick Look
436	Q0109-3518	17.9376	-35.0527	17.356449	-35.318066	0.204002	-38.849268	275.45528409	-80.96443984	40.3411	54606.0677199074	2008-05-20 01:37:31	54606.6772453704	2008-05-20 16:15:14	703037010	29.9585	18	29.9665	29.9585	0	29.9665	1	1	0	1	1	0	0	22.8339	22.8339	52.6559	1	PROCESSED	57542.5808101852	2016-06-03 13:56:22	54982	2009-05-31 00:00:00	54616.3810300926	2008-05-30 09:08:41	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031334	Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates.	EXTRAGALACTIC COMPACT SOURCES	7	A	GEORGE CHARTAS		USA	3	AO3	A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703037010/	Quick Look
437	G189 EAST	95.4705	22.4826	94.715097	22.507311	95.056054	-0.862354	189.63783855	3.93426331	258.2106	57096.5099652778	2015-03-15 12:14:21	57098.6780324074	2015-03-17 16:16:22	509036010	66.0529	85	66.0529	86.2237	0	86.2397	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.8236226852	2016-08-17 19:46:01	57524	2016-05-16 00:00:00	57157.5685416667	2015-05-15 13:38:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091314	We propose observations of G189.6+3.3, a large candidate supernova remnant (SNR) that overlaps with the much better studied remnant IC 443. Little is known about G189; ROSAT images show a shell-like structure about 1.5$^{circ}$ in diameter, but it has never been observed with modern X-ray telescopes. Its association, or lack thereof, with IC 443 is unknown. It may not be a supernova remnant at all; a superbubble origin for the X-ray emission also provides an intriguing possibility. Spatially-resolved spectroscopy with Suzaku will allow the detailed measurement of the plasma properties, illuminating the nature of this object. Determining the nature of G189 will help to probe the evolution of the ISM driven by the deaths of massive stars.	GALACTIC DIFFUSE EMISSION	5	B	BRIAN WILLIAMS		USA	9	AO9	OBSERVATIONS OF G189.6+3.3: AN SNR COMPANION TO IC 443?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509036010/	Quick Look
438	KES 69	278.2575	-10.136	277.567341	-10.174332	278.335469	13.065931	21.8245316	-0.57033928	267.6495	56927.2830902778	2014-09-27 06:47:39	56929.1391435185	2014-09-29 03:20:22	509037010	77.3795	80	77.3795	77.9708	0	77.9953	2	2	0	3	0	0	0	0	0	0	0	PROCESSED	57616.5892361111	2016-08-16 14:08:30	57345	2015-11-19 00:00:00	56979.4056944444	2014-11-18 09:44:12	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091315	We propose to conduct Suzaku observations of the Galactic supernova remnants (SNRs) Kes 69 (G21.8-0.6) and 3C 396 (G39.2-0.3). These SNRs were detected in the infrared by Spitzer and their infrared colors suggest that shocked molecules produce the observed emission. Published analyses of the X-ray emission from these SNRs (along with our own analysis of archival XMM-Newton and Chandra observations of these sources) reveals that the emission from both Kes 69 and 3C 396 is thermal and that they may both be mixed-morphology SNRs (MMSNRs) but deeper observations are needed to clarify their X-ray spectral properties. In particular, we will investigate whether these X-ray emitting plasmas are overionized, which is observed for other MMSNRs.	GALACTIC DIFFUSE EMISSION	5	A	THOMAS PANNUTI		USA	9	AO9	SUZAKU OBSERVATIONS OF THE SPITZER-DETECTED GALACTIC SUPERNOVA REMNANTS KES 69 (G21.8-0.6) AND 3C 396 (G39.2-0.3)	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509037010/	Quick Look
439	FERMI_JET_COCOON_2	320.2279	-29.504	319.485138	-29.716859	313.416673	-13.31861	17.00065384	-44.00205209	255.063	56981.4053356482	2014-11-20 09:43:41	56981.8683217593	2014-11-20 20:50:23	509048010	19.9032	20	19.9032	19.9032	0	19.9032	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57616.7951736111	2016-08-16 19:05:03	57362	2015-12-06 00:00:00	56995.5937268518	2014-12-04 14:14:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091322	The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way.	GALACTIC DIFFUSE EMISSION	5	C	MATTHEW MILLER		USA	9	AO9	OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509048010/	Quick Look
440	DIFFUSE1E	200.6072	7.3824	199.979251	7.643505	196.163547	14.87503	324.76377809	68.9302329	123.5311	57011.0086458333	2014-12-20 00:12:27	57011.5252083333	2014-12-20 12:36:18	509062010	23.9762	20	23.9762	24.5362	0	24.5362	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57617.5495023148	2016-08-17 13:11:17	57475	2016-03-28 00:00:00	57107.4289583333	2015-03-26 10:17:42	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091324	In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them.	GALACTIC DIFFUSE EMISSION	5	C	JOEL BREGMAN		USA	9	AO9	UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509062010/	Quick Look
441	VELA FRAGMENT C	136.2696	-44.691	135.819541	-44.490549	161.57955	-57.213344	266.51473212	1.58715492	269.3614	54580.6978703704	2008-04-24 16:44:56	54582.3056481482	2008-04-26 07:20:08	503095010	84.1167	70	84.1167	84.1167	0	84.1167	2	2	0	2	1	0	0	91.3547	91.3547	138.9018	2	PROCESSED	57542.4305439815	2016-06-03 10:19:59	54960	2009-05-09 00:00:00	54594.2480324074	2008-05-08 05:57:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031212	Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM.	GALACTIC DIFFUSE EMISSION	5	B	TERRANCE GAETZ		USA	3	AO3	SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503095010/	Quick Look
442	3C120	68.2984	5.3555	67.633855	5.251051	67.433469	-16.402094	190.37315865	-27.39441526	237.4585	53775.1527199074	2006-02-09 03:39:55	53776.2433217593	2006-02-10 05:50:23	700001010	41.9321	160	41.9321	41.9321	41.9321	41.9321	2	2	2	2	1	0	0	34.0941	34.0941	94.2219	1	PROCESSED	57532.9769791667	2016-05-24 23:26:51	54247	2007-05-27 00:00:00	53906.2470601852	2006-06-20 05:55:46	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001003	Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate.	EXTRAGALACTIC COMPACT SOURCES	7	A	JUN KATAOKA		JAP	0	SWG	BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700001010/	Quick Look
443	PKS2155-304	329.7191	-30.2247	328.99529	-30.464273	321.189186	-16.770975	17.73226544	-52.24760927	254.1358	53704.7749884259	2005-11-30 18:35:59	53706.3613888889	2005-12-02 08:40:24	700012010	63.9114	80	63.9194	63.9114	63.9194	63.9166	2	2	2	2	1	0	0	58.0114	58.0114	137.0498	3	PROCESSED	57532.3797685185	2016-05-24 09:06:52	54247	2007-05-27 00:00:00	54038.8920138889	2006-10-30 21:24:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001100	Jets in blazars are believed to be a powerful site of particle acceleration. TeV emitting blazars are very important, because we can study very end of electron distribution near the maximum energy by using X-ray spectrum, because X-ray emission is believed to be due to synchrotron emission from the higher energy electron. Comparison of spectral index between X-ray and TeV gives us a crucial information on these source, because this is very sensitive to the particle injection and rapid cooling. In order to maximize the capability of sensitive hard X-ray observations of Suzaku, we propose reserved TOO observations for the next six months of PV phase from the TeV emitting blazars established by HESS, selected from five candidates.	EXTRAGALACTIC COMPACT SOURCES	7	A	TADAYUKI TAKAHASHI		JAP	0	SWG-TOO	RESERVED TOO OBSERVATIONS OF SELECTED TEV-BRIGHT BLAZARS	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700012010/	Quick Look
444	ANTLIA E1	157.8782	-35.3295	157.312453	-35.072071	176.074864	-40.746998	273.21530285	19.3432713	277.4995	56091.5629398148	2012-06-13 13:30:38	56092.2633912037	2012-06-14 06:19:17	807066010	25.747	23	25.755	25.747	0	25.755	2	2	0	2	1	0	0	22.9291	22.9291	60.5139	1	PROCESSED	57605.6597106482	2016-08-05 15:49:59	56473	2013-06-30 00:00:00	56107.272650463	2012-06-29 06:32:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071521	We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	7	AO7	MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807066010/	Quick Look
445	HESS J1809-193B	272.6789	-19.1585	271.941455	-19.169725	272.527802	4.258732	11.32661741	-0.06027609	269.0544	55084.4838773148	2009-09-10 11:36:47	55085.7488310185	2009-09-11 17:58:19	504078010	52.4748	50	52.4748	52.4748	0	52.4748	2	2	0	2	1	0	0	43.3733	43.3733	109.2758	1	PROCESSED	57548.5486226852	2016-06-09 13:10:01	55475	2010-10-06 00:00:00	55109.4280555556	2009-10-05 10:16:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041303	We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background.	GALACTIC DIFFUSE EMISSION	5	A	OLEG KARGALTSEV		USA	4	AO4	CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504078010/	Quick Look
446	330.2+1.0	240.2384	-51.525	239.295706	-51.384773	249.047523	-30.224565	330.18352169	1.02987491	98.9027	55239.832025463	2010-02-12 19:58:07	55242.125150463	2010-02-15 03:00:13	504083030	92.505	30	92.513	92.505	0	92.521	2	2	0	2	1	0	0	86.0965	86.0965	198.0897	4	PROCESSED	57550.6564699074	2016-06-11 15:45:19	55622	2011-03-02 00:00:00	55253.5397685185	2010-02-26 12:57:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041312	Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity.	GALACTIC DIFFUSE EMISSION	5	B	GLENN ALLEN		USA	4	AO4	MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504083030/	Quick Look
447	NGC 526A	20.9794	-35.0729	20.408158	-35.333404	3.010528	-40.076485	263.77547728	-79.45131683	257.0195	55578.7592939815	2011-01-17 18:13:23	55580.6404050926	2011-01-19 15:22:11	705044010	72.9346	70	72.9346	72.9346	0	72.9346	2	2	0	2	1	0	0	63.1372	63.1372	162.4977	2	PROCESSED	57600.6980324074	2016-07-31 16:45:10	55961	2012-02-04 00:00:00	55595.4905671296	2011-02-03 11:46:25	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051434	The Compton-thin NELG NGC 526a has large hard X-ray variability and likely an abnormally flat photon index, Gamma near 1.6. We request two observations of 70 ks each, spaced six months apart, to accurately constrain Compton reflection and obtain geometrical constraints on the accreting material to test Seyfert unification schemes, as well as constrain coronal power law parameters. Importantly, we will track long-term spectral variability to constrain the location and nature of the reflecting material. We also will resolve the moderately broad Fe K alpha line, which may indicate the presence of a truncated accretion disk, and thus constrain the amount of reflection off an accretion disk versus that from a torus.	EXTRAGALACTIC COMPACT SOURCES	7	C	ALEX MARKOWITZ		USA	5	AO5	COMPTON REFLECTION AND LONG-TERM SPECTRAL VARIABILITY IN THE SEYFERT AGN NGC 526A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705044010/	Quick Look
448	MARKARIAN 335	1.5539	20.2624	0.911019	19.984083	9.744165	17.917566	108.74842011	-41.36053721	68.4831	53907.0624537037	2006-06-21 01:29:56	53910.7585532407	2006-06-24 18:12:19	701031010	151.2884	150	151.2964	151.2884	151.2964	151.2964	2	2	2	2	1	0	0	140.9812	140.9812	319.3028	4	PROCESSED	57534.8340046296	2016-05-26 20:00:58	54401	2007-10-28 00:00:00	53928.5392361111	2006-07-12 12:56:30	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011323	We propose to observe the two Seyfert 1 galaxies Mrk 335 and ESO198-G024 for a total exposure of 150 ks each with the high sensitivity and broad band coverage of the Suzaku satellite. Both sources show a broad Fe K line and a strong soft excess. One appealing explanation for the nature of the soft excess is reflection. Fundamental to this hypothesis is the assumption that the same self-consistent reflection spectrum explains the Fe K line (including its shape), the soft excess, and also the Compton reflection hump above 20 keV. Suzaku's ability to measure all three reflection components simultaneously enables the different spectral models to be disentangled and reflection to be strongly tested. Understanding black hole accretion is fundamental to NASA's "SEU" theme.	EXTRAGALACTIC COMPACT SOURCES	7	B	JON MILLER		USA	1	AO1	REVEALING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701031010/	Quick Look
449	NGC 1068	40.6928	-0.0667	40.052721	-0.278811	38.248989	-15.097296	172.18986515	-51.95763403	248.588	54141.0038078704	2007-02-10 00:05:29	54141.9168287037	2007-02-10 22:00:14	701039010	41.6229	35	41.6309	41.6309	0	41.6229	2	2	0	2	1	0	0	41.8024	41.8024	78.8839	0	PROCESSED	57537.346875	2016-05-29 08:19:30	54525	2008-02-29 00:00:00	54151.5012962963	2007-02-20 12:01:52	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011333	The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB.	EXTRAGALACTIC COMPACT SOURCES	7	C	AARON STEFFEN		USA	1	AO1	MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701039010/	Quick Look
450	VELA SNR CB-LBG	130.6266	-44.6167	130.194556	-44.436193	154.988854	-59.23497	263.87788945	-1.43970243	293.482	55319.3460648148	2010-05-03 08:18:20	55319.7940046296	2010-05-03 19:03:22	505071010	27.1799	20	27.1799	27.1799	0	27.1799	2	2	0	2	1	0	0	25.0945	25.0945	38.6939	1	PROCESSED	57551.3691203704	2016-06-12 08:51:32	55696	2011-05-15 00:00:00	55330.1543981482	2010-05-14 03:42:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051304	The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	5	AO5	IRON-RICH EJECTA BULLET IN THE VELA SNR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505071010/	Quick Look
451	NGC 4593	189.9131	-5.3426	189.268208	-5.068085	191.201579	-0.987759	297.48049807	57.40434975	112.24	54449.1962384259	2007-12-15 04:42:35	54451.972349537	2007-12-17 23:20:11	702040010	118.8415	107	118.8415	118.8415	0	118.8415	2	2	0	2	1	0	0	108.976	108.976	239.7899	6	PROCESSED	57540.92	2016-06-01 22:04:48	54829	2008-12-29 00:00:00	54462.4425462963	2007-12-28 10:37:16	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021302	We propose a 80 ksec observation of the bright Seyfert 1 NGC 4593 to resolve the moderately relativistic Fe K line, and test for a truncated or ionized accretion disk. To achieve accurate modeling of the broad Fe line, Suzaku's broad bandpass is required to deconvolve the broadband emitting component and accurately constrain the continuum. NGC 4593 is one of the few Seyferts to also show evidence for Fe XXVI emission at 6.9 keV; we will use the XIS to confirm the line and constrain its origin. If the thin accretion disk is truncated or transitions to an ADAF, it would reveal NGC 4593 to be an analogue of low/hard-state X-ray Binaries.	EXTRAGALACTIC COMPACT SOURCES	7	C	ALEX MARKOWITZ		USA	2	AO2	DOES THE SEYFERT AGN NGC 4593 HAVE A TRUNCATED OR IONIZED ACCRETION DISK?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702040010/	Quick Look
452	NGC7582	349.5472	-42.3304	348.858747	-42.603943	331.723267	-34.368393	348.20905034	-65.68466064	49.5845	54221.7937384259	2007-05-01 19:02:59	54222.3176273148	2007-05-02 07:37:23	702052010	23.9412	25	23.9572	23.9412	0	23.9572	2	2	0	2	1	0	0	21.5816	21.5816	45.256	0	PROCESSED	57538.5368402778	2016-05-30 12:53:03	54695	2008-08-17 00:00:00	54228.073275463	2007-05-08 01:45:31	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021332	We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARCO CHIABERGE		USA	2	AO2	MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052010/	Quick Look
453	NGC7582	349.6446	-42.4137	348.956435	-42.687331	331.752163	-34.475865	347.94526846	-65.70277041	233.1822	54413.9093981482	2007-11-09 21:49:32	54414.6459490741	2007-11-10 15:30:10	702052030	29.3538	25	29.3538	29.3538	0	29.3538	2	2	0	2	1	0	0	24.4331	24.4331	63.6319	1	PROCESSED	57540.4723842593	2016-06-01 11:20:14	54790	2008-11-20 00:00:00	54423.1929398148	2007-11-19 04:37:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021332	We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARCO CHIABERGE		USA	2	AO2	MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052030/	Quick Look
454	NGC7582	349.6411	-42.4153	348.952917	-42.688928	331.748482	-34.476047	347.94523476	-65.69973119	236.7954	54420.0722337963	2007-11-16 01:44:01	54420.8960532407	2007-11-16 21:30:19	702052040	31.8955	25	31.8955	31.8955	0	31.8955	2	2	0	2	1	0	0	25.7806	25.7806	71.1719	0	PROCESSED	57540.5407060185	2016-06-01 12:58:37	54797	2008-11-27 00:00:00	54430.3041203704	2007-11-26 07:17:56	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021332	We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARCO CHIABERGE		USA	2	AO2	MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702052040/	Quick Look
455	3C 33	17.2445	13.2796	16.584921	13.013252	20.958615	5.507742	129.4936436	-49.368548	249.2604	54460.3029282407	2007-12-26 07:16:13	54463.6390509259	2007-12-29 15:20:14	702059010	127.3677	100	127.3757	127.3757	0	127.3677	2	2	0	2	1	0	0	106.5885	106.5885	288.2036	7	PROCESSED	57541.0545833333	2016-06-02 01:18:36	54854	2009-01-23 00:00:00	54483.4886458333	2008-01-18 11:43:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021356	We propose a 100 ks Suzaku observation of the nucleus of the nearby (z=0.0597) FRII radio galaxy 3C 33, to constrain the nature of its Compton reflection component, and make an accurate measurement of its Fe Ka emission line. 3C 33 (awarded category-C time in Suzaku AO-1, not observed) is the only radio-loud AGN with evidence of Compton reflection in its low-energy (< 10 keV) spectrum, and so offers a unique opportunity to study both the soft- and hard-band properties of reflection. The HXD will allow us, for the first time, to constrain the nature of the Compton reflection component in 3C 33 and, when combined with the superb sensitivity of the XIS, will enable us to determine the line-of-sight geometry and structure of the reflecting region.	EXTRAGALACTIC COMPACT SOURCES	7	B	DANIEL EVANS		USA	2	AO2	CONSTRAINING THE REFLECTION PROPERTIES OF THE NARROW-LINE RADIO GALAXY 3C 33	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702059010/	Quick Look
456	Q1017+1055	155.041	10.671	154.377707	10.922699	152.99156	0.282434	230.36219873	50.83483368	121.1263	54431.9135185185	2007-11-27 21:55:28	54432.4376851852	2007-11-28 10:30:16	702064010	18.0486	20	18.0486	18.0486	0	18.0486	2	2	0	2	1	0	0	15.0316	15.0316	45.2819	0	PROCESSED	57540.6059606482	2016-06-01 14:32:35	54805	2008-12-05 00:00:00	54438.285150463	2007-12-04 06:50:37	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021361	The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars.	EXTRAGALACTIC COMPACT SOURCES	7	C	GEORGE CHARTAS		USA	2	AO2	AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702064010/	Quick Look
457	3C 273	187.2559	1.9961	186.616492	2.272457	185.868054	4.712799	289.92713501	64.30042167	293.1671	54281.0022569444	2007-06-30 00:03:15	54282.2661342593	2007-07-01 06:23:14	702070010	54.8927	67	54.8927	54.8927	0	54.8927	2	2	0	2	1	0	0	51.2592	51.2592	109.1439	1	PROCESSED	57539.0801388889	2016-05-31 01:55:24	54695	2008-08-17 00:00:00	54322.4904166667	2007-08-10 11:46:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021364	We propose a Suzaku campaign on the bright z=0.158 quasar 3C 273. The source exhibits a Seyfert-like X-ray spectrum when the luminosity is low but is dominated by emission from the jet in a high state. Suzaku will be able to measure the broadband spectrum, especially X-ray reprocessed features, with greater sensitivity than ever before. Decoupling and monitoring of the disk and jet components will enable detailed spectroscopy to help understand the disk-jet connection and the wider implications for AGN physics in general. The target is bright and well-suited because for most AGN either the disk or jet component dominates. For this pilot study we propose two 50 ks observations, one in each visibility window. The science goals cannot be achieved with existing data or other missions.	EXTRAGALACTIC COMPACT SOURCES	7	C	TAHIR YAQOOB		USA	2	AO2	EXPLORING THE ACCRETION DISK AND JET CONNECTION IN 3C 273 WITH SUZAKU	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702070010/	Quick Look
458	SWIFT J0318.7+6828	49.4315	68.5395	48.26024	68.35635	69.167768	48.016071	135.6962435	9.37350025	42.3301	54365.4488078704	2007-09-22 10:46:17	54367.125162037	2007-09-24 03:00:14	702075010	77.1156	53	77.1396	77.1156	0	77.1396	2	2	0	2	1	0	0	70.6855	70.6855	144.7978	1	PROCESSED	57540.0779513889	2016-06-01 01:52:15	54770	2008-10-31 00:00:00	54403.1984490741	2007-10-30 04:45:46	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021372	The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs.	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	2	AO2	SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702075010/	Quick Look
459	VELA PWN E6	131.2685	-45.4809	130.840764	-45.298021	156.629635	-59.743456	264.83769354	-1.61837696	304.5065	55712.9576273148	2011-05-31 22:58:59	55713.2292939815	2011-06-01 05:30:11	506049010	18.1968	15	18.2048	18.1968	0	18.2128	2	2	0	2	1	0	0	14.209	14.209	23.4699	0	PROCESSED	57602.1814699074	2016-08-02 04:21:19	56103	2012-06-25 00:00:00	55735.9387268518	2011-06-23 22:31:46	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061302	Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles.	GALACTIC DIFFUSE EMISSION	5	B	SATORU KATSUDA		USA	6	AO6	THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506049010/	Quick Look
460	NGC 4051	180.7952	44.5393	180.156844	44.817625	159.255387	40.346248	148.86124636	70.08047443	126.4079	54793.7	2008-11-23 16:48:00	54795.572025463	2008-11-25 13:43:43	703023020	78.3855	70	78.3935	78.3855	0	78.3939	1	1	0	1	1	0	0	62.7604	62.7604	161.7358	0	PROCESSED	57544.5729513889	2016-06-05 13:45:03	54557	2008-04-01 00:00:00	54811.74875	2008-12-11 17:58:12	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031014	The powerful combination of Principal Components Analysis with time-resolved X-ray spectroscopy of Seyfert AGN has shown strong evidence that changes in a complex absorber are the origin of much of observed AGN spectral and flux variability. Large column, high ionization layers of gas may arise in a disk wind, representing a significant new, and possibly dominant, component, responsible for shaping the X-ray spectrum of AGN. The broad bandpass of Suzaku gives us a unique opportunity to model primary and reflected continua and the effects of variable absorbing zones, and test wind and other models. We propose a long 340 ks exposure on the NLSy1 NGC 4051 whose large amplitude of variability and well-studied complex absorption will test those models to the limit	EXTRAGALACTIC COMPACT SOURCES	7	A	TRACEY TURNER		USA	3	AO3	DECONSTRUCTING SEYFERT SPECTRA - TIME FOR A PARADIGM SHIFT?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703023020/	Quick Look
461	SMC X-1	19.2829	-73.4465	18.951639	-73.709645	312.337269	-66.476032	300.41108523	-43.55576838	356.8796	55658.8646759259	2011-04-07 20:45:08	55659.2447106482	2011-04-08 05:52:23	706030010	18.4662	18	18.4662	18.55	0	18.5448	1	1	0	1	1	0	0	15.5577	15.5577	32.8239	0	PROCESSED	57601.4235185185	2016-08-01 10:09:52	56040	2012-04-23 00:00:00	55673.2343055556	2011-04-22 05:37:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030010/	Quick Look
462	SMC X-1	19.2476	-73.446	18.915775	-73.709202	312.329896	-66.466401	300.42473809	-43.55764171	6.4299	55669.2561805556	2011-04-18 06:08:54	55669.705775463	2011-04-18 16:56:19	706030020	17.2769	18	17.2769	17.2849	0	17.4844	2	2	0	1	1	0	0	17.6646	17.6646	38.8159	0	PROCESSED	57601.5313657407	2016-08-01 12:45:10	56058	2012-05-11 00:00:00	55691.1543171296	2011-05-10 03:42:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030020/	Quick Look
463	NGC 7172	330.5062	-31.8708	329.778877	-32.112297	321.223494	-18.549637	15.12698367	-53.06449716	59.7356	54611.0658680556	2008-05-25 01:34:51	54612.8558217593	2008-05-26 20:32:23	703030010	82.2797	80	82.2797	82.2877	0	82.2877	2	2	0	2	1	0	0	71.7465	71.7465	154.6338	0	PROCESSED	57542.6661805556	2016-06-03 15:59:18	54999	2009-06-17 00:00:00	54633.7016203704	2008-06-16 16:50:20	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031322	X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s.	EXTRAGALACTIC COMPACT SOURCES	7	A	VALENTINA BRAITO		USA	3	AO3	THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703030010/	Quick Look
464	NGC 3281	157.9591	-34.9074	157.391937	-34.649823	175.881528	-40.345828	273.03211125	19.73409342	278.2413	54607.8508449074	2008-05-21 20:25:13	54609.2287615741	2008-05-23 05:29:25	703033010	46.234	40	46.242	46.25	0	46.234	2	2	0	2	1	0	0	41.4549	41.4549	119.038	0	PROCESSED	57542.6257175926	2016-06-03 15:01:02	54988	2009-06-06 00:00:00	54620.2890162037	2008-06-03 06:56:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031323	The classical unified model predicts only one type of Seyfert II (Sy2). Recent observations of SWIFT BAT-detected AGN found at least 4 classes of Sy2s: (1) objects with high column density and scattered soft x-rays, (2) Compton thick objects, (3) `hidden' AGN (Ueda et al. 2007), and (4) the `changing look' objects (Risaliti et al. 2006). The nature of these sources can only be revealed with high quality broad-band X-ray spectra from Suzaku. Thus, we are proposing 40ks observations for 2 of the brightest BAT AGN without high quality data, NGC 788, a type (3) object showing polarized optical broad lines, and NGC 3281, a classified (2) object. Such observations are necessary to build a reasonably large sample of high-quality, broad-band Sy2 spectra covering the range of X-ray/optical types.	EXTRAGALACTIC COMPACT SOURCES	7	A	RICHARD MUSHOTZKY		USA	3	AO3	SUZAKU OBSERVATIONS OF X-RAY BRIGHT TYPE II AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703033010/	Quick Look
465	3C279	194.0699	-5.7328	193.422743	-5.462367	195.164566	0.26232	305.15066173	57.11808922	113.6425	54854.8772222222	2009-01-23 21:03:12	54856.125162037	2009-01-25 03:00:14	703049020	56.937	200	56.937	56.937	0	56.937	2	2	0	2	1	0	0	12.6263	12.6263	107.7799	2	PROCESSED	57545.3327777778	2016-06-06 07:59:12	55328	2010-05-12 00:00:00	54880.5584259259	2009-02-18 13:24:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031346	We propose a 200 ks observation of 3C279, the archetypal EGRET blazar to be conducted simultaneously with GLAST as well as many other facilities, with the goal of obtaining broadband spectra and light-curves. The flux in all observable bands is known to be rapidly variable, but the information regarding the correlation between the time history of flux in various bands is limited, and the proposed observations are designed to remedy this shortcoming. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles.	EXTRAGALACTIC COMPACT SOURCES	7	A	GRZEGORZ MADEJSKI		USA	3	AO3	SUZAKU AND GLAST OBSERVATIONS OF 3C279	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703049020/	Quick Look
466	NGC985	38.6279	-8.738	38.014145	-8.956444	33.218289	-22.635173	180.72422437	-59.4803664	62.3866	55027.6174884259	2009-07-15 14:49:11	55028.5925231482	2009-07-16 14:13:14	704042010	31.9969	30	31.9969	32.0063	0	32.0063	2	2	0	2	1	0	0	25.7241	25.7241	84.2379	1	PROCESSED	57547.8515856482	2016-06-08 20:26:17	55406	2010-07-29 00:00:00	55040.2752430556	2009-07-28 06:36:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041414	We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc.	EXTRAGALACTIC COMPACT SOURCES	7	B	EZEQUIEL TREISTER		USA	4	AO4	THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704042010/	Quick Look
467	COMA NW6.5	194.0774	29.5523	193.474522	29.822643	179.856398	32.45513	99.36309014	87.34957637	319.9974	55734.7422685185	2011-06-22 17:48:52	55735.2522569444	2011-06-23 06:03:15	806045010	15.5013	15	15.5013	15.5151	0	15.5093	2	2	0	2	1	0	0	17.3764	17.3764	44.0599	0	PROCESSED	57602.3928587963	2016-08-02 09:25:43	55652	2011-04-01 00:00:00	55768.3250231482	2011-07-26 07:48:02	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806045010/	Quick Look
468	ABELL 1795	207.2241	26.601	206.646901	26.849155	193.922602	34.994161	33.84733119	77.1817764	130.8638	53714.5034259259	2005-12-10 12:04:56	53714.7752199074	2005-12-10 18:36:19	800012010	13.0982	120	13.1062	13.0982	13.1062	13.1062	1	1	1	1	1	0	0	10.3759	10.3759	23.4639	1	PROCESSED	57532.3922453704	2016-05-24 09:24:50	54247	2007-05-27 00:00:00	54038.7903703704	2006-10-30 18:58:08	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012010/	Quick Look
469	CEN A S LOBE NO. 4	196.751	-45.1436	196.031726	-44.876448	214.740849	-34.712794	305.81117883	17.64110832	288.0039	55421.3479282407	2010-08-13 08:21:01	55421.67375	2010-08-13 16:10:12	705035010	20.642	20	20.642	20.65	0	20.658	1	1	0	1	1	0	0	18.9643	18.9643	28.1439	0	PROCESSED	57552.9465277778	2016-06-13 22:43:00	55803	2011-08-30 00:00:00	55435.1577314815	2010-08-27 03:47:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051401	We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays).	EXTRAGALACTIC COMPACT SOURCES	7	B	GRZEGORZ MADEJSKI		USA	5	AO5	SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705035010/	Quick Look
470	IRAS 00397-1312	10.5707	-12.9503	9.941553	-13.224287	4.464578	-16.066781	113.89016485	-75.66108211	246.4295	55558.1361342593	2010-12-28 03:16:02	55560.2501388889	2010-12-30 06:00:12	705046010	83.7928	90	83.7928	83.7928	0	83.7928	2	2	0	2	1	0	0	71.9314	71.9314	182.6317	1	PROCESSED	57632.5965856482	2016-09-01 14:19:05	56040	2012-04-23 00:00:00	55670.3615046296	2011-04-19 08:40:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051441	We propose two Suzaku-HXD observations of two ULIRGs hosting a deeply buried AGN. These two objects are expected to host a powerful AGN in the luminosity range of quasars, based on solid evidence from mid-IR Spitzer spectroscopy. However, these sources are completely buried behind a screen of dust with column density in excess of 10^24 cm^-2, so not only the primary emission below 10 keV is obscured, but the reflected emission, usually ascribed to a circumnuclear "torus", is also absent. This suggests a complete spherical coverage of the X-ray source along all directions. The unique capabilities of Suzaku at high energies will allow to confirm the existence of these objects, representing the most extreme examples of buried AGNs, both in terms of obscuration and of intrinsic luminosity.	EXTRAGALACTIC COMPACT SOURCES	7	C	GUIDO RISALITI		USA	5	AO5	BURIED QUASAR 2S INSIDE ULIRGS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705046010/	Quick Look
471	NGC 4945	196.3415	-49.5274	195.611435	-49.259681	217.040288	-38.699914	305.25336122	13.28155854	286.7821	55386.9936226852	2010-07-09 23:50:49	55388.2626388889	2010-07-11 06:18:12	705047020	44.1517	40	44.1517	44.1597	0	44.1517	2	2	0	2	1	0	0	40.1612	40.1612	109.434	0	PROCESSED	57552.6167824074	2016-06-13 14:48:10	55777	2011-08-04 00:00:00	55411.4916898148	2010-08-03 11:48:02	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051442	We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval.	EXTRAGALACTIC COMPACT SOURCES	7	B	GUIDO RISALITI		USA	5	AO5	HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047020/	Quick Look
472	NGC 4945	196.2918	-49.5144	195.562046	-49.246615	216.996084	-38.704359	305.2209968	13.29631795	319.7988	55438.8990277778	2010-08-30 21:34:36	55439.9896990741	2010-08-31 23:45:10	705047040	39.3859	40	39.3859	39.3859	0	39.3859	2	2	0	2	1	0	0	35.7823	35.7823	94.2239	0	PROCESSED	57553.267962963	2016-06-14 06:25:52	55815	2011-09-11 00:00:00	55449.2596296296	2010-09-10 06:13:52	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051442	We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval.	EXTRAGALACTIC COMPACT SOURCES	7	B	GUIDO RISALITI		USA	5	AO5	HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705047040/	Quick Look
473	ESP 39607	11.5922	-40.0968	10.997666	-40.369881	351.254657	-40.701682	307.24150307	-76.98900447	243.1952	55549.7680208333	2010-12-19 18:25:57	55551.3175810185	2010-12-21 07:37:19	705048010	60.6687	60	60.6927	60.6687	0	60.6847	2	2	0	2	1	0	0	48.9555	48.9555	133.8399	3	PROCESSED	57554.5018402778	2016-06-15 12:02:39	55960	2012-02-03 00:00:00	55593.2278472222	2011-02-01 05:28:06	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051443	We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec.	EXTRAGALACTIC COMPACT SOURCES	7	C	WAYNE BAUMGARTNER		USA	5	AO5	SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705048010/	Quick Look
474	3C 433	320.9422	25.055	320.383545	24.83969	333.197862	37.998992	74.46917661	-17.70913692	252.1178	55506.5663310185	2010-11-06 13:35:31	55508.0953472222	2010-11-08 02:17:18	705050010	62.5009	60	62.54	62.5009	0	62.54	2	2	0	2	1	0	0	44.4271	44.4271	132.0698	0	PROCESSED	57554.0198958333	2016-06-15 00:28:39	55890	2011-11-25 00:00:00	55524.1485416667	2010-11-24 03:33:54	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051443	We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec.	EXTRAGALACTIC COMPACT SOURCES	7	C	WAYNE BAUMGARTNER		USA	5	AO5	SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705050010/	Quick Look
475	0509-67.5	77.4163	-67.5163	77.433384	-67.576954	343.17919	-85.012675	278.13367069	-34.57909379	302.8449	56393.0595949074	2013-04-11 01:25:49	56397.1258912037	2013-04-15 03:01:17	508072010	175.9192	320	175.9352	175.9192	0	175.9432	2	2	0	2	1	0	0	166.6668	166.6668	351.2916	3	PROCESSED	57611.1504513889	2016-08-11 03:36:39	56383	2013-04-01 00:00:00	56425.6930439815	2013-05-13 16:37:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081315	We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics.	GALACTIC DIFFUSE EMISSION	5	B	HIROYA YAMAGUCHI		USA	8	AO8	LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508072010/	Quick Look
476	MBM16-OFF	46.1075	13.1563	45.420617	12.96209	47.406639	-4.032974	165.8625544	-38.38773927	69.5985	56513.919849537	2013-08-09 22:04:35	56515.9119791667	2013-08-11 21:53:15	508073010	83.0565	80	83.0565	83.0565	0	83.0565	2	2	0	2	1	0	0	81.1386	81.1386	172.0979	2	PROCESSED	57612.2143981482	2016-08-12 05:08:44	56953	2014-10-23 00:00:00	56587.5588541667	2013-10-22 13:24:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081322	We propose the observation of three off-cloud targets near the targets of the Solar Wind Charge Exchange (SWCX) Key Project to study the properties of the Diffuse X-ray Background below 1 keV, with particular focus on the characterization of the Galactic Halo. The Key Project targets are at a distance of a few hundreds pc from the Sun and their high density portions shields about 90% of X-rays at the O VII energy, our proposed targets, instead, shield only about 50% of the Galactic Halo emission. The contrast between on- and off-cloud allows us to disentangle the foreground and background emissions. In particular we will focus on the properties of the galactic halo, which dominates the oxygen background emission.	GALACTIC DIFFUSE EMISSION	5	A	EUGENIO URSINO		USA	8	AO8	PROPERTIES OF THE GALACTIC HALO THROUGH SHADOW OBSERVATIONS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508073010/	Quick Look
477	Z8852	347.6318	7.5789	346.999079	7.307292	351.631711	11.858062	84.17423864	-47.55525942	260.3346	54065.5867013889	2006-11-26 14:04:51	54066.1543287037	2006-11-27 03:42:14	801074010	14.8526	15	14.8526	14.8526	0	14.8526	2	2	0	2	1	0	0	13.9834	13.9834	49.0379	0	PROCESSED	57536.1918402778	2016-05-28 04:36:15	54695	2008-08-17 00:00:00	54088.6000694444	2006-12-19 14:24:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801074010/	Quick Look
478	WISE J1819+4532	274.9137	45.5584	274.555701	45.535406	279.54226	68.836144	73.38480627	24.31157427	77.6532	56020.3333333333	2012-04-03 08:00:00	56021.0070833333	2012-04-04 00:10:12	707038010	30.8819	30	30.8819	30.8819	0	30.8819	2	2	0	2	1	0	0	27.564	27.564	58.2039	0	PROCESSED	57605.0974537037	2016-08-05 02:20:20	56399	2013-04-17 00:00:00	56033.2380787037	2012-04-16 05:42:50	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071443	We request a 30-ks observation of WISE J1819+4532, an extreme WISE-selected AGN at z=2.031. This source stands out even amongst the rare WISE-selected sources we have been targeting: at mid-IR wavelengths, WISE J1819+4532 is ~10x brighter than similarly selected WISE sources, and more than 50x brighter than extreme Spitzer-selected sources. Assuming the local mid-IR to hard X-ray correlations, the implied intrinsic hard X-ray luminosity is L(2-10)~3e46 erg/s. WISE J1819+4532 is optically faint and the optical spectrum shows a typical obscured AGN with narrow emission lines. However, the object is infrared bright and the near-IR spectrum shows broad H-alpha emission. This implies that WISE J1819+4532 is a rare example of a an extremely luminous, semi-obscured AGN.	EXTRAGALACTIC COMPACT SOURCES	7	A	DANIEL STERN		USA	7	AO7	WISE J1819+4532: AN OBSCURED, HYPERLUMINOUS ULIRG/AGN AT Z~2	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707038010/	Quick Look
479	ZW229-15	286.3333	42.4706	285.936982	42.393229	298.560222	64.301193	73.09172558	15.5517204	34.6696	55715.0128356482	2011-06-03 00:18:29	55719.6251736111	2011-06-07 15:00:15	706035010	167.0838	165	168.6766	167.0838	0	168.6846	2	2	0	2	1	0	0	218.1832	218.1832	398.4357	2	PROCESSED	57602.3250694445	2016-08-02 07:48:06	56127	2012-07-19 00:00:00	55757.7055671296	2011-07-15 16:56:01	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061414	The optical emission from AGN is though to be a combination of direct radiation from an accretion disk and reprocessed x-ray emission. Separating these components requires simultaneous high-precision x-ray/optical monitoring, which has heretofore not been achieved. We propose to gather this necessary data via simultaneous optical and x-ray monitoring of the Sy 1 galaxy Zw 229-15. Kepler is monitoring Zw 229-15 every 30 minutes with unprecedented 99% duty cycle and 0.1% repeatability. The key missing data is an appropriate x-ray campaign. We propose a 64-orbit (165 ks) Suzaku long-look combined with a series of 48 Swift visits to probe lags of 0.1-10 days. This will be the first experiment sensitive to such short lags and thus will critically test the present disc/reprocessing paradigm	EXTRAGALACTIC COMPACT SOURCES	7	B	RICHARD MUSHOTZKY		USA	6	AO6	SIMULTANEOUS SUZAKU/SWIFT/ KEPLER MONITORING OF ZW 229-15	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706035010/	Quick Look
480	A2495	342.5662	10.9218	341.941655	10.656649	348.262816	16.910805	81.19678392	-41.92445268	65.1354	54260.5857523148	2007-06-09 14:03:29	54261.1668287037	2007-06-10 04:00:14	801080020	25.7806	18	25.7806	25.7806	0	25.7806	2	2	0	2	1	0	0	20.9762	20.9762	50.1959	2	PROCESSED	57538.8757291667	2016-05-30 21:01:03	54695	2008-08-17 00:00:00	54270.430625	2007-06-19 10:20:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080020/	Quick Look
481	0528+134	82.7323	13.541	82.025359	13.504077	82.83368	-9.719507	191.35839601	-11.00951452	89.1633	55832.6802314815	2011-09-28 16:19:32	55833.0119444444	2011-09-29 00:17:12	706043010	14.7892	10	14.7892	14.7892	0	14.7892	2	2	0	2	1	0	0	15.8659	15.8659	28.6359	0	PROCESSED	57603.2623032407	2016-08-03 06:17:43	56225	2012-10-25 00:00:00	55875.6223958333	2011-11-10 14:56:15	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061601	We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	6	AO6	EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706043010/	Quick Look
482	G93.3+6.9 NW RIM	312.9527	55.5354	312.608547	55.346344	352.30712	67.106977	93.368132	7.08938459	52.0991	56814.8070023148	2014-06-06 19:22:05	56817.24125	2014-06-09 05:47:24	509040010	107.8986	100	107.9066	107.9066	0	107.8986	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57615.2100115741	2016-08-15 05:02:25	57236	2015-08-02 00:00:00	56869.6106481482	2014-07-31 14:39:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091316	We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN.	GALACTIC DIFFUSE EMISSION	5	C	MICHAEL STAGE		USA	9	AO9	G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509040010/	Quick Look
483	OFF-FIELD4	173.7625	-36.8508	173.145535	-36.574162	191.286304	-35.787139	286.33839516	23.54732297	109.4045	57008.1600925926	2014-12-17 03:50:32	57009.6814699074	2014-12-18 16:21:19	509045010	81.321	80	81.321	81.321	0	81.321	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.5308680556	2016-08-17 12:44:27	56748	2014-04-01 00:00:00	57112.4059490741	2015-03-31 09:44:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091321	Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma.	GALACTIC DIFFUSE EMISSION	5	C	ANJALI GUPTA		USA	9	AO9	CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509045010/	Quick Look
484	MCG-03-34-64	200.5996	-16.727	199.930176	-16.465808	205.288367	-7.470033	313.53711237	45.50625694	110.133	56296.8837384259	2013-01-04 21:12:35	56301.1737384259	2013-01-09 04:10:11	707027010	155.7127	150	155.7367	155.7127	0	155.7287	2	2	0	2	1	0	0	135.0516	135.0516	370.6038	4	PROCESSED	57608.5292824074	2016-08-08 12:42:10	56018	2012-04-01 00:00:00	56336.6958680556	2013-02-13 16:42:03	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071423	Analysis of Suzaku observations selected from the BAT 58-month catalog has shown extreme hard X-ray excesses to exist in ~70% of type 1 AGN, and these can be modeled by partial-covering of Compton-thick gas. This new result shows the importance of broad X-ray coverage, currently available only with Suzaku. The most extreme of the sample sources, MCG-03-34-64 and NGC 1194, show significant spectral and flux variability above 10 keV, likely attributable to changes in the Compton-thick absorber. We request new observations of MCG-03-34-64 (150 ks) and NGC 1194 (200 ks) to study the X-ray reprocessor in these extreme systems, confirm the high-energy spectral variability and constrain the nature and location of the Compton-thick absorber.	EXTRAGALACTIC COMPACT SOURCES	7	C	TRACEY TURNER		USA	7	AO7	THE CASE FOR VARIATIONS IN COMPTON-THICK ABSORPTION: MCG-03-34-64 AND NGC 1194	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707027010/	Quick Look
485	FERMI_JET_COCOON_5	306.4609	-33.261	305.672059	-33.424933	300.742491	-13.631284	9.28791468	-33.23258901	260.3818	56968.8506481482	2014-11-07 20:24:56	56969.3612847222	2014-11-08 08:40:15	509051010	22.0438	20	22.0518	22.0438	0	22.0573	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7478125	2016-08-16 17:56:51	57358	2015-12-02 00:00:00	56982.4350694445	2014-11-21 10:26:30	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091322	The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way.	GALACTIC DIFFUSE EMISSION	5	C	MATTHEW MILLER		USA	9	AO9	OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509051010/	Quick Look
486	H1821+643	275.4669	64.3595	275.403094	64.333117	318.334051	86.844268	94.01942058	27.4280098	65.0004	56402.5419444444	2013-04-20 13:00:24	56404.6925462963	2013-04-22 16:37:16	708037020	128.2485	400	128.2703	128.2485	0	128.2485	2	2	0	2	1	0	0	132.8215	132.8215	185.8058	2	PROCESSED	57611.1374884259	2016-08-11 03:17:59	56383	2013-04-01 00:00:00	56425.6256712963	2013-05-13 15:00:58	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081436	H1821+643 (z=0.297) is not "just another quasar". This luminous active galactic nucleus (AGN) is an extremely rare example of a powerful quasar at the center of a rich, cooling-core cluster of galaxies. As such, it may represent a key evolutionary stage in the complex interplay between AGN and the core regions of the intracluster medium (ICM). Our analysis of archival XMM-Newton data has found evidence for a relativistically broad iron line. Here, we build on this request deep (400ks) Suzaku spectroscopy of H1821+643 to (1) measure the spin of this supermassive black hole and (2) search for powerful highly ionized outflows. In addition to measuring spin in the most luminous and distant object yet, this will enable us to test key predictions of recent models for AGN feedback.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	8	AO8	THE BLACK HOLE SPIN AND IONIZED OUTFLOWS IN THE COOLING-FLOW QUASAR H1821+643	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708037020/	Quick Look
487	IRAS F11119+3257	168.6582	32.6829	167.981225	32.955487	156.042952	25.438757	192.21056175	68.35212615	301.5808	56425.1110185185	2013-05-13 02:39:52	56431.3329050926	2013-05-19 07:59:23	708038010	252.2992	250	252.3232	252.2992	0	252.3232	2	2	0	2	1	0	0	220.3036	220.3036	400.8599	10	PROCESSED	57611.4720717593	2016-08-11 11:19:47	56858	2014-07-20 00:00:00	56491.9181828704	2013-07-18 22:02:11	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081441	Recent Herschel observations provided a breakthrough in identifying powerful, large-scale molecular outflows in ULIRGs, indicating that AGN feedback can indeed have a strong impact on star formation and galaxy evolution, in accordance with theoretical models. However, observational evidence for the connection between the putative fast nuclear AGN winds required for the formation of these large-scale outflows is missing. X-ray observations of blue-shifted Fe K absorption lines directly probe ultra-fast outflows (UFOs) ejected from the AGN accretion disk with v>10,000km/s. A 250ks Suzaku exposure of the ULIRG F11119+3257 with observed extreme molecular/neutral/ionized outflows would allow to characterize the expected UFO, providing the "smoking gun" evidence for feedback driven by AGN winds.	EXTRAGALACTIC COMPACT SOURCES	7	A	FRANCESCO TOMBESI		USA	8	AO8	IRAS F11119+3257: THE "SMOKING GUN" EVIDENCE FOR AGN FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708038010/	Quick Look
488	UGC 03142	70.9469	28.9681	70.161272	28.87543	73.291585	6.626144	172.09277202	-10.99747628	264.8107	56335.692349537	2013-02-12 16:36:59	56336.9946296296	2013-02-13 23:52:16	707032010	51.2847	50	51.2847	51.2927	0	51.3007	2	2	0	2	1	0	0	47.5632	47.5632	112.51	1	PROCESSED	57610.6216898148	2016-08-10 14:55:14	56721	2014-03-05 00:00:00	56349.5963541667	2013-02-26 14:18:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071424	A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN.	EXTRAGALACTIC COMPACT SOURCES	7	C	TRACEY TURNER		USA	7	AO7	INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707032010/	Quick Look
489	MCG -5-23-16	146.9445	-30.9023	146.395049	-30.669659	162.619875	-41.096298	262.72964912	17.28396386	118.3849	53711.9526388889	2005-12-07 22:51:48	53714.4939699074	2005-12-10 11:51:19	700002010	95.6774	100	95.6774	95.7174	95.7174	95.6854	2	2	2	2	1	0	0	85.5647	85.5647	219.5251	3	PROCESSED	57532.4508680556	2016-05-24 10:49:15	54247	2007-05-27 00:00:00	54039.1988310185	2006-10-31 04:46:19	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001006	We request a 100ks Suzaku observation of the bright Seyfert galaxy, MCG -5-23-16 simultaneously with approved XMM-Newton and Chandra HETG observations in December 2005. MCG -5-23-16 has one of the best known examples of a relativistically broadened iron K line. With a Swift-BAT flux of 1.6e-10 cgs (15-100 keV), it is one of the brightest AGN above 10 keV. The simultaneous observations will allow us to determine the shape of the broad relativistic Fe line after subtracting the narrow line components measured by HETG. Importantly, Suzaku's wide bandpass will accurately measure the broad-band continuum and reflection component of MCG -5-23-16, essential for constraining the broad iron line. These observations will also allow us to determine the temperature of the high energy cut-off.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		JAP	0	SWG	PROBING THE BROAD IRON LINE AND HIGH ENERGY CONTINUUM OF MCG -5-23-16 SIMULTANEOUSLY WITH SUZAKU, XMM-NEWTON AND CHANDRA	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700002010/	Quick Look
490	IRAS 12127-1412	183.8305	-14.4966	183.185484	-14.2187	189.338442	-11.765951	289.94461652	47.46236248	294.8513	56113.7580671296	2012-07-05 18:11:37	56115.2862615741	2012-07-07 06:52:13	707037010	63.6095	60	63.6095	63.6095	0	63.6095	2	2	0	2	1	0	0	57.584	57.584	132.012	2	PROCESSED	57606.6111342593	2016-08-06 14:40:02	56508	2013-08-04 00:00:00	56142.1406018518	2012-08-03 03:22:28	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071441	We propose to observe with the Hard X-ray Detector onboard Suzaku the two Ultraluminous Infrared Galaxies IRAS 00182-7112 and IRAS 12127-1412, both of which are known to harbour very luminous and highly obscured active galactic nuclei (AGN). An AGN reflection component arising from ionized gas is clearly identified at 2 10 keV: the detection of the direct AGN emission above 10 keV and the measure of the reflection efficiency would provide fundamental information on both the physical structure of Compton-thick AGN embedded in a nuclear starburst and their feedback on the surrounding environment.	EXTRAGALACTIC COMPACT SOURCES	7	B	EMANUELE NARDINI		USA	7	AO7	THE PHYSICAL STRUCTURE OF COMPTON-THICK AGN/ULIRGS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707037010/	Quick Look
491	PG 1211+143	183.6045	14.1097	182.967898	14.387617	177.569786	14.352789	267.53559231	74.37841457	120.7913	53698.7348263889	2005-11-24 17:38:09	53701.3397453704	2005-11-27 08:09:14	700009010	96.3241	100	96.59	97.5802	96.3241	96.3241	3	2	3	3	1	0	0	84.0087	84.0087	225.0438	2	PROCESSED	57528.1616203704	2016-05-20 03:52:44	54247	2007-05-27 00:00:00	54038.7422106482	2006-10-30 17:48:47	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001041	A 100ks Suzaku observation of the NLS1, PG 1211+143 is proposed. Previous XMM-Newton and Chandra observation claimed both blue-shifted (0.1c) and redshifted (0.26c-0.40c) iron Kalpha absorption lines. The redshifted iron K lines may originate from matter falling onto the supermassive black hole. The high effective area and low background of Suzaku XIS above 5 keV will enable us to measure these relativistically shifted iron lines in PG 1211+143 with great accuracy. Constraining the time variability of the lines will allow us to determine the physical origins of the absorption, e.g. failed jet/outflow or gravitational redshift from a Kerr black hole. The excellent broadband capabilities of Suzaku will accurately determine the continuum, essential for modeling the iron K band.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		JAP	0	SWG	EXPLORING THE RELATIVISTICALLY SHIFTED IRON LINES IN PG 1211+143	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/700009010/	Quick Look
492	3C345	250.7487	39.7945	250.326948	39.887223	238.332578	61.133151	63.43440525	40.94504508	267.732	56181.2697453704	2012-09-11 06:28:26	56181.4772337963	2012-09-11 11:27:13	707043010	12.7008	10	12.7088	12.7168	0	12.7008	1	1	0	1	1	0	0	10.7314	10.7314	17.9199	0	PROCESSED	57606.986412037	2016-08-06 23:40:26	56582	2013-10-17 00:00:00	56212.7656712963	2012-10-12 18:22:34	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071601	We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	7	AO7	MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707043010/	Quick Look
493	HOLMBERG II X-1	124.8874	70.7162	123.586257	70.872801	106.845907	49.308193	144.27230635	32.72696637	127.9069	56552.1954398148	2013-09-17 04:41:26	56553.2994212963	2013-09-18 07:11:10	708015010	52.19	50	52.19	52.19	0	52.19	2	2	0	2	1	0	0	48.9852	48.9852	95.376	0	PROCESSED	57612.6731481482	2016-08-12 16:09:20	56954	2014-10-24 00:00:00	56588.6670717593	2013-10-23 16:00:35	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081251	Recent X-ray observations have produced evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in an unusual super-Eddington state. Current data are unable to deliver a clear answer, as attempts to model the 0.5-10keV spectra have been plagued by degeneracies resulting from the limited bandpass, owing to the previous lack of focusing hard X-ray telescopes. Combined, Suzaku and NuSTAR will obtain high-quality spectra covering 0.5-30keV, providing powerful probes for understanding the accretion modes and nature of the central BHs. A definitive statement on the existence of either 100-1000Msun black holes or extreme accretion states will be an important legacy of both missions.	EXTRAGALACTIC COMPACT SOURCES	7	A	DOMINIC WALTON		USA	8	AO8	COORDINATED SUZAKU AND NUSTAR OBSERVATIONS OF HOLMBERG II X-1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708015010/	Quick Look
494	MKN 335	1.5763	20.2091	0.933386	19.930785	9.740827	17.860354	108.75916207	-41.41726175	71.5255	56457.9792939815	2013-06-14 23:30:11	56461.868287037	2013-06-18 20:50:20	708016020	154.8168	300	154.8648	154.8168	0	154.8568	2	2	0	2	1	0	0	141.5908	141.5908	335.8944	3	PROCESSED	57611.6590162037	2016-08-11 15:48:59	56383	2013-04-01 00:00:00	56512.7189467593	2013-08-08 17:15:17	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081411	The idea of this proposal is trigger a 300ks observation with Suzaku of the Narrow Line Seyfert 1 Galaxy Mkn 335 during one of its low X-ray flux states. The goal here is to measure its underlying broad-band continuum with Suzaku during a low state and compare it with the 2006 high-state observations. Mkn 335 is one of the best examples of an AGN that went into a deep minimum X-ray flux state. Two competing models can explain these extreme low states: reflection models and partial covering absorber models. Both models still require a variable underlying intrinsic continuum. The science driver is to find out what is causing these low X-ray flux states that have been observed in several NLS1s.	EXTRAGALACTIC COMPACT SOURCES	7	A	DIRK GRUPE		USA	8	AO8-TOO	INTRINSIC LOW-STATE X-RAY LUMINOSITY OF THE NLS1 MKN 335	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708016020/	Quick Look
495	CENTAURUS CLUSTER	192.2012	-41.3132	191.510497	-41.040677	209.072585	-32.853902	302.40029759	21.55583076	106.2442	53731.2579050926	2005-12-27 06:11:23	53732.1808333333	2005-12-28 04:20:24	800014010	36.5192	30	36.5192	36.5464	36.5464	36.5224	2	2	2	2	1	0	0	32.1498	32.1498	79.7399	0	PROCESSED	57532.5349652778	2016-05-24 12:50:21	54247	2007-05-27 00:00:00	54039.373900463	2006-10-31 08:58:25	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001070	A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	0	SWG	OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800014010/	Quick Look
496	NGC5929	231.5229	41.6989	231.07632	41.872918	210.309469	57.436696	67.89643134	55.30533508	120.4869	56651.8033217593	2013-12-25 19:16:47	56652.6042824074	2013-12-26 14:30:10	708022010	24.649	30	24.649	24.6689	0	24.6565	2	2	0	2	1	0	0	25.1767	25.1767	69.1919	0	PROCESSED	57613.6825925926	2016-08-13 16:22:56	56383	2013-04-01 00:00:00	56700.6301388889	2014-02-12 15:07:24	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081418	Using Suzaku's sensitivity in the 2-50keV range, we propose to obtain broad-band spectral fits to the X-ray emission from five Seyfert galaxies which have nuclei that are likely to be Compton-thick. We will thereby derive estimates of their absorbing column densities (hitherto unknown), Fe line widths and equivalent widths, absorption-corrected nuclear X-ray emission and the reprocessed components. With these new estimates we will have complete measurements for a rigorously selected sample of 20 Seyferts that are matched in orientation-independent parameters. The sample selection enables us to account for orientation effects which dominate in them, and investigate the AGN evolution, AGN-star burst connection, and host galaxy evolution.	EXTRAGALACTIC COMPACT SOURCES	7	C	PRAJVAL SHASTRI		USA	8	AO8	COMPTON-THICK SEYFERT NUCLEI AND SEYFERT UNIFICATION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708022010/	Quick Look
497	MRK533	351.9889	8.7759	351.354325	8.500435	356.155514	11.232339	90.62800693	-48.78900326	248.1747	56634.8830671296	2013-12-08 21:11:37	56636.0847569444	2013-12-10 02:02:03	708023010	52.194	50	52.194	52.194	0	52.194	2	2	0	2	1	0	0	48.5617	48.5617	103.8059	0	PROCESSED	57613.5724421296	2016-08-13 13:44:19	56383	2013-04-01 00:00:00	56646.7358449074	2013-12-20 17:39:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081418	Using Suzaku's sensitivity in the 2-50keV range, we propose to obtain broad-band spectral fits to the X-ray emission from five Seyfert galaxies which have nuclei that are likely to be Compton-thick. We will thereby derive estimates of their absorbing column densities (hitherto unknown), Fe line widths and equivalent widths, absorption-corrected nuclear X-ray emission and the reprocessed components. With these new estimates we will have complete measurements for a rigorously selected sample of 20 Seyferts that are matched in orientation-independent parameters. The sample selection enables us to account for orientation effects which dominate in them, and investigate the AGN evolution, AGN-star burst connection, and host galaxy evolution.	EXTRAGALACTIC COMPACT SOURCES	7	C	PRAJVAL SHASTRI		USA	8	AO8	COMPTON-THICK SEYFERT NUCLEI AND SEYFERT UNIFICATION	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708023010/	Quick Look
498	NGC 4552	188.9456	12.612	188.314388	12.887225	183.105993	15.109639	287.9907408	75.02773792	120.0696	54072.312974537	2006-12-03 07:30:41	54072.8405092593	2006-12-03 20:10:20	701037010	20.4398	20	20.4398	20.4398	0	20.4398	1	1	0	1	1	0	0	16.553	16.553	45.5439	0	PROCESSED	57536.226875	2016-05-28 05:26:42	54455	2007-12-21 00:00:00	54088.5410069444	2006-12-19 12:59:03	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011333	The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB.	EXTRAGALACTIC COMPACT SOURCES	7	C	AARON STEFFEN		USA	1	AO1	MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701037010/	Quick Look
499	PDS 456	262.0807	-14.2604	261.370018	-14.220332	262.221238	8.96686	10.39565911	11.16772638	98.239	54155.7486574074	2007-02-24 17:58:04	54160.0355787037	2007-03-01 00:51:14	701056010	190.6002	188	190.6082	190.6002	0	190.6142	2	2	0	2	1	0	0	176.4708	176.4708	370.3428	4	PROCESSED	57537.5850578704	2016-05-29 14:02:29	54757	2008-10-18 00:00:00	54168.6244560185	2007-03-09 14:59:13	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011351	A long 150ks Suzaku observation of the most luminous nearby quasar, PDS 456, is proposed. In the X-ray band, PDS 456 shows a deep iron K absorption trough. One possibility is that the absorption arises from a massive 0.1c outflow, of column density 10^24 cm^-2. Such an outflow would represent a significant fraction of the quasar energy budget. A deep Suzaku observation is proposed to test this outflow model, in particular the high energy bandpass of Suzaku is essential for measuring the profile of the absorption feature and determining the kinematics of the outflow. It is also possible to differentiate between competing models for the iron K feature, most notably between an outflow and a strong reflection component from the innermost radii around a Kerr black hole.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		USA	1	AO1	SOLVING THE ORIGIN OF THE DEEP IRON K ABSORPTION IN PDS 456	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701056010/	Quick Look
500	ABELL 1005	156.925	68.2013	156.004708	68.456472	124.194907	52.556114	140.47803773	43.70739533	119.4313	56609.4953819444	2013-11-13 11:53:21	56610.8334490741	2013-11-14 20:00:10	708042010	61.3496	60	61.3496	61.3496	0	61.3496	2	2	0	2	1	0	0	58.9645	58.9645	115.5998	2	PROCESSED	57613.3284722222	2016-08-13 07:53:00	56994	2014-12-03 00:00:00	56625.7198611111	2013-11-29 17:16:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081533	We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters.	EXTRAGALACTIC COMPACT SOURCES	7	C	LAURENCE DAVID		USA	8	AO8	MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708042010/	Quick Look
501	BL LACERTAE	330.6466	42.3471	330.130697	42.105096	354.282545	49.658149	92.61224541	-10.37092111	71.9797	53882.2303703704	2006-05-27 05:31:44	53883.305775463	2006-05-28 07:20:19	701073010	48.5294	50	48.5454	48.5454	48.5294	48.5374	2	2	2	2	1	0	0	35.5443	35.5443	92.902	1	PROCESSED	57534.4514236111	2016-05-26 10:50:03	54401	2007-10-28 00:00:00	53926.2373032407	2006-07-10 05:41:43	3.0.22.43	5	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011377	We propose two 50 ks Suzaku observations, one for each of gamma-ray bright blazars PKS 1510-089 and BL Lacertae, to be coordinated with optical and radio observations. The goal is to obtain broadband spectra and light-curves. The X-ray fluxes are known to be rapidly variable, but there is no information about the correlation between the spectral shape and flux, which is necessary to establish the origin of previously detected prominent soft X-ray excesses. They are crucial to discriminate between different radiation scenarios responsible for production of hard X-rays and gamma-rays, and to constrain the content and by extension, the acceleration process of the jet. These observations will be ingredients of a "pilot" campaigns for the future joint Suzaku-GLAST investigations.	EXTRAGALACTIC COMPACT SOURCES	7	A	GRZEGORZ MADEJSKI		USA	1	AO1	SUZAKU OBSERVATIONS OF GAMMA-RAY BRIGHT BLAZARS BL LACERTAE AND PKS 1510-089	HXD	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701073010/	Quick Look
502	BEYOND VIRGO 4	187.7154	16.9006	187.085728	17.176651	180.130581	18.529302	276.92044319	78.71921322	118.472	55915.331099537	2011-12-20 07:56:47	55916.0466666667	2011-12-21 01:07:12	806063010	30.1361	30	30.1361	30.1361	0	30.1361	2	2	0	2	1	0	0	22.7334	22.7334	61.818	0	PROCESSED	57604.1732407407	2016-08-04 04:09:28	56299	2013-01-07 00:00:00	55932.1295949074	2012-01-06 03:06:37	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061523	To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	NORBERT WERNER		USA	6	AO6	LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806063010/	Quick Look
503	LMC X-4	83.221	-66.3591	83.212611	-66.392014	1.088478	-87.292124	276.32094979	-32.52452295	284.2438	54561.5523842593	2008-04-05 13:15:26	54562.3058333333	2008-04-06 07:20:24	702036020	25.3397	20	25.3425	25.3425	0	25.3397	2	2	0	2	1	0	0	24.502	24.502	65.07	0	PROCESSED	57542.2490046296	2016-06-03 05:58:34	54943	2009-04-22 00:00:00	54574.4237152778	2008-04-18 10:10:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021127	We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects.	EXTRAGALACTIC COMPACT SOURCES	7	A	RYAN HICKOX		USA	2	AO2	SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702036020/	Quick Look
504	NGC5548	214.4955	25.1272	213.928592	25.357387	201.997114	36.406484	31.93108614	70.4962838	289.7815	54303.4447337963	2007-07-22 10:40:25	54304.2711111111	2007-07-23 06:30:24	702042060	28.9178	30	28.9258	28.9258	0	28.9178	1	1	0	1	1	0	0	24.8181	24.8181	71.3839	1	PROCESSED	57539.29125	2016-05-31 06:59:24	54706	2008-08-28 00:00:00	54339.5363310185	2007-08-27 12:52:19	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021307	We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	2	AO2	NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702042060/	Quick Look
505	NGC 4507	188.8987	-39.9119	188.223538	-39.636542	205.656728	-32.779926	299.63576127	22.85843053	109.5879	54454.5145717593	2007-12-20 12:20:59	54456.5835532407	2007-12-22 14:00:19	702048010	103.626	80	103.634	103.626	0	103.634	2	2	0	2	1	0	0	110.9021	110.9021	178.7279	0	PROCESSED	57540.963900463	2016-06-01 23:08:01	54829	2008-12-29 00:00:00	54462.288287037	2007-12-28 06:55:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021331	Recent X-ray observations of Seyfert 2 galaxies have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by AGN Unified Schemes. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (60 ksec each) of four local bright Compton-thin Seyfert2s, selected from the Swift/BAT survey with a hard X-ray flux exceeding 1e-10 cgs to form a flux-limited sample. The unprecedented broad bandpass of Suzaku offers a unique tool to investigate the X-ray emission, placing strong constraints on the geometry and location of the reprocessing matter.	EXTRAGALACTIC COMPACT SOURCES	7	B	JAMES REEVES		USA	2	AO2	REVEALING THE REPROCESSING MATTER IN SEYFERT 2 GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702048010/	Quick Look
506	RCS215222-0503.9	328.0881	-5.0633	327.433899	-5.298799	328.489701	7.382957	52.1030598	-42.03624594	70.7002	55696.1248842593	2011-05-15 02:59:50	55696.8398263889	2011-05-15 20:09:21	806081010	30.6482	30	30.6482	30.6482	0	30.6482	1	1	0	1	1	0	0	25.3728	25.3728	61.744	0	PROCESSED	57602.0507986111	2016-08-02 01:13:09	56072	2012-05-25 00:00:00	55705.2063310185	2011-05-24 04:57:07	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061533	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AMALIA HICKS		USA	6	AO6	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806081010/	Quick Look
507	HOLMBERG IX X-1	149.4756	69.0751	148.45738	69.31359	119.76782	51.701026	141.91985765	41.06519535	104.8942	56976.7425347222	2014-11-15 17:49:15	56977.5230787037	2014-11-16 12:33:14	709015020	34.1281	30	34.1281	34.1281	0	34.1281	1	1	0	1	0	0	0	0	0	0	0	PROCESSED	57616.7878240741	2016-08-16 18:54:28	57359	2015-12-03 00:00:00	56993.4304513889	2014-12-02 10:19:51	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091251	Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs.	EXTRAGALACTIC COMPACT SOURCES	7	A	DOMINIC WALTON		USA	9	AO9	MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015020/	Quick Look
508	I ZW 18	143.5064	55.23	142.623877	55.452479	125.705805	38.222173	160.54065348	44.84408453	279.2158	56792.4911111111	2014-05-15 11:47:12	56792.8568402778	2014-05-15 20:33:51	709021010	17.2612	100	17.2612	17.2612	0	17.2612	1	1	0	1	1	0	0	16.549	16.549	31.1279	0	PROCESSED	57615.102650463	2016-08-15 02:27:49	57358	2015-12-02 00:00:00	56818.6775347222	2014-06-10 16:15:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091441	The source of energetic photons that reionized and heated the early universe remains uncertain. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectrum with the Suzaku XIS. These observations are important to our understanding of the heating of the universe during the epoch of reionization.	EXTRAGALACTIC COMPACT SOURCES	7	A	PHILIP KAARET		USA	9	AO9	X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709021010/	Quick Look
509	XBONGBLUE1	217.1061	32.8569	216.573655	33.079659	200.393656	44.372245	54.10325006	68.28811801	132.8525	54453.8528587963	2007-12-19 20:28:07	54454.166875	2007-12-20 04:00:18	702082010	15.1725	13	15.1725	15.1725	0	15.1725	2	2	0	2	1	0	0	15.6996	15.6996	27.1259	0	PROCESSED	57540.9008217593	2016-06-01 21:37:11	54828	2008-12-28 00:00:00	54461.0450231482	2007-12-27 01:04:50	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021376	We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs.	EXTRAGALACTIC COMPACT SOURCES	7	C	CHRISTINE JONES		USA	2	AO2	OBSCURED AGN AND XBONGS IN BOOTES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702082010/	Quick Look
510	A1060	159.1744	-27.531	158.58579	-27.271265	172.752913	-33.32931	269.60056717	26.48279097	103.6438	53696.6258796296	2005-11-22 15:01:16	53697.7211111111	2005-11-23 17:18:24	800003010	39.139	40	39.139	39.147	39.155	39.155	2	2	2	2	1	0	0	34.6024	34.6024	94.6259	1	PROCESSED	57528.0675462963	2016-05-20 01:37:16	54247	2007-05-27 00:00:00	54037.8583449074	2006-10-29 20:36:01	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001021	A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYA OHASHI		JAP	0	SWG	OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800003010/	Quick Look
511	NGC720	28.2529	-13.7362	27.644452	-13.982164	20.9363	-23.62893	173.01572713	-70.35499124	242.5294	53734.3673611111	2005-12-30 08:49:00	53739.5627546296	2006-01-04 13:30:22	800009010	177.1929	100	177.1929	177.1929	177.1929	177.1929	2	2	2	2	1	0	0	9.6621	9.6621	47.5408	0	PROCESSED	57532.602962963	2016-05-24 14:28:16	54247	2007-05-27 00:00:00	54039.6651736111	2006-10-31 15:57:51	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001031	We propose to observe an isolated elliptical galaxy NGC720 with Suzaku. Isolated elliptical galaxies are important to probe the ISM metal abundance, since their hot gas is not affected by the amibient bright intracluster medium which often exists around X-ray bright elliptical galaxies. Suzaku is expected to measure the Oxygen abundance in the ISM bettern than XMM-Newton and constrain the origin of metals in the ISM and also ICM. Dark matter content around elliptical galaxies can also be constrained better than XMM-Newton. Such a measurement is difficult for X-ray bright galaxies due to the superposition of the cluster potential.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	0	SWG	OXYGEN ABUNDANCE AND DARK MATTER CONTENT AROUDN AN ISOLATED ELLIPTICAL GALAXY NGC720	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800009010/	Quick Look
512	NGC3227	155.8772	19.8684	155.194638	20.121777	150.38806	9.142968	216.98573476	55.44624837	110.6974	54797.8953703704	2008-11-27 21:29:20	54799.750162037	2008-11-29 18:00:14	703022050	79.4298	50	79.4298	79.4339	0	79.4378	2	2	0	2	1	0	0	39.8439	39.8439	160.2418	1	PROCESSED	57544.6203819444	2016-06-05 14:53:21	54557	2008-04-01 00:00:00	54809.8059490741	2008-12-09 19:20:34	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031013	We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge.	EXTRAGALACTIC COMPACT SOURCES	7	A	MARTIN ELVIS		USA	3	AO3	NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703022050/	Quick Look
513	MKN 279	208.2253	69.3021	207.933654	69.547649	144.919228	67.626916	115.05735618	46.87522986	345.4595	54965.2632407407	2009-05-14 06:19:04	54968.6668287037	2009-05-17 16:00:14	704031010	160.3514	150	160.3594	160.3514	0	160.3594	2	2	0	2	1	0	0	150.386	150.386	293.9979	3	PROCESSED	57546.636099537	2016-06-07 15:15:59	55345	2010-05-29 00:00:00	54978.3987152778	2009-05-27 09:34:09	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041403	We aim to test if the high-luminosity Seyfert 1.5 Mkn 279 contains an ionized inner accretion disk by using Suzaku to spectroscopically separate the ionized and neutral reflectors. This source is relatively unobscured, allowing clear modeling of the shape of the strong soft excess; we will also test for a Fe K diskline component, which may be missing if the disk is ionized or truncated. Only a broadband X-ray spectrum, including simultaneous > 10 keV coverage to constrain Compton reflection, will allow us to thoroughly test blurred, ionized disk reflection models and constrain the nature of the reflector(s).	EXTRAGALACTIC COMPACT SOURCES	7	A	ALEX MARKOWITZ		USA	4	AO4	DOES THE LOW-OBSCURATION, LOW-REFLECTION, HIGH-LUMINOSITY SEYFERT MKN279 CONTAIN AN IONIZED OR TRUNCATED ACCRETION DISK?	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704031010/	Quick Look
514	NGC1194	45.9522	-1.1044	45.31576	-1.299082	43.150403	-17.672733	179.17914291	-48.96176874	76.9913	55044.6911689815	2009-08-01 16:35:17	55045.8141087963	2009-08-02 19:32:19	704046010	50.3161	50	50.3161	50.5961	0	50.5961	2	2	0	2	1	0	0	48.4268	48.4268	97.0038	1	PROCESSED	57548.0499074074	2016-06-09 01:11:52	55427	2010-08-19 00:00:00	55061.5275115741	2009-08-18 12:39:37	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041414	We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc.	EXTRAGALACTIC COMPACT SOURCES	7	B	EZEQUIEL TREISTER		USA	4	AO4	THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704046010/	Quick Look
515	NGC 4472	187.4441	8.005	186.80838	8.281234	183.627851	10.299036	286.9163593	70.20028227	117.8054	54072.8427893518	2006-12-03 20:13:37	54075.7014699074	2006-12-06 16:50:07	801064010	121.0358	120	121.0358	121.0358	0	121.0358	2	2	0	2	1	0	0	103.4464	103.4464	246.9548	6	PROCESSED	57536.3089467593	2016-05-28 07:24:53	54702	2008-08-24 00:00:00	54089.1857523148	2006-12-20 04:27:29	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011403	We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MICHAEL LOEWENSTEIN		USA	1	AO1	INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801064010/	Quick Look
516	NGC 4649	190.9148	11.557	190.284732	11.830628	185.371113	14.926523	295.86493189	74.32191724	113.3108	54098.4203703704	2006-12-29 10:05:20	54104.1473263889	2007-01-04 03:32:09	801065010	224.0304	120	224.0304	224.0304	0	224.0304	2	2	0	2	1	0	0	26.3042	26.3042	69.2898	1	PROCESSED	57536.4300578704	2016-05-28 10:19:17	54743	2008-10-04 00:00:00	54132.9809027778	2007-02-01 23:32:30	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011403	We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MICHAEL LOEWENSTEIN		USA	1	AO1	INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801065010/	Quick Look
517	UGC03957	115.2433	55.429	114.235063	55.545488	106.863653	33.455815	162.22286538	28.93195726	271.243	53841.9927314815	2006-04-16 23:49:32	53842.2828587963	2006-04-17 06:47:19	801072010	10.7714	12	10.7794	10.7794	10.7874	10.7714	1	1	1	1	1	0	0	9.642	9.642	25.0079	0	PROCESSED	57533.4729166667	2016-05-25 11:21:00	54401	2007-10-28 00:00:00	53906.7753240741	2006-06-20 18:36:28	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801072010/	Quick Look
518	IC 2497	145.222	34.6799	144.47003	34.907483	135.80747	19.598067	190.267728	48.8163504	306.2341	54939.6906365741	2009-04-18 16:34:31	54941.5550810185	2009-04-20 13:19:19	704053010	76.4837	75	76.4837	76.4837	0	76.4837	2	2	0	2	1	0	0	63.948	63.948	161.0478	2	PROCESSED	57546.2140046296	2016-06-07 05:08:10	55318	2010-05-02 00:00:00	54952.1320717593	2009-05-01 03:10:11	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041432	The discovery of `Hanny's Voorwerp' near IC 2497 opens an unprecedented window into the time evolution of a single AGN on timescales up to 100,000 years. Based on its properties, the Voorwerp was illuminated by a luminous AGN ~100,000 years ago, but the AGN host galaxy - IC 2497 - does not seem to host a sufficiently luminous AGN. Thus, IC 2497 either hosts a highly obscured AGN only detectable in hard X-rays, or it has dropped in luminosity by a factor of 10-1000. We propose to observe IC 2497 with Suzaku for 75 ksec to determine the hard X-ray luminosity and spectrum to measure the amount of obscuration and the current intrinsic luminosity of its AGN. Only with hard X-ray observations can we break the degeneracy between obscuration and decrease in luminosity.	EXTRAGALACTIC COMPACT SOURCES	7	A	KEVIN SCHAWINSKI		USA	4	AO4	HOW FAST CAN AN AGN SHUT DOWN? - SUZAKU OBSERVATION OF IC 2497 AND `HANNY'S VOORWERP'	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704053010/	Quick Look
519	A272	28.7603	33.9026	28.031098	33.657734	38.955118	20.665911	137.73606223	-27.1341127	64.9465	53943.0449537037	2006-07-27 01:04:44	53943.6842476852	2006-07-27 16:25:19	801084010	22.2455	21	22.2535	22.2535	22.2455	22.2535	2	2	2	2	1	0	0	24.6035	24.6035	55.2319	0	PROCESSED	57535.0602430556	2016-05-27 01:26:45	54401	2007-10-28 00:00:00	53955.6516782407	2006-08-08 15:38:25	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801084010/	Quick Look
520	A566	106.0915	63.2647	104.91759	63.339113	99.420321	40.34898	152.76309519	25.45548296	285.637	54178.3128587963	2007-03-19 07:30:31	54178.8029976852	2007-03-19 19:16:19	801085010	22.2711	20	22.2711	22.2711	0	22.2711	2	2	0	2	1	0	0	22.1523	22.1523	42.3399	0	PROCESSED	57537.7151157407	2016-05-29 17:09:46	54695	2008-08-17 00:00:00	54185.9799305556	2007-03-26 23:31:06	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011422	We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	CALEB SCHARF		USA	1	AO1	A ZERO-REDSHIFT GALAXY CLUSTER BASELINE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801085010/	Quick Look
521	RXJ 0658	104.704	-55.933	104.461428	-55.862903	130.333928	-77.302143	266.02429497	-21.20357002	164.9362	54095.6181597222	2006-12-26 14:50:09	54098.4099421296	2006-12-29 09:50:19	801089010	101.3845	100	101.3845	101.3845	0	101.3845	2	2	0	2	1	0	0	84.3679	84.3679	241.1547	2	PROCESSED	57637.5971180556	2016-09-06 14:19:51	54702	2008-08-24 00:00:00	54111.5842013889	2007-01-11 14:01:15	3.0.22.44	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	011448	We propose SUZAKU X-ray observations of an intriguing cluster of galaxies, RXJ0658, to determine and characterize the nature of the hard X-ray spectral emission and other nonthermal activity. It also has many other interesting features, such as a cold front, evidence for merger, a shock, and regions of unusually high temperature, all of which are related to the hard X-ray emission and the nonthermal activity. The more accurate measure of the spectral characteristics of the hard component, when combined with the radio and other past X-ray data, can reveal the nature of the emission process and the acceleration mechanism of the relativistic electrons, provide a means of measuring the magnetic field strength, and aid in understanding the process of formation of clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	VAHE PETROSIAN		USA	1	AO1	HARD X-RAY EMISSION FROM CLUSTER RXJ0658	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801089010/	Quick Look
522	CEN A S LOBE NO. 1	200.8664	-45.1602	200.128121	-44.89936	217.870253	-33.408756	308.83796576	17.34395301	288.0039	55418.6612962963	2010-08-10 15:52:16	55419.7758101852	2010-08-11 18:37:10	705032010	75.1654	80	75.1654	75.1654	0	75.1654	2	2	0	2	1	0	0	64.2728	64.2728	96.2818	0	PROCESSED	57552.9742476852	2016-06-13 23:22:55	55803	2011-08-30 00:00:00	55428.1537152778	2010-08-20 03:41:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051401	We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays).	EXTRAGALACTIC COMPACT SOURCES	7	B	GRZEGORZ MADEJSKI		USA	5	AO5	SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705032010/	Quick Look
523	SEGUE 1	151.7658	16.0862	151.086487	16.330668	148.083031	4.208593	220.47149585	50.42674703	110.8027	56248.0740625	2012-11-17 01:46:39	56250.3182291667	2012-11-19 07:38:15	807046010	85.4391	85	85.4622	85.4431	0	85.4391	2	2	0	2	1	0	0	77.5645	77.5645	193.8419	4	PROCESSED	57608.0603240741	2016-08-08 01:26:52	56641	2013-12-15 00:00:00	56275.5584490741	2012-12-14 13:24:10	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071502	Our ongoing dedicated X-ray search for dark matter targeting dwarf spheroidal galaxies set new constraints on the mass and mixing angle of the sterile neutrino -- a plausible dark matter candidate that emits an X-ray via radiative decay. We have proposed a new well-motivated candidate -- moduli dark matter, that also produces a detectable X-ray line. We propose Suzaku observations of the Segue 1 dwarf spheroidal -- the most dark matter dominated galaxy known. Its extreme nature implies that it provides the tightest constraints on sterile neutrino and moduli parameters in the event of a detection, and best limits in the absence of one. The resulting spectrum is optimal for exploring new physics, such as string theory compactification or supersymmetry breaking, and as a legacy for Astro-H.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	MICHAEL LOEWENSTEIN		USA	7	AO7	SEARCH FOR DARK MATTER WITH SUZAKU OBSERVATIONS OF THE MOST DARK MATTER DOMINATED GALAXY IN THE UNIVERSE	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807046010/	Quick Look
524	CEN A S LOBE NO. 3	205.7514	-45.1409	204.991343	-44.889287	221.546575	-31.897052	312.39292182	16.78143613	279.0007	55420.9668981482	2010-08-12 23:12:20	55421.3452777778	2010-08-13 08:17:12	705034010	20.0575	20	20.0815	20.0735	0	20.0575	3	2	0	2	1	0	0	18.9436	18.9436	32.6879	1	PROCESSED	57552.9389467593	2016-06-13 22:32:05	55803	2011-08-30 00:00:00	55435.169537037	2010-08-27 04:04:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051401	We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays).	EXTRAGALACTIC COMPACT SOURCES	7	B	GRZEGORZ MADEJSKI		USA	5	AO5	SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705034010/	Quick Look
525	DRACO	260.0265	57.929	259.823545	57.97767	237.171171	80.222303	86.38548758	34.73420948	52.1224	54196.7611458333	2007-04-06 18:16:03	54198.2216898148	2007-04-08 05:19:14	802051010	63.3232	67	63.3232	63.3232	0	63.3232	2	2	0	2	1	0	0	64.9572	64.9572	126.1818	2	PROCESSED	57538.1232291667	2016-05-30 02:57:27	54829	2008-12-29 00:00:00	54203.3603703704	2007-04-13 08:38:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021405	We propose 50 ksec Suzaku observations of the Ursa Minor and Draco dwarf spheroidal galaxies. These dense, dark-matter-dominated systems are carefully selected as the strongest potential sources of line emission from radiatively decaying keV dark matter of any astrophysical object. The low-level, stable Suzaku background makes it the most sensitive instrument to-date for this purpose. At the very least, constraints that enter a significant new regime are derived: non-detections are still of great importance. In the best case, the long sought-after identity of dark matter will be discovered, pointing the way to physics beyond the Standard Model.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MICHAEL LOEWENSTEIN		USA	2	AO2	SEARCH FOR WARM DARK MATTER WITH SUZAKU OBSERVATIONS OF DWARF SPHEROIDAL GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802051010/	Quick Look
526	SDSS J0854+3524	133.7386	35.4192	132.953536	35.610263	126.168595	17.306871	188.0033984	39.53150085	111.2842	56214.3546527778	2012-10-14 08:30:42	56214.8244560185	2012-10-14 19:47:13	807063010	20.6148	20	20.6148	20.6148	0	20.6148	1	1	0	1	1	0	0	18.084	18.084	40.56	0	PROCESSED	57607.7601157407	2016-08-07 18:14:34	56598	2013-11-02 00:00:00	56232.4365856482	2012-11-01 10:28:41	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071512	Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ERIC MILLER		USA	7	AO7	FINDING FOSSIL GROUPS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807063010/	Quick Look
527	BOOTES GROUP 30	219.4427	33.5107	218.918921	33.726455	202.46828	45.823682	55.01212205	66.25629851	308.903	54276.6949189815	2007-06-25 16:40:41	54277.5271875	2007-06-26 12:39:09	802056010	38.5045	38	38.5045	38.5045	0	38.5045	2	2	0	2	1	0	0	35.7473	35.7473	71.8979	1	PROCESSED	57539.0466782407	2016-05-31 01:07:13	54702	2008-08-24 00:00:00	54333.4389583333	2007-08-21 10:32:06	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021424	We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	MARSHALL BAUTZ		USA	2	AO2	SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802056010/	Quick Look
528	SMC X-1	19.2337	-73.4445	18.901627	-73.707724	312.330059	-66.462167	300.42986971	-43.55966827	9.1005	55673.6490625	2011-04-22 15:34:39	55674.1112037037	2011-04-23 02:40:08	706030030	15.6526	18	15.6526	15.6526	0	15.871	2	2	0	1	1	0	0	21.2614	21.2614	39.9199	1	PROCESSED	57601.5606597222	2016-08-01 13:27:21	56067	2012-05-20 00:00:00	55692.2968634259	2011-05-11 07:07:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061236	We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk.	EXTRAGALACTIC COMPACT SOURCES	7	A	JOSEPH NEILSEN		USA	6	AO6	THE WANDERING WARP OF SMC X-1	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706030030/	Quick Look
529	RXJ1159+5531	179.9637	55.4123	179.320531	55.690619	149.995673	49.037125	137.70641489	60.21165624	302.8269	56074.0600694445	2012-05-27 01:26:30	56075.6800578704	2012-05-28 16:19:17	807064010	82.2339	100	82.2419	82.2419	0	82.2339	2	2	0	2	1	0	0	98.6011	98.6011	139.964	1	PROCESSED	57605.5596875	2016-08-05 13:25:57	56657	2013-12-31 00:00:00	56086.0194328704	2012-06-08 00:27:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071513	With Chandra and Suzaku we recently constrained the hot gas and dark matter out to the virial radius (rvir=R108) in the fossil group/cluster RXJ1159+5531. Unlike some recent observations of cluster outskirts, the gas fraction is consistent with the cosmic value, and the entropy profile at rvir is consistent with gravity-only structure formation simulations. As a fossil group, RXJ1159+5531 may be unusually relaxed at large scales. If so, the gas properties should not vary much azimuthally. We propose a complementary Suzaku observation to explore this by measuring the gas in a different azimuthal region, more than doubling the current (~27%) azimuthal coverage. Our results will help determine if gas clumping, invoked to explain the outskirts of some clusters, is ubiquitous.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	PHILIP HUMPHREY		USA	7	AO7	RELAXED GAS AT THE VIRIAL RADIUS IN A FOSSIL GROUP	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807064010/	Quick Look
530	PKS 0745-191	116.7966	-19.5079	116.243978	-19.383587	123.623714	-39.870751	236.58636127	2.85363493	294.0004	54234.0374884259	2007-05-14 00:53:59	54234.8446643518	2007-05-14 20:16:19	802062050	33.4146	30	33.4146	33.4226	0	33.4226	2	2	0	2	1	0	0	31.3065	31.3065	69.7239	1	PROCESSED	57538.6567708333	2016-05-30 15:45:45	54695	2008-08-17 00:00:00	54245.5456712963	2007-05-25 13:05:46	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021440	PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ANDREW YOUNG		USA	2	AO2	PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062050/	Quick Look
531	MRK 841	226.0091	10.4587	225.405512	10.653095	220.178836	26.612533	11.24319757	54.63999984	112.9994	55931.8646180556	2012-01-05 20:45:03	55937.1896990741	2012-01-11 04:33:10	706029010	244.3518	350	244.3518	244.3518	0	244.3598	2	2	0	2	1	0	0	229.726	229.726	419.686	4	PROCESSED	57604.4310648148	2016-08-04 10:20:44	55652	2011-04-01 00:00:00	55946.5082407407	2012-01-20 12:11:52	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061119	We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade.	EXTRAGALACTIC COMPACT SOURCES	7	A	CHRISTOPHER REYNOLDS		USA	6	AO6-LP	A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706029010/	Quick Look
532	ABELL 665	127.3329	65.7462	126.195484	65.912794	110.615683	44.954956	149.92967896	34.55444535	289.9972	56027.8062847222	2012-04-10 19:21:03	56028.5592476852	2012-04-11 13:25:19	807072030	50.3486	50	50.3526	50.3486	0	50.3561	2	2	0	2	1	0	0	47.3856	47.3856	65.049	0	PROCESSED	57605.1517939815	2016-08-05 03:38:35	56018	2012-04-01 00:00:00	56044.1669791667	2012-04-27 04:00:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072030/	Quick Look
533	NGC 3079	150.444	55.6163	149.59923	55.857396	130.078493	40.265138	157.91350273	48.36319014	294.1052	54590.7432407407	2008-05-04 17:50:16	54591.1147800926	2008-05-05 02:45:17	803039010	14.4083	100	14.4083	14.4083	0	14.4083	2	2	0	2	1	0	0	12.9538	12.9538	32.0799	0	PROCESSED	57542.4484027778	2016-06-03 10:45:42	54999	2009-06-17 00:00:00	54602.2023958333	2008-05-16 04:51:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031303	We will determine whether AGN can drive galactic-scale winds by observing NGC 3079, the best nearby candidate for such a wind. The edge-on spiral NGC 3079 hosts a Compton-thick AGN and is surrounded by a 40 kpc-scale soft X-ray nebula, the largest manifestation of outflow activity also seen in the optical and radio. Proving the outflow is AGN-driven requires Suzaku's unique abilities. We will measure the AGN luminosity using the HXD in the 15-40 keV range and the 2-10 keV band reflection spectrum to assess whether the AGN can radiatively-or-mechanically power the observed superwind. We will determine the origin of the soft X-ray nebula using the relative elemental abundances in the plasma. We can also detect any significant starburst through the 6.7 keV line emission it would create.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	DAVID STRICKLAND		USA	3	AO3	NGC 3079'S 40 KPC-SCALE OUTFLOW: AGN OR STARBURST-DRIVEN?	HXD	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803039010/	Quick Look
534	CYGNUS A CLUSTER	299.7609	40.7885	299.328588	40.65123	317.589132	59.411403	76.19456446	5.8531495	241.849	54785.9049537037	2008-11-15 21:43:08	54786.9154976852	2008-11-16 21:58:19	803050010	44.6587	45	44.6587	44.6587	0	44.6587	1	1	0	1	1	0	0	42.966	42.966	87.28	0	PROCESSED	57544.3868055556	2016-06-05 09:17:00	55167	2009-12-02 00:00:00	54796.9718981482	2008-11-26 23:19:32	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031426	The radio galaxy Cygnus A lies in a cooling core cluster which is currently undergoing a cluster merger with a particularly simple geometry. We propose XIS spectra of the radio source/cooling core interaction region, merger shock region, and second subcluster. The Fe K emission line will be used to measure gas velocities in these 3 regions to determine the dynamics of the merger, and to constrain hydro/N-body simulations of the merger. Collisionless merger shocks may produce detectable non-equilibrium effects. We will also determine an upper limit for the rate of expansion of the X-ray bubble around the radio source, studying the interaction of the radio galaxy and X-ray gas in the only FR-II radio galaxy in a nearby cluster. HXD data will constrain inverse Compton from the radio source.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	DANIEL WIK		USA	3	AO3	PROPERTIES OF THE MERGER AND RADIO SOURCE INTERACTION IN THE CYGNUS A CLUSTER	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803050010/	Quick Look
535	ABELL 2597	351.1561	-12.0446	350.50582	-12.319475	347.114403	-7.564991	65.23010074	-64.66820365	250.0003	56262.3308680556	2012-12-01 07:56:27	56263.5369212963	2012-12-02 12:53:10	807073020	50.0345	50	50.0585	50.0425	0	50.0345	1	1	0	1	1	0	0	44.785	44.785	104.1919	0	PROCESSED	57608.1666319444	2016-08-08 03:59:57	56018	2012-04-01 00:00:00	56336.4705902778	2013-02-13 11:17:39	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073020/	Quick Look
536	NGC 2110	88.0457	-7.4586	87.441571	-7.469572	87.744639	-30.884812	212.92775975	-16.54787795	79.201	56170.1053009259	2012-08-31 02:31:38	56172.5412268518	2012-09-02 12:59:22	707034010	103.2595	100	103.2595	103.2595	0	103.2595	2	2	0	2	1	0	0	102.8063	102.8063	210.4361	1	PROCESSED	57607.0102199074	2016-08-07 00:14:43	56667	2014-01-10 00:00:00	56301.6411458333	2013-01-09 15:23:15	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071426	We request two 100 ks	EXTRAGALACTIC COMPACT SOURCES	7	B	ELIZABETH RIVERS		USA	7	AO7	TRACKING THE PARTIAL COVERING ABSORBERS IN NGC 2110: CONSTRAINTS FOR CLUMPY ABSORBER MODELS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707034010/	Quick Look
537	NGC 4125	182.0568	65.1777	181.434624	65.455888	140.391429	57.000336	130.16762444	51.33919783	175.9017	55103.512037037	2009-09-29 12:17:20	55105.4578009259	2009-10-01 10:59:14	804047010	104.0801	100	104.0801	104.0881	0	104.0961	2	2	0	2	1	0	0	93.7257	93.7257	168.0857	0	PROCESSED	57548.726712963	2016-06-09 17:26:28	55491	2010-10-22 00:00:00	55125.5744212963	2009-10-21 13:47:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041502	Recent observations of relaxed galaxy groups have revealed ubiquitous abundance gradients, indicating large-scale mixing of the gas, possibly driven by AGN feedback. Exploiting the low background and good sensitivity of Suzaku, we have found similar gradients in two lower mass, galaxy-scale systems, which has important implications for models of feedback and chemical enrichment. We propose to observe two more isolated elliptical galaxies, thus starting to building a sample for determining the frequency and properties of such abundance gradients in early-type galaxies.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	PHILIP HUMPHREY		USA	4	AO4	ABUNDANCE GRADIENTS IN EARLY-TYPE GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804047010/	Quick Look
538	NGC6482	267.957	23.086	267.434837	23.097176	267.256842	46.506557	48.10607859	22.91404378	109.6205	55238.2645949074	2010-02-11 06:21:01	55239.2919444444	2010-02-12 07:00:24	804050010	46.5467	45	46.5467	46.5467	0	46.5467	2	2	0	2	1	0	0	28.5166	28.5166	88.7438	0	PROCESSED	57550.5834143518	2016-06-11 14:00:07	55622	2011-03-02 00:00:00	55251.3186458333	2010-02-24 07:38:51	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041513	Fossil groups present a puzzle to current theories of structure formation. Despite the low number of bright galaxies, their high velocity dispersions and gas temperatures indicate potential wells deeper than that of normal groups. Their measured c200 are high indicating very early formation epochs, which is in contradiction with the lack of cooling cores observed. We can constrain their ages by looking at the distribution of the SN Ia and II ejecta near their core. If they are formed more recently than normal groups by galaxy merging near the core, the central gas should have a reduction of SN Ia dominance, differently from what is observed in normal groups. We propose to test this with the most optimal and nearest fossil group, NGC6482, matching very well the capabilities of Suzaku.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	RENATO DUPKE		USA	4	AO4	DISCRIMINATING COMPETING MODELS FOR THE ORIGIN OF FOSSIL GROUPS OF GALAXIES WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804050010/	Quick Look
539	NGC741MOSAICE_P4	29.8808	5.7741	29.226568	5.531917	29.834623	-6.020542	152.02832852	-53.20754513	71.8261	55054.5770138889	2009-08-11 13:50:54	55054.8084953704	2009-08-11 19:24:14	804052040	11.0257	10	11.0257	11.3217	0	11.3057	3	2	0	2	1	0	0	11.3902	11.3902	19.9959	0	PROCESSED	57548.1244328704	2016-06-09 02:59:11	55448	2010-09-09 00:00:00	55081.2593055556	2009-09-07 06:13:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052040/	Quick Look
540	1730-130	263.2641	-13.0933	262.559168	-13.058946	263.324851	10.191548	12.02258907	10.80244107	271.1606	55829.6599537037	2011-09-25 15:50:20	55830.0946643518	2011-09-26 02:16:19	706046010	11.0858	10	11.0938	11.0938	0	11.0858	1	1	0	1	1	0	0	9.8811	9.8811	37.5359	1	PROCESSED	57603.2457407407	2016-08-03 05:53:52	56225	2012-10-25 00:00:00	55875.6203703704	2011-11-10 14:53:20	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061601	We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	6	AO6	EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706046010/	Quick Look
541	ABELL 426 E2	50.6767	41.5228	49.847142	41.344864	59.17553	22.199581	151.03351832	-12.94989772	90.0008	55041.7150115741	2009-07-29 17:09:37	55041.9654976852	2009-07-29 23:10:19	804057010	12.9048	10	12.9048	12.9048	0	12.9048	2	2	0	2	1	0	0	12.962	12.962	21.6399	1	PROCESSED	57547.969849537	2016-06-08 23:16:35	55419	2010-08-11 00:00:00	55050.2440277778	2009-08-07 05:51:24	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804057010/	Quick Look
542	ABELL 426 N6	48.8242	42.9264	47.990569	42.741631	58.170143	23.930613	149.06870737	-12.52705179	59.999	55063.8243055556	2009-08-20 19:47:00	55064.6334837963	2009-08-21 15:12:13	804068010	36.5265	30	36.5345	36.5265	0	36.5425	2	2	0	2	1	0	0	30.8843	30.8843	69.9119	0	PROCESSED	57548.3037731482	2016-06-09 07:17:26	55441	2010-09-02 00:00:00	55075.1362037037	2009-09-01 03:16:08	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804068010/	Quick Look
543	ESO 511-G030	214.8452	-26.646	214.125789	-26.416487	221.403618	-12.022581	326.22952078	32.2164843	286.9689	56130.0282407407	2012-07-22 00:40:40	56136.3340856482	2012-07-28 08:01:05	707023020	224.0255	270	224.0255	224.0255	0	224.0335	2	2	0	2	1	0	0	195.6334	195.6334	410.8958	3	PROCESSED	57606.8434606482	2016-08-06 20:14:35	56646	2013-12-20 00:00:00	56279.0046064815	2012-12-18 00:06:38	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071413	The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined.	EXTRAGALACTIC COMPACT SOURCES	7	A	JAMES REEVES		USA	7	AO7	MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707023020/	Quick Look
544	SNR 1987A	83.833	-69.2775	83.924877	-69.307216	307.543742	-86.433259	279.71430694	-31.94790633	135.9732	56233.5143981482	2012-11-02 12:20:44	56234.854375	2012-11-03 20:30:18	707020010	81.2764	80	81.2764	81.2844	0	81.2924	2	2	0	2	1	0	0	78.5842	78.5842	115.7599	0	PROCESSED	57607.9555439815	2016-08-07 22:55:59	56611	2013-11-15 00:00:00	56245.4956365741	2012-11-14 11:53:43	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071331	Despite extensive observations of supernova remnant (SNR) 1987A with Chandra and XMM-Newton, the origin of the hard band (3-10 keV) X-ray emission is elusive (thermal vs nonthermal). A straightforward way to discriminate the thermal and nonthermal origins of the hard X-rays is to detect Fe K lines. The Suzaku XIS provides a uniquely efficient opportunity for a sensitive search for the Fe K lines, which is an excellent complement to the existing Chandra and XMM-Newton studies of SNR 1987A. Thus, we propose an 80 ks Suzaku observation of SNR 1987A.	EXTRAGALACTIC COMPACT SOURCES	7	C	SANGWOOK PARK		USA	7	AO7	X-RAY EMISSION FROM SUPERNOVA REMNANT 1987A	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707020010/	Quick Look
545	A1413_FIELD_3	179.0207	23.4251	178.377297	23.70339	169.347727	21.006295	226.37028623	76.95859752	302.9994	55347.1862037037	2010-05-31 04:28:08	55348.2079050926	2010-06-01 04:59:23	805061010	40.9225	40	40.9225	40.9385	0	40.9305	2	2	0	2	1	0	0	32.9944	32.9944	88.2578	0	PROCESSED	57553.3965856482	2016-06-14 09:31:05	55287	2010-04-01 00:00:00	55393.4280208333	2010-07-16 10:16:21	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805061010/	Quick Look
546	A383_FIELD_2	41.9447	-3.4083	41.315431	-3.616408	38.400744	-18.662791	177.53047769	-53.46482162	60.9996	55389.1380208333	2010-07-12 03:18:45	55390.062662037	2010-07-13 01:30:14	805063010	43.3415	40	43.3575	43.3415	0	43.3575	2	2	0	2	1	0	0	39.2589	39.2589	79.8749	0	PROCESSED	57552.6168055556	2016-06-13 14:48:12	55287	2010-04-01 00:00:00	55411.2445601852	2010-08-03 05:52:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051115	We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	5	AO5	THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805063010/	Quick Look
547	CTA102	338.1458	11.7401	337.526658	11.482274	344.409824	19.371456	77.43997335	-38.57166798	72.4263	56431.345462963	2013-05-19 08:17:28	56431.6134606482	2013-05-19 14:43:23	707045010	9.5626	10	9.5706	9.5626	0	9.5706	1	1	0	1	1	0	0	7.283	7.283	23.1439	0	PROCESSED	57611.3187847222	2016-08-11 07:39:03	56809	2014-06-01 00:00:00	56443.5010069444	2013-05-31 12:01:27	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071601	We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars.	EXTRAGALACTIC COMPACT SOURCES	7	S	SVETLANA JORSTAD		USA	7	AO7	MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707045010/	Quick Look
548	LEDA 168563	73.0158	49.5506	72.064208	49.467096	77.740518	26.831198	157.24701812	3.42018054	86.3166	56536.8773611111	2013-09-01 21:03:24	56539.0592708333	2013-09-04 01:25:21	708017010	100.011	100	100.035	100.011	0	100.035	3	2	0	2	1	0	0	92.947	92.947	188.5018	1	PROCESSED	57612.530162037	2016-08-12 12:43:26	56383	2013-04-01 00:00:00	56608.7327893518	2013-11-12 17:35:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081413	We propose to carry out Suzaku observations, a 100 ks each, of three Seyfert I nuclei hard X-ray selected by Swift. Our goal is to distinguish between various competing models proposed for the X-ray spectra of Seyfert I nuclei. Especially we will test, by observing these targets, the ionized relativistic reflection (hereafter IRR). We will take advantage of Suzaku s unique capability of detecting hard X-rays beyond 10 keV by its HXD-PIN, simultaneously with X-rays in lower to medium energy bands by its XIS on board. With our proposed studies we will gain deeper understanding of accretion-powered AGN in general. Since the IRR takes place close to the black hole we will test the effects of strong gravity, such as the black hole spin.	EXTRAGALACTIC COMPACT SOURCES	7	B	SACHIKO TSURUTA		USA	8	AO8	SPECTRAL STUDIES OF SOME HARD X-RAY SELECTED SEYFERT NUCLEI	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708017010/	Quick Look
549	MKW 4-OFFSET1	181.1304	2.2289	180.489911	2.507266	180.147119	2.494288	276.66004128	62.68282085	114.5816	55528.2862847222	2010-11-28 06:52:15	55530.2501967593	2010-11-30 06:00:17	805081010	79.4261	80	79.4261	79.4261	0	79.4261	2	2	0	2	1	0	0	68.2112	68.2112	169.6679	2	PROCESSED	57554.312025463	2016-06-15 07:29:19	55909	2011-12-14 00:00:00	55543.4043402778	2010-12-13 09:42:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051525	We propose a set of two 19 arcmin offset observations for the galaxy groups MKW 4 to measure spatially resolved density, temperature and iron abundance out to r_{500}. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to its brightness, regularity and low temperature, the object is an ideal candidate for an offset observation of its peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	FABIO GASTALDELLO		USA	5	AO5	THE OUTSKIRTS OF MKW 4	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805081010/	Quick Look
550	PKS 0745-191	116.3632	-19.0871	115.808852	-18.964679	122.979801	-39.556071	236.01662317	2.71025988	294.0001	55316.6424189815	2010-04-30 15:25:05	55317.3675231482	2010-05-01 08:49:14	805085010	34.9999	35	34.9999	34.9999	0	34.9999	2	2	0	2	1	0	0	32.7804	32.7804	62.6419	2	PROCESSED	57551.3324074074	2016-06-12 07:58:40	55696	2011-05-15 00:00:00	55330.1114236111	2010-05-14 02:40:27	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	051526	Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MATTHEW GEORGE		USA	5	AO5	BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805085010/	Quick Look
551	IGR J09026-4812	135.6468	-48.2323	135.224236	-48.033912	164.675258	-60.400706	268.86967218	-1.09239209	115.8572	56622.3203356482	2013-11-26 07:41:17	56622.9521990741	2013-11-26 22:51:10	708031010	37.7924	35	37.8244	37.8164	0	37.7924	2	2	0	2	1	0	0	35.2029	35.2029	54.5859	1	PROCESSED	57613.429212963	2016-08-13 10:18:04	56383	2013-04-01 00:00:00	56632.5852777778	2013-12-06 14:02:48	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081419	The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come.	EXTRAGALACTIC COMPACT SOURCES	7	C	TAHIR YAQOOB		USA	8	AO8	ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708031010/	Quick Look
552	ABELL 981	156.0884	68.0988	155.16023	68.352315	123.8863	52.287736	140.87577234	43.55064218	119.4308	56601.2179398148	2013-11-05 05:13:50	56601.7917708333	2013-11-05 19:00:09	708040010	27.5945	30	27.6025	27.5945	0	27.5945	2	2	0	2	1	0	0	25.286	25.286	49.574	1	PROCESSED	57613.2182060185	2016-08-13 05:14:13	56980	2014-11-19 00:00:00	56614.6564583333	2013-11-18 15:45:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081533	We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters.	EXTRAGALACTIC COMPACT SOURCES	7	C	LAURENCE DAVID		USA	8	AO8	MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708040010/	Quick Look
553	HOLMBERG IX X-1	149.4572	69.0544	148.43919	69.292844	119.777434	51.680142	141.94722641	41.07197433	311.5038	57118.9110416667	2015-04-06 21:51:54	57119.5667708333	2015-04-07 13:36:09	709015030	31.5263	30	31.5263	31.5263	0	31.5263	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57617.9243402778	2016-08-17 22:11:03	57513	2016-05-05 00:00:00	57129.4193171296	2015-04-17 10:03:49	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	091251	Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs.	EXTRAGALACTIC COMPACT SOURCES	7	A	DOMINIC WALTON		USA	9	AO9	MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709015030/	Quick Look
554	ABELL 1795 Far South	207.2227	26.2001	206.644395	26.44826	194.131601	34.631873	32.0541753	77.13779505	129.4115	53716.5361921296	2005-12-12 12:52:07	53717.4168865741	2005-12-13 10:00:19	800012050	40.1206	30	40.1366	40.1526	40.1206	40.1366	2	2	2	2	1	0	0	39.4373	39.4373	76.0819	1	PROCESSED	57532.4477314815	2016-05-24 10:44:44	54247	2007-05-27 00:00:00	54039.1460069445	2006-10-31 03:30:15	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001056	We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	MARK BAUTZ		JAP	0	SWG	TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012050/	Quick Look
555	ABELL 3112	49.4982	-44.2507	49.063827	-44.432376	25.5219	-58.972557	252.95298598	-56.06981795	43.5004	56466.5743634259	2013-06-23 13:47:05	56468.5418055556	2013-06-25 13:00:12	808068010	119.1247	200	119.1247	119.1247	0	119.1247	2	2	0	2	1	0	0	114.5618	114.5618	169.9418	0	PROCESSED	57611.6340856482	2016-08-11 15:13:05	56848	2014-07-10 00:00:00	56481.8003356482	2013-07-08 19:12:29	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	081522	The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ESRA BULBUL		USA	8	AO8	CHEMICAL EVOLUTION HISTORY OF A COOL CORE CLUSTER A3112 OUT TO THE VIRIAL RADIUS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808068010/	Quick Look
556	OJ 287	133.705	20.1043	132.989927	20.295379	130.505973	2.596868	206.81753743	35.82068078	285.8744	57148.4467708333	2015-05-06 10:43:21	57151.4189351852	2015-05-09 10:03:16	710011020	110.2819	323	110.2819	112.3099	0	112.3099	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.1271643518	2016-08-18 03:03:07	57113	2015-04-01 00:00:00	57164.5272337963	2015-05-22 12:39:13	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101431	Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously.	EXTRAGALACTIC COMPACT SOURCES	7	A	RICK EDELSON		USA	10	AO10	SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011020/	Quick Look
557	OJ 287	133.7049	20.1044	132.989827	20.295479	130.505855	2.596938	206.81738245	35.82062575	285.8744	57151.4189467593	2015-05-09 10:03:17	57154.3266666667	2015-05-12 07:50:24	710011030	107.7143	323	107.7143	107.7143	0	107.7143	2	2	0	2	0	0	0	0	0	0	0	PROCESSED	57618.6879166667	2016-08-18 16:30:36	57113	2015-04-01 00:00:00	57164.5596527778	2015-05-22 13:25:54	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	101431	Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously.	EXTRAGALACTIC COMPACT SOURCES	7	A	RICK EDELSON		USA	10	AO10	SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710011030/	Quick Look
558	ABELL2811	10.4703	-28.5552	9.856516	-28.82929	357.097887	-30.138768	358.34166022	-87.45073592	232.1065	53702.1678240741	2005-11-28 04:01:40	53702.8814699074	2005-11-28 21:09:19	800005010	30.6546	25	30.6626	30.6826	30.6546	30.6659	2	2	2	2	1	0	0	28.3254	28.3254	61.656	0	PROCESSED	57528.0937268518	2016-05-20 02:14:58	54247	2007-05-27 00:00:00	54038.5109722222	2006-10-30 12:15:48	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001025	We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	TAKAYUKI TAMURA		JAP	0	SWG	THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800005010/	Quick Look
559	A426	49.9554	41.5039	49.127963	41.323287	58.608686	22.329679	150.58326426	-13.26576669	260.2176	53767.568900463	2006-02-01 13:39:13	53768.5294560185	2006-02-02 12:42:25	800010010	50.3986	50	50.4066	50.4066	50.3986	50.4066	2	2	2	2	1	0	0	54.4364	54.4364	82.9758	0	PROCESSED	57532.8781365741	2016-05-24 21:04:31	54247	2007-05-27 00:00:00	54041.0862152778	2006-11-02 02:04:09	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001036	A426 is the X-ray brightest cluster in the Sky. The core is X-ray peaked, has a short radiative cooling time, a temperature drop and a central radio source which is blowing bubbles in the intracluster medium. A radio minihalo extends over the central 6 arcmin. A coincident power-law component is seen in deep Chandra data. This is likely to be inverse Compton emission from the electron population responsible for the radio emission. The region is expected to be a luminous, extended, hard X-ray source easily detectable by the Suzaku HXD. Confirmation of this hard X-ray component will enable the magnetic field to be securely determined in the intracluster gas.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ANDREW FABIAN		JAP	0	SWG	THE HARD X-RAY FLUX FROM THE CORE OF THE PERSEUS CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800010010/	Quick Look
560	ABELL 773	139.6415	51.5835	138.770726	51.794221	124.818527	33.970374	166.25628799	43.50358503	276.9979	55683.2110185185	2011-05-02 05:03:52	55684.0730208333	2011-05-03 01:45:09	806027020	47.2223	50	47.2303	47.2223	0	47.2383	2	2	0	2	1	0	0	46.5115	46.5115	74.4719	0	PROCESSED	57601.9085185185	2016-08-01 21:48:16	55652	2011-04-01 00:00:00	55697.3168981482	2011-05-16 07:36:20	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806027020/	Quick Look
561	CENCL OFFSET2	192.2009	-41.1804	191.510431	-40.907877	208.999282	-32.736275	302.39848339	21.68862024	106.52	53733.2507407407	2005-12-29 06:01:04	53734.3543865741	2005-12-30 08:30:19	800016010	43.2773	40	43.2853	43.2853	43.2773	43.2933	2	2	2	2	1	0	0	35.2531	35.2531	95.332	1	PROCESSED	57532.5900578704	2016-05-24 14:09:41	54247	2007-05-27 00:00:00	54039.6041203704	2006-10-31 14:29:56	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001070	A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	YASUSHI FUKAZAWA		JAP	0	SWG	OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800016010/	Quick Look
562	NGC 4636	190.7243	2.7556	190.086173	3.029415	188.766391	6.778722	297.77503713	65.54179663	112.2967	53710.1073726852	2005-12-06 02:34:37	53711.9446643518	2005-12-07 22:40:19	800018010	79.201	80	79.201	79.201	79.201	79.201	2	2	2	2	1	0	0	75.7771	75.7771	158.7278	2	PROCESSED	57532.4099421296	2016-05-24 09:50:19	54247	2007-05-27 00:00:00	54038.9551388889	2006-10-30 22:55:24	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	001083	We propose to observe NGC 4636 for 50~ksec in a single pointing, to determine the chemical evolution of elliptical galaxies via the determination of the spatially resolved abundance of Oxygen and other elements. Being one of the most X-ray luminous ellipticals, and having been observed by both Chandra and XMM, this is also an important target to compare the capabilities of the three observatories and interpret the results of the Suzaku XIS in light of the source spectrum provided by the XMM RGS.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ENECTALI FIGUEROA-FELICIANO		JAP	0	SWG	OBSERVATION OF THE X-RAY LUMINOUS EXTENDED EARLY-TYPE GALAXY NGC 4636	XIS	N	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800018010/	Quick Look
563	ABELL 2667	357.7341	-26.0226	357.087227	-26.30077	347.004408	-22.85609	34.17814736	-76.43580815	64.8804	55722.9055208333	2011-06-10 21:43:57	55724.4196990741	2011-06-12 10:04:22	806029020	51.6577	50	51.6657	51.6577	0	51.6721	2	2	0	2	1	0	0	45.656	45.656	130.802	1	PROCESSED	57602.2808333333	2016-08-02 06:44:24	55652	2011-04-01 00:00:00	55757.7009027778	2011-07-15 16:49:18	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061116	We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	6	AO6-LP	THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806029020/	Quick Look
564	COMA E6.5	196.9526	27.8857	196.354379	28.152377	183.408228	32.112773	45.6576416	86.29162208	279.9993	55731.5902199074	2011-06-19 14:09:55	55732.0578935185	2011-06-20 01:23:22	806037010	14.9596	15	14.9676	14.9596	0	14.9676	1	1	0	1	1	0	0	13.6142	13.6142	40.3999	0	PROCESSED	57602.3577314815	2016-08-02 08:35:08	55652	2011-04-01 00:00:00	55770.17125	2011-07-28 04:06:36	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806037010/	Quick Look
565	COMA SW7	193.2936	26.7739	192.684688	27.045132	180.600519	29.664204	350.54999025	89.47529971	314.5993	55737.124212963	2011-06-25 02:58:52	55737.4447106482	2011-06-25 10:40:23	806051010	15.4152	15	15.4152	15.4232	0	15.4232	1	1	0	1	1	0	0	15.0368	15.0368	27.6719	0	PROCESSED	57602.4087847222	2016-08-02 09:48:39	55652	2011-04-01 00:00:00	55795.0185763889	2011-08-22 00:26:45	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061117	Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	AURORA SIMIONESCU		USA	6	AO6-LP	BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806051010/	Quick Look
566	30 DORADUS	84.6512	-69.1008	84.737262	-69.126573	305.902613	-86.759222	279.46621821	-31.68092384	162.7542	55895.6278472222	2011-11-30 15:04:06	55897.0640162037	2011-12-02 01:32:11	806052010	101.6448	100	101.6528	101.6528	0	101.6448	2	2	0	2	1	0	0	89.0823	89.0823	124.076	0	PROCESSED	57604.044837963	2016-08-04 01:04:34	56281	2012-12-20 00:00:00	55907.9795486111	2011-12-12 23:30:33	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061322	We propose a deep Suzaku observation of 30 Doradus to provide a direct X-ray measurement of the chemical enrichment in the enclosed hot gas. The soft X-ray sensitivity and spectral resolution of this observation will allow us to measure key elemental abundances and thus to test models for metal yields of massive stars. We will determine the spatial variation in the thermal and chemical properties of the hot gas and the effect on the global estimation of the chemical enrichment from an integrated spectrum, as would be obtained for a distant starburst region. We will also estimate the mass-loading from the general interstellar medium --- a key parameter for determining the evolution of the hot gas. The results will serve as an observational benchmark for understanding massive star feedback.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	Q. DANIEL WANG		USA	6	AO6	X-RAY SPECTROSCOPIC MAPPING OF 30 DORADUS: CHEMICAL ENRICHMENT BY MASSIVE STARS IN A CLOSED BOX	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806052010/	Quick Look
567	RCS131723-0201.3	199.3422	-2.034	198.698505	-1.770799	198.620431	5.687336	316.04491283	60.17589221	291.8811	55756.3454513889	2011-07-14 08:17:27	55756.9585532407	2011-07-14 23:00:19	806078010	24.921	25	24.921	24.921	0	24.921	2	2	0	2	1	0	0	23.1205	23.1205	52.9619	1	PROCESSED	57602.5803009259	2016-08-02 13:55:38	56163	2012-08-24 00:00:00	55783.6867939815	2011-08-10 16:28:59	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	061533	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AMALIA HICKS		USA	6	AO6	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806078010/	Quick Look
568	PKS 0745-191	116.9737	-19.0727	116.418821	-18.947622	123.702706	-39.408553	236.29361594	3.21678926	294.0001	54232.5006712963	2007-05-12 12:00:58	54233.2258564815	2007-05-13 05:25:14	802062030	30.7942	30	30.8022	30.7942	0	30.8022	2	2	0	2	1	0	0	26.6388	26.6388	62.6301	0	PROCESSED	57538.6331134259	2016-05-30 15:11:41	54695	2008-08-17 00:00:00	54245.5042592593	2007-05-25 12:06:08	3.0.22.43	4	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	021440	PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ANDREW YOUNG		USA	2	AO2	PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062030/	Quick Look
569	SDSS J1302+4729	195.5068	47.4831	194.946247	47.751657	168.926268	48.423966	117.80880843	69.53967787	316.2365	56076.2710648148	2012-05-29 06:30:20	56076.7058217593	2012-05-29 16:56:23	807060010	20.427	20	20.427	20.427	0	20.427	1	1	0	1	1	0	0	24.66	24.66	37.5599	1	PROCESSED	57605.5578240741	2016-08-05 13:23:16	56500	2013-07-27 00:00:00	56134.0735300926	2012-07-26 01:45:53	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071512	Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	ERIC MILLER		USA	7	AO7	FINDING FOSSIL GROUPS WITH SUZAKU	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807060010/	Quick Look
570	ANTLIA E5	159.3469	-35.3315	158.776481	-35.071439	177.451568	-40.165459	274.29394045	19.97884062	279.4997	56095.3697337963	2012-06-17 08:52:25	56096.5972916667	2012-06-18 14:20:06	807070010	46.7814	45	46.7894	46.7814	0	46.7974	2	2	0	2	1	0	0	41.0617	41.0617	106.0579	2	PROCESSED	57605.7158333333	2016-08-05 17:10:48	56590	2013-10-25 00:00:00	56219.6892361111	2012-10-19 16:32:30	3.0.22.44	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071521	We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	KA-WAH WONG		USA	7	AO7	MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807070010/	Quick Look
571	RCS0442-2815	70.5602	-28.2499	70.060746	-28.343732	62.940418	-49.88298	228.44078987	-39.40072076	273.8381	54903.705462963	2009-03-13 16:55:52	54905.2669444444	2009-03-15 06:24:24	803060010	52.3573	40	52.3573	52.3573	0	52.3573	2	2	0	2	1	0	0	47.4137	47.4137	134.8779	1	PROCESSED	57545.8322222222	2016-06-06 19:58:24	55329	2010-05-13 00:00:00	54917.4174652778	2009-03-27 10:01:09	3.0.22.43	3	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	031441	Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	3	AO3	COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803060010/	Quick Look
572	ABELL 665	128.154	65.9045	127.018266	66.074275	110.985423	45.219486	149.6634974	34.85484411	289.999	56026.3998958333	2012-04-09 09:35:51	56027.1251967593	2012-04-10 03:00:17	807072010	50.431	50	50.431	50.431	0	50.431	2	2	0	2	1	0	0	41.0111	41.0111	62.6599	1	PROCESSED	57605.1298958333	2016-08-05 03:07:03	56018	2012-04-01 00:00:00	56044.1528240741	2012-04-27 03:40:04	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072010/	Quick Look
573	ABELL 665	127.5519	65.9953	126.410061	66.162736	110.613991	45.219649	149.61230509	34.59661242	290.0005	56027.1259953704	2012-04-10 03:01:26	56027.8057638889	2012-04-10 19:20:18	807072020	51.446	50	51.446	51.446	0	51.446	2	2	0	2	1	0	0	43.2769	43.2769	58.728	1	PROCESSED	57605.1345717593	2016-08-05 03:13:47	56018	2012-04-01 00:00:00	56044.1899537037	2012-04-27 04:33:32	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071522	We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	ERIC MILLER		USA	7	AO7	COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072020/	Quick Look
574	RCS110619-0423.6	166.5769	-4.3915	165.941193	-4.121064	169.375504	-9.341083	260.07293798	49.52807614	109.9541	56253.8521296296	2012-11-22 20:27:04	56256.0092476852	2012-11-25 00:13:19	807075010	77.0765	75	77.0925	77.0765	0	77.1005	2	2	0	2	1	0	0	69.3805	69.3805	186.3458	4	PROCESSED	57608.1296875	2016-08-08 03:06:45	56641	2013-12-15 00:00:00	56275.577025463	2012-12-14 13:50:55	3.0.22.44	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	071525	Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample.	EXTRAGALACTIC DIFFUSE SOURCES	8	C	AMALIA HICKS		USA	7	AO7	AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807075010/	Quick Look
575	NGC741 E	29.459	5.6113	28.805334	5.368113	29.381945	-6.027315	151.51137993	-53.53548595	71.776	55054.8091087963	2009-08-11 19:25:07	55055.0619675926	2009-08-12 01:29:14	804053010	11.3778	10	11.3778	11.3858	0	11.3938	2	2	0	2	1	0	0	8.0052	8.0052	21.838	0	PROCESSED	57548.1250231482	2016-06-09 03:00:02	55430	2010-08-22 00:00:00	55064.1656134259	2009-08-21 03:58:29	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804053010/	Quick Look
576	NGC741MOSAICS_P1	29.0595	4.7357	28.408059	4.491575	28.699079	-6.708921	151.53660126	-54.49712787	71.6617	55052.4780671296	2009-08-09 11:28:25	55052.6946643518	2009-08-09 16:40:19	804054010	9.3222	10	9.3302	9.3222	0	9.3302	1	1	0	1	1	0	0	8.003	8.003	18.6719	1	PROCESSED	57548.0801967593	2016-06-09 01:55:29	55451	2010-09-12 00:00:00	55084.9869212963	2009-09-10 23:41:10	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041515	Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	JOEL BREGMAN		USA	4	AO4	THE MISSING BARYONS IN GALAXY GROUPS	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054010/	Quick Look
577	ABELL 426 E3	51.0503	41.5202	50.219736	41.343661	59.4655	22.121233	151.27232524	-12.79481746	89.0003	55041.9666666667	2009-07-29 23:12:00	55042.2904398148	2009-07-30 06:58:14	804058010	11.2798	10	11.2798	11.5518	0	11.5518	3	2	0	2	1	0	0	10.7201	10.7201	27.9661	0	PROCESSED	57547.981412037	2016-06-08 23:33:14	55427	2010-08-19 00:00:00	55060.7814236111	2009-08-17 18:45:15	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041522	Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster.	EXTRAGALACTIC DIFFUSE SOURCES	8	A	STEVEN ALLEN		USA	4	AO4	TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY	XIS	Y	https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804058010/	Quick Look
578	RCS1620+3046	245.0418	30.7908	244.551505	30.909318	234.634805	51.209306	50.54291734	44.60353773	131.519	55203.6116666667	2010-01-07 14:40:48	55204.6008564815	2010-01-08 14:25:14	804081010	43.4882	38	43.4882	43.4882	0	43.4882	2	2	0	2	1	0	0	16.6324	16.6324	85.4538	0	PROCESSED	57550.1212615741	2016-06-11 02:54:37	55584	2011-01-23 00:00:00	55218.2018402778	2010-01-22 04:50:39	3.0.22.43	2	Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22	041525	Understanding relationships between baryons in galaxy clusters and the underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a cluster sample chosen independently of X-ray properties. We propose to study 14 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Chandra observations of 8 high-dispersion, low-z targets. Suzaku s superior throughput is required to probe the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 6 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters.	EXTRAGALACTIC DIFFUSE SOURCES	8	B	AMALIA HICKS		USA	4	AO4	DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES	XIS	Y